WorldWideScience

Sample records for board venus express

  1. Results from VIRTIS on board Venus Express after the end of the mission operations

    Science.gov (United States)

    Piccioni, G.; Drossart, P.; VIRTIS Venus Express Team

    After more than 8 years since the orbit insertion, the Venus Express mission is now at its end of mission operations. VIRTIS aboard the Venus Express spacecraft has addressed a significant amount of scientific results from the surface up to the upper atmosphere, in terms of mapping, composition, structure and dynamics. The VIRTIS instrument consists of two channels: VIRTIS-M, an imaging spectrometer with moderate spectral resolution in the range from 0.25 to 5.2 mu m and VIRTIS-H, a high spectral resolution spectrometer in the range from 2 to 5 mu m co-aligned with the field of view of -M \\citep{Piccioni2007a,Drossart2007a}. The resolution of VIRTIS-M is 2 nm from 0.25 to 1 mu m, and 10 nm from 1 to 5.2 mu m. The resolution of VIRTIS-H is about 2 nm. The atmosphere above the clouds has been observed both on day and night sides, in solar reflection and thermal emission in nadir geometry \\citep{Ignatiev2009, Cottini2012, Peralta2012, Peralta2009}. Limb observations provided O2\\citep{Piccioni2009, Garcia2009a, Gerard2013, Migliorini2013a, Gerard2008, Gerard2009}, OH \\citep{Piccioni2008,Gerard2010,Soret2010,Soret2012}, NO \\citep{Garcia2009b}, CO2 \\citep{Drossart2007b,Lopez-Valverde2011} and CO \\citep{Gilli2009,Gilli2015,Gilli2011} emissions, through nightglow and fluorescence observations. Spectroscopy of the 4-5 mu m range gave access to the cloud structure in the 60-95 km altitude levels \\citep{Irwin2008a,Grassi2014, Grassi2008,Grassi2010,Luz2011}. The deeper atmospheric windows, limited by CO2 and H2O bands were accessible only in thermal emission on the night side. The sounded levels at 1.7 and 2.3 mu m were limited respectively to 30-20 km altitude \\citep{Barstow2012,Bezard2009,Marcq2008a,Satoh2009,Tsang2009, Tsang2010,Tsang2008,Wilson2008,Wilson2009}, while at shorter wavelengths (1.18, 1.10, 1.01, 0.9 and 0.85 mu m), the hot surface of Venus was seen through the scattering clouds \\citep{Mueller2009,Helbert2008,Arnold2008a,Smrekar2010,Mueller2012

  2. Venus

    CERN Document Server

    Payment, Simone

    2017-01-01

    This straightforward but fascinating book takes a close look at Venus and shows young people just how different our neighboring planet is from our own. Known as the hottest planet, Venus is an example of the greenhouse effect to the extreme. Young readers will take a tour beneath the sulfur dioxide clouds and see the planet's surface up close with images taken by the Magellan and the Venus Express missions. This book will surely fascinate any young person interested in alien worlds.

  3. Venus Express ready for lift-off

    Science.gov (United States)

    2005-10-01

    Venus Express is Europe’s first mission to Venus, a place of many mysteries that scientists are still eager to solve. Principal among those mysteries is why a planet so similar to the Earth in size, mass, and composition has evolved so differently over the course of the last 4.6 billion years. ESA’s ESOC establishment, the Space Operations Centre in Darmstadt, Germany will control the mission and organise a launch event from 06:00 to 12:00. A live televised transmission of the launch will bring images from Baikonur to broadcasters and the general public. ESA senior management and specialists will be on hand at ESOC and at other ESA establishments for explanations and interviews. All live transmissions are carried free-to-air. For broadcasters, complete details of the various satellite feeds (on Eutelsat W2) are listed at http://television.esa.int. For the general public, a launch transmission via Astra 1G has again been organised, with all schedule and transmission details online at http://television.esa.int/photos/Astra.pdf On the occasion of the launch of Venus Express, the Planetary Society has teamed up with ESA to invite youths and adults worldwide to enter a Venus Express Art Contest. The theme of the contest is "Postcards from Venus". Entrants are invited to imagine the surface of Venus from an above-ground perspective. The winner will be invited to follow the Venus Orbit Insertion event at ESA's control centre in Darmstadt, Germany, on 6 April 2006. More on the constest at http://planetary.org/postcards_from_venus/ Media representatives wishing to follow the event at ESA/ESOC, or the retransmission at other ESA establishments, are requested to fill in the attached registration form and fax it back to the place of their choice.

  4. Low-frequency magnetic field fluctuations in Venus' solar wind interaction region: Venus Express observations

    Directory of Open Access Journals (Sweden)

    L. Guicking

    2010-04-01

    Full Text Available We investigate wave properties of low-frequency magnetic field fluctuations in Venus' solar wind interaction region based on the measurements made on board the Venus Express spacecraft. The orbit geometry is very suitable to investigate the fluctuations in Venus' low-altitude magnetosheath and mid-magnetotail and provides an opportunity for a comparative study of low-frequency waves at Venus and Mars. The spatial distributions of the wave properties, in particular in the dayside and nightside magnetosheath as well as in the tail and mantle region, are similar to observations at Mars. As both planets do not have a global magnetic field, the interaction process of the solar wind with both planets is similar and leads to similar instabilities and wave structures. We focus on the spatial distribution of the wave intensity of the fluctuating magnetic field and detect an enhancement of the intensity in the dayside magnetosheath and a strong decrease towards the terminator. For a detailed investigation of the intensity distribution we adopt an analytical streamline model to describe the plasma flow around Venus. This allows displaying the evolution of the intensity along different streamlines. It is assumed that the waves are generated in the vicinity of the bow shock and are convected downstream with the turbulent magnetosheath flow. However, neither the different Mach numbers upstream and downstream of the bow shock, nor the variation of the cross sectional area and the flow velocity along the streamlines play probably an important role in order to explain the observed concentration of wave intensity in the dayside magnetosheath and the decay towards the nightside magnetosheath. But, the concept of freely evolving or decaying turbulence is in good qualitative agreement with the observations, as we observe a power law decay of the intensity along the streamlines. The observations support the assumption of wave convection through the magnetosheath, but

  5. O+ pickup ions outside of Venus' bow shock: Venus Express observations

    Science.gov (United States)

    Wei, Yong; Fraenz, Markus; Dubinin, Eduard; Zhang, Tielong; Jarvinen, Riku; Wan, Weixing; Kallio, Esa; Collinson, Glyn; Barabash, Stars; Norbert, Krupp; Woch, Joachim; Lundin, Rickard; delva, Magda

    2013-04-01

    Pickup ions are ions of planetary origin that become assimilated into the solar wind flow through their interaction with the solar wind magnetic and electric field. The speed of pickup ions varies between zero and twice the underlying plasma flow component perpendicular to magnetic field vector. For the unmagnetized planet Venus and Mars, oxygen (O+) pickup ions are known to be important because they can modify the global configuration of planetary plasma environment and significantly contribute to the atmospheric O+ loss [1]. Since the kinetic energy of an O+ pickup ion can reach 64 times that of a co-moving proton, an instrument must be able to measure O+ ions with energy of at least tens of keV to investigate the O+ pickup ion distribution from planetary ionosphere to solar wind. The in-situ observations and simulations at Mars have shown that the energy of O+ pickup ions can be 55-72 keV outside of the bow shock [2]. For Venus case, the plasma analyzer (OPA) onboard Pioneer Venus Orbiter (PVO), which was designed for solar wind monitoring, has an 8 keV energy limit for O+ detection and the limited sampling and data rate [3]. Therefore, OPA can only measure the O+ pickup ions in the sheath flow or inside the induced magnetosphere where the speed of ambient plasma flow is significantly lower than that of the unshocked solar wind outside of the bow shock. In addition, Galileo also did not capture O+ outside bowshock during its 1-hour Venus flyby though its plasma instrument had ability to cover the energy band of O+ pickup ions [4]. The Ion Mass Analyzer (IMA), included in the Analyzer of Space Plasma and Energetic Atoms (ASPERA-4) package on board Venus Express (VEX), determines the composition, energy, and angular distribution of ions in the energy range ~10 eV/q to 30 keV/q. Note that an O+ ion moving at the typical solar wind speed 400 km/s has kinetic energy 13.4 keV. Therefore, IMA has ability to measure the O+ pickup ions outside of Venus' bow shock. We

  6. Venus Express uurib Maa kurja kaksikut / ref. Triin Thalheim

    Index Scriptorium Estoniae

    2005-01-01

    9. novembril startis Baikonuri kosmodroomilt Veenusele Euroopa Kosmoseagentuuri sond Venus Express, mis peaks planeedi atmosfääri sisenema aprillis. Teadlaste sõnul peab sondi saadetav info aitama mõista naaberplaneedi kliimat ja atmosfääri ning tooma selgust, kas Maa võib kunagi Veenuse sarnaseks muutuda. Lisaks joonis: Venus Express

  7. Sulfuric Acid Vapor in the Atmosphere of Venus as Observed by the Venus Express Radio Science Experiment VeRa

    Science.gov (United States)

    Oschlisniok, Janusz; Pätzold, Martin; Häusler, Bernd; Tellmann, Silvia; Bird, Michael; Andert, Thomas

    2017-10-01

    The cloud deck within Venus' atmosphere, which covers the entire planet between approx. 50 and 70 km altitude, consists mostly of liquid and gaseous sulfuric acid. The gaseous part increases strongly just below the main clouds and builds an approx. 15 km thick haze layer of H2SO4. This region is responsible for a strong absorption of radio waves as seen in Mariner, Pioneer Venus, Magellan and Venera radio science observations. The amount of H2SO4 is derived from the observed absorption as a function of altitude and latitude. The radio science experiment VeRa onboard Venus Express probed the atmosphere of Venus between 2006 and 2015 with radio signals at 13 cm (S-band) and 3.6 cm (X-band) wavelengths. The orbit of the Venus Express spacecraft allowed to sound the atmosphere over a wide range of latitudes and local times providing a global picture of the sulfuric acid vapor distribution. We present absorptivity and H2SO4 profiles derived from X-band signal attenuation for the time of the entire Venus Express mission. More than 600 H2SO4 profiles show the global sulfuric acid vapor distribution covering the northern and southern hemisphere on the day- and night side of the planet. A distinct latitudinal H2SO4 gradient and a southern northern symmetry are clearly visible. Observations over 8 years allow to study also long-term variations. Indications for temporal H2SO4 variations are found, at least at northern polar latitudes. The results shall be compared with observations retrieved by other experiments (VIRTIS, SPICAV) onboard Venus Express as well as with previous observations like Mariner, Pioneer Venus and the Magellan spacecraft.

  8. Sulfuric Acid Vapor in the Atmosphere of Venus as observed by the Venus Express Radio Science Experiment VeRa.

    Science.gov (United States)

    Oschlisniok, J.; Paetzold, M.; Häusler, B.; Tellmann, S.; Bird, M. K.; Andert, T.

    2017-12-01

    The cloud deck within Venus' atmosphere, which covers the entire planet between approx. 50 and 70 km altitude, consists mostly of liquid and gaseous sulfuric acid. The gaseous part increases strongly just below the main clouds and builds an approx. 15 km thick haze layer of H2SO4. This region is responsible for a strong absorption of radio waves as seen in Mariner, Pioneer Venus, Magellan and Venera radio science observations. The amount of H2SO4 is derived from the observed absorption as a function of altitude and latitude. The radio science experiment VeRa onboard Venus Express probed the atmosphere of Venus between 2006 and 2015 with radio signals at 13 cm (S-band) and 3.6 cm (X-band) wavelengths. The orbit of the Venus Express spacecraft allowed to sound the atmosphere over a wide range of latitudes and local times providing a global picture of the sulfuric acid vapor distribution. We present absorptivity and H2SO4 profiles derived from X-band signal attenuation for the time of the entire Venus Express mission. More than 600 H2SO4 profiles show the global sulfuric acid vapor distribution covering the northern and southern hemisphere on the day- and night side of the planet. A distinct latitudinal H2SO4 gradient and a southern northern symmetry are clearly visible. Observations over 8 years allow to study also long-term variations. Indications for temporal H2SO4 variations are found, at least at northern polar latitudes. The results shall be compared with observations retrieved by other experiments (VIRTIS, SPICAV) onboard Venus Express as well as with previous observations like Mariner, Pioneer Venus and the Magellan spacecraft.

  9. Venus Express en route to probe the planet's hidden mysteries

    Science.gov (United States)

    2005-11-01

    Venus Express will eventually manoeuvre itself into orbit around Venus in order to perform a detailed study of the structure, chemistry and dynamics of the planet's atmosphere, which is characterised by extremely high temperatures, very high atmospheric pressure, a huge greenhouse effect and as-yet inexplicable "super-rotation" which means that it speeds around the planet in just four days. The European spacecraft will also be the first orbiter to probe the planet's surface while exploiting the "visibility windows" recently discovered in the infrared waveband. The 1240 kg mass spacecraft was developed for ESA by a European industrial team led by EADS Astrium with 25 main contractors spread across 14 countries. It lifted off onboard a Soyuz-Fregat rocket, the launch service being provided by Starsem. The lift-off from the Baikonur Cosmodrome in Kazakstan this morning took place at 09:33 hours local time (04:33 Central European Time). Initial Fregat upper-stage ignition took place 9 minutes into the flight, manoeuvring the spacecraft into a low-earth parking orbit. A second firing, 1 hour 22 minutes later, boosted the spacecraft to pursue its interplanetary trajectory. Contact with Venus Express was established by ESA's European Space Operations Centre (ESOC) at Darmstadt, Germany approximately two hours after lift-off. The spacecraft has correctly oriented itself in relation to the sun and has deployed its solar arrays. All onboard systems are operating perfectly and the orbiter is communicating with the Earth via its low-gain antenna. In three days' time, it will establish communications using its high-gain antenna. Full speed ahead for Venus Venus Express is currently distancing itself from the Earth full speed, heading on its five-month 350 million kilometre journey inside our solar system. After check-outs to ensure that its onboard equipment and instrument payload are in proper working order, the spacecraft will be mothballed, with contact with the Earth being

  10. Description, accessibility and usage of SOIR/Venus Express atmospheric profiles of Venus distributed in VESPA (Virtual European Solar and Planetary Access)

    Science.gov (United States)

    Trompet, L.; Geunes, Y.; Ooms, T.; Mahieux, A.; Wilquet, V.; Chamberlain, S.; Robert, S.; Thomas, I. R.; Erard, S.; Cecconi, B.; Le Sidaner, P.; Vandaele, A. C.

    2018-01-01

    Venus Express SOIR profiles of pressure, temperature and number densities of different constituents of the mesosphere and lower thermosphere of Venus are the only experimental data covering the 60 km to 220 km range of altitudes at the terminator of Venus. This unique dataset is now available in the open access VESPA infrastructure. This paper describes the content of these data products and provides some use cases.

  11. Investigation of winds in Venus mesosphere by digital method using UV images from VMC aboard Venus Express.

    Science.gov (United States)

    Patsaeva, Marina; Khatuntsev, Igor; Ignatiev, Nikolai

    2013-04-01

    Investigation of winds at the top cloud layer is important for understanding the global circulation of the Venus atmosphere. The Venus Monitoring Camera (VMC) aboard Venus Express has acquired a huge number of UV (365 nm) images. UV images of top cloud layer are customary to obtain the wind velocity due to their high contrast. Visual estimation of wind velocities is a labor intensive procedure. Authors have developed a digital method to estimate velocities of shifts of cloud details. The method is based on analysis of correlations between two UV images acquired at different moments. The method takes into account the change of a correlation function due to latitudinal peculiarities of cloud morphology and eliminates image regions which are far from the sub-spacecraft point. The digital method provides with good vector coverage of the Venus day side (9-16 local time) from the equator to high latitudes. The best agreement between the digital and visual methods is observed at low latitudes (below 35S). The discrepancy at higher latitudes is related to complicated cloud morphology, namely domination of streaks, which increases errors in the zonal wind speed. The method is productive for long-scale circulation at the top cloud layer. Sizes of regions for correlation were chosen empirically as a trade-off of sensitivity against noise immunity and varies from 10x7.5 ° to 20x10 ° depending on grid step. 580 orbits covering ten Venus years have been processed by using the digital method. The database of shift vectors counts about 400000 records. The mean wind speed at low latitudes is about 100 m/s. Wind vector fields were obtained for every orbit. The zonal wind speed in the equatorial region exhibits short-period (about 4.8 days) and long-period variations (long-term trend). Vector field averaged by all orbits show deviations of the main stream up to 5 degrees poleward in the early afternoon (12.5-14.5h) at 45-55S. The mean absolute value of the wind speed increases from

  12. Characterization of Earth as an exoplanet on the basis of VIRTIS-Venus Express data analysis.

    Science.gov (United States)

    Oliva, Fabrizio; Piccioni, Giuseppe; D'Aversa, Emiliano; Bellucci, Giancarlo; Sindoni, Giuseppe; Grassi, Davide; Filacchione, Gianrico; Tosi, Federico; Capaccioni, Fabrizio

    2017-04-01

    The Visible and InfraRed Thermal Imaging Spectrometer (VIRTIS, Piccioni et al., 2007) on board the Venus Express spacecraft observed the planet Earth several times in the course of the mission. In particular, a subset of 48 observations has been taken from a distance at which our planet is imaged at sub-pixel size, as exoplanets are observed using current technologies. We studied this full subset to understand which spectral signatures, related to different surface and cloud types, can be identified from the integrated planet spectrum. As expected, we found that the cloud coverage has a key role in the identification of surface features and that vegetation is very difficult to be detected. To validate our results we built a simple tool capable to simulate observations of an Earth-like planet as seen from a VIRTIS-like spectrometer in the 0.3 - 5.0 μm range. The illumination and viewing geometries, along with the spectrometer instantaneous field of view and spectral grid and sampling, can be defined by the user. The spectral endmembers used to generate the planet have been selected from an observation of Earth registered from the instrument VIRTIS on board the ESA mission Rosetta, with similar characteristics, during the third flyby of the spacecraft around our planet, occurred in November 2009. Hence, we simulated planets made of: vegetation, desert, ocean, water ice clouds and liquid water clouds. Using different amounts for each spectral class we inferred the percentages that are required to identify each class when all the spectral information is integrated into a single pixel. The outcome of this analysis confirms that clouds are not a negligible issue in the research for spectral signatures, in particular those related to the habitability of a planet and its climate conditions, even when the cloud coverage is not so high. Acknowledgements: This study has been performed within the WOW project financed by INAF and thanks to the support from the Italian Space

  13. The Quasi-monochromatic ULF Wave Boundary in the Venusian Foreshock: Venus Express Observations

    Science.gov (United States)

    Shan, Lican; Mazelle, Christian; Meziane, Karim; Romanelli, Norberto; Ge, Yasong S.; Du, Aimin; Lu, Quanming; Zhang, Tielong

    2018-01-01

    The location of ultralow-frequency (ULF) quasi-monochromatic wave onset upstream of Venus bow shock is explored using Venus Express magnetic field data. We report the existence of a spatial foreshock boundary behind which ULF waves are present. We have found that the ULF wave boundary at Venus is sensitive to the interplanetary magnetic field (IMF) direction like the terrestrial one and appears well defined for a cone angle larger than 30°. In the Venusian foreshock, the inclination angle of the wave boundary with respect to the Sun-Venus direction increases with the IMF cone angle. We also found that for the IMF nominal direction (θBX = 36°) at Venus' orbit, the value of this inclination angle is 70°. Moreover, we have found that the inferred velocity of an ion traveling along the ULF boundary is in a qualitative agreement with a quasi-adiabatic reflection of a portion of the solar wind at the bow shock. For an IMF nominal direction at Venus, the inferred bulk speed of ions traveling along this boundary is 1.07 VSW, sufficiently enough to overcome the solar wind convection. This strongly suggests that the backstreaming ions upstream of the Venusian bow shock provide the main energy source for the ULF waves.

  14. Winds in the Middle Cloud Deck From the Near-IR Imaging by the Venus Monitoring Camera Onboard Venus Express

    Science.gov (United States)

    Khatuntsev, I. V.; Patsaeva, M. V.; Titov, D. V.; Ignatiev, N. I.; Turin, A. V.; Fedorova, A. A.; Markiewicz, W. J.

    2017-11-01

    For more than 8 years the Venus Monitoring Camera (VMC) onboard the Venus Express orbiter performed continuous imaging of the Venus cloud layer in UV, visible and near-IR filters. We applied the correlation approach to sequences of the near-IR images at 965 nm to track cloud features and determine the wind field in the middle and lower cloud (49-57 km). From the VMC images that spanned from December of 2006 through August of 2013 we derived zonal and meridional components of the wind field. In low-to-middle latitudes (5-65°S) the velocity of the retrograde zonal wind was found to be 68-70 m/s. The meridional wind velocity slowly decreases from peak value of +5.8 ± 1.2 m/s at 15°S to 0 at 65-70°S. The mean meridional speed has a positive sign at 5-65°S suggesting equatorward flow. This result, together with the earlier measurements of the poleward flow at the cloud tops, indicates the presence of a closed Hadley cell in the altitude range 55-65 km. Long-term variations of zonal and meridional velocity components were found during 1,200 Earth days of observation. At 20° ± 5°S the zonal wind speed increases from -67.18 ± 1.81 m/s to -77.30 ± 2.49 m/s. The meridional wind gradually increases from +1.30 ± 1.82 m/s to +8.53 ± 2.14 m/s. Following Bertaux et al. (2016) we attribute this long-term trend to the influence from the surface topography on the dynamical process in the atmosphere via the upward propagation of gravity waves that became apparent in the VMC observations due to slow drift of the Venus Express orbit over Aphrodite Terra.

  15. Study of upper haze of Venus from Venus Express SPICAV-IR data

    Science.gov (United States)

    Luginin, Mikhail; Fedorova, Anna; Belyaev, Denis; Montmessin, Franck; Wilquet, Valerie; Korablev, Oleg; Bertaux, Jean-Loup; Carine Vandaele, Ann

    2017-04-01

    The upper haze of Venus located at 70-90 km is composed of submicron aerosol particles of H2SO4 (Esposito et al., 1983). Three channels of SPICAV/SOIR instrument onboard the VEX orbiter provided the occultation profiles in three spectral ranges that resulted in the discovery of the bimodal nature of the size distribution in the upper haze comprising a mode with a radius of 0.1-0.3 μm, and a coarser mode of radius 0.4-1.0 μm; while the presence of detached haze layers was also reported (Montmessin et al., 2008; Wilquet et al., 2009). Recently, results from 222 SPICAV-IR solar occultations observed from May 2006 to November 2014 were reported (Luginin et al., 2016). Microphysical properties of the mesospheric haze were derived from the vertical profiles of atmospheric extinction obtained at 10 near-IR wavelengths. Bimodal distribution of particles was found to be consistent with data for some orbits with mean radius for mode 1 reff1=0.12±0.03 μm and reff2=0.84±0.16 μm for mode 2. The radius for the single mode case was found to be Reff=0.54±0.25 μm, being 1.5 to 2 times smaller at polar region (60°N-90°N). In the bimodal case the number density profiles decreased smoothly for both modes, from 500 cm-3 at 75 km to 50 cm-3 at 90 km for mode 1, and from 1 cm-3 at 75 km to 0.1 cm-3 at 90 km for mode 2. In this paper, we pursue the study of the aerosols in the Venus' upper haze. Scale heights were retrieved from 43 number density profiles in unimodal case. The mean scale height is found to be 3.6 ± 0.7 km. Scale height is larger at polar region than at middle latitudes both on morning and evening terminators ( 5 km at 85°N vs 2 km at 70°N). Retrieved scale heights is consistent with a mean upward motion of 1 mm/s at 80 km and 1 cm/s at 90 km. In several occultations, detached haze layers at altitudes between 70 and 90 km were observed. The structures sometimes can be observed over consecutive orbits. In some instances, detached haze layers are shifted in

  16. Analysis of Venusian Atmospheric Two-Dimensional Winds and Features Using Venus Express, Akatsuki, and Ground-Based Images

    Science.gov (United States)

    McCabe, Ryan M.; Gunnarson, Jacob; Sayanagi, Kunio M.; Blalock, John J.; Peralta, Javier; Gray, Candace L.; McGouldrick, Kevin; Imamura, Takeshi; Watanabe, Shigeto

    2017-10-01

    We investigate the horizontal dynamics of Venus’s atmosphere at cloud-top level. In particular, we focus on the atmospheric superrotation, in which the equatorial atmosphere rotates with a period of approximately 4-5 days (~60 times faster than the solid planet). The superrotation’s forcing and maintenance mechanisms remain to be explained. Temporal evolution of the zonal (latitudinal direction) wind could reveal the transport of energy and momentum in/out of the equatorial region, and eventually shed light on mechanisms that maintain the Venusian superrotation. As a first step, we characterize the zonal mean wind field of Venus between 2006 and 2013 in ultraviolet images captured by the Venus Monitoring Camera (VMC) on board the ESA Venus Express (VEX) spacecraft which observed Venus’s southern hemisphere. Our measurements show that, between 2006 and 2013, the westward wind speed at mid- to equatorial latitudes exhibit an increase of ~20 m/s; these results are consistent with previous studies by Kouyama et al. 2013 and Khatuntsev et al. 2013. The meridional component of the wind could additionally help us characterize large-scale cloud features and their evolution that may be connected to such superrotation. We also conduct ground-based observations contemporaneously with JAXA’s Akatsuki orbiter at the 3.5 m Astrophysical Research Consortium (ARC) telescope at the Apache Point Observatory (APO) in Sunspot, NM to extend our temporal coverage to present. Images we have captured at APO to date demonstrate that, even under unfavorable illumination, it is possible to see large features that could be used for large-scale feature tracking to be compared to images taken by Akatsuki. Our work has been supported by the following grants: NASA PATM NNX14AK07G, NASA MUREP NNX15AQ03A, NSF AAG 1212216, and JAXA’s ITYF Fellowship.Kouyama, T. et al (2013), J. Geophys. Res. Planets, 118, 37-46, doi:10.1029/2011JE004013.Khatuntsev et al. (2013), Icarus, 226, 140-158, doi

  17. Access to VIRTIS / Venus-Express post-operations data archive

    Science.gov (United States)

    Erard, Stéphane; Drossart, Pierre; Piccioni, Giuseppe; Henry, Florence; Politi, Romolo

    2016-10-01

    All data acquired during the Venus-Express mission are publicly available on ESA's Planetary Science Archive (PSA). The PSA itself is being redesigned to provide more comprehensive access to its content and a new interface is expected to be ready in the coming months.However, an alternative access to the VIRTIS/VEx dataset is also provided in the PI institutes as part of the Europlanet-2020 European programme. The VESPA user interface (http://vespa.obspm.fr) provides a query mechanism based on observational conditions and instrument parameters to select data cubes of interest in the PSA and to connect them to standard plotting and analysis tools. VESPA queries will also identify related data in other datasets responsive to this mechanism, e. g., contextual images or dynamic simulations of the atmosphere, including outcomes of the EuroVenus programme funded by the EU. A specific on-line spectral cube viewer has been developed at Paris Observatory (http://voplus.obspm.fr/apericubes/js9/demo.php). Alternative ways to access the VIRTIS data are being considered, including python access to PDS3 data (https://github.com/VIRTIS-VEX/VIRTISpy) and distribution in NetCDF format on IAPS website (http://planetcdf.iaps.inaf.it). In the near future, an extended data service will provide direct access to individual spectra on the basis of viewing angles, time, and location.The next step will be to distribute products derived from data analysis, such as surface and wind maps, atmospheric profiles, movies of the polar vortices or O2 emission on the night side, etc. Such products will be accessed in a similar way, and will make VIRTIS results readily available for future Venus studies. Similar actions are taken in the frame of Europlanet concerning atmospheric data from the Mars-Express mission and Cassini observations of Titan.

  18. A new view of Earth's sister: Insights following nine years of Venus Express observations

    Science.gov (United States)

    Titov, Dmitrij; Svedhem, Håkan; Drossart, Pierre; Taylor, Fredric W.; Zhang, Tielong; Barabash, Stas; Paetzold, Martin; Piccioni, Giuseppe; Markiewicz, Wojciech; Vandaele, Ann C.; Wilson, Colin; Bertaux, Jean-Loup

    Since April 2006 ESA’s Venus Express has been performing a global survey of the remarkably dense, cloudy, and dynamic atmosphere of our near neighbour. The mission delivers comprehensive data on the temperature structure, the atmospheric composition, the cloud morphology, the atmospheric dynamics, the solar wind interaction and the escape processes. Vertical profiles of the atmospheric temperature show strong latitudinal trend in the mesosphere and upper troposphere correlated with changes in the cloud top structure and indicate convective instability in the main cloud deck at 50-60 km. Observations reveal significant latitudinal variations and temporal changes in the global cloud top morphology, which modulate the solar energy deposited in the atmosphere. The cloud top altitude varies from 72 km in the low and middle latitudes to 64 km in the polar region, correlated with decrease of the aerosol scale height from 4±1.6 km to 1.7±2.4 km, marking vast polar depression. UV imaging shows for the first time the middle latitudes and polar regions in unprecedented detail. The eye of the Southern polar vortex was found to be a strongly variable feature with complex dynamics. Solar occultation observations and deep atmosphere spectroscopy in spectral transparency windows mapped the distribution of the major trace gases H _{2}O, SO _{2}, CO, COS and their variations above and below the clouds, revealing key features of the dynamical and chemical processes at work. Tracking motions of cloud features provided the most complete characterization of the mean atmospheric circulation as well as its variability. Low and middle latitudes show an almost constant zonal wind speed at the cloud tops and vertical wind shear of 2-3 m/s/km. The zonal wind speed increased from 84±20 m/s to 110±16 m/s over the course of the mission. Towards the pole, the wind speed drops quickly and the vertical shear vanishes. The meridional poleward wind ranges from 0 at equator to about 15 m/s in

  19. Detailed Expression Pattern of Aldolase C (Aldoc) in the Cerebellum, Retina and Other Areas of the CNS Studied in Aldoc-Venus Knock-In Mice

    Science.gov (United States)

    Ajioka, Itsuki; Yamazaki, Maya; Abe, Manabu; Oh-Nishi, Arata; Sakimura, Kenji; Sugihara, Izumi

    2014-01-01

    Aldolase C (Aldoc, also known as “zebrin II”), a brain type isozyme of a glycolysis enzyme, is expressed heterogeneously in subpopulations of cerebellar Purkinje cells (PCs) that are arranged longitudinally in a complex striped pattern in the cerebellar cortex, a pattern which is closely related to the topography of input and output axonal projections. Here, we generated knock-in Aldoc-Venus mice in which Aldoc expression is visualized by expression of a fluorescent protein, Venus. Since there was no obvious phenotypes in general brain morphology and in the striped pattern of the cerebellum in mutants, we made detailed observation of Aldoc expression pattern in the nervous system by using Venus expression in Aldoc-Venus heterozygotes. High levels of Venus expression were observed in cerebellar PCs, cartwheel cells in the dorsal cochlear nucleus, sensory epithelium of the inner ear and in all major types of retinal cells, while moderate levels of Venus expression were observed in astrocytes and satellite cells in the dorsal root ganglion. The striped arrangement of PCs that express Venus to different degrees was carefully traced with serial section alignment analysis and mapped on the unfolded scheme of the entire cerebellar cortex to re-identify all individual Aldoc stripes. A longitudinally striped boundary of Aldoc expression was first identified in the mouse flocculus, and was correlated with the climbing fiber projection pattern and expression of another compartmental marker molecule, heat shock protein 25 (HSP25). As in the rat, the cerebellar nuclei were divided into the rostrodorsal negative and the caudoventral positive portions by distinct projections of Aldoc-positive and negative PC axons in the mouse. Identification of the cerebellar Aldoc stripes in this study, as indicated in sample coronal and horizontal sections as well as in sample surface photos of whole-mount preparations, can be referred to in future experiments. PMID:24475166

  20. VIRTIS on Venus Express thermal emission spectra near 1μm

    Science.gov (United States)

    Mueller, Nils; Tsang, Constantine; Helbert, Joern; Smrekar, Suzanne; Piccioni, Giuseppe; Drossart, Pierre

    2016-10-01

    Thermal emission from the surface of Venus is observable through narrow spectral windows close to 1μm. Surface temperature is strongly constrained by surface elevation, due to the thick and dense atmosphere. The data from Visible and InfraRed Thermal Imaging Spectrometer VIRTIS on Venus Express together with altimetry constrain surface emissivity. In VIRTIS observations at 1.02μm, strongly deformed highland plateaus (tesserae) appear to have a lower emissivity consistent with continental crust, an interpretation that implies existence of an early ocean. Comparison between the Magellan stereo digital elevation model (DEM) and altimetry shows that the altimetry height error in rough tesserae greatly exceeds the formal error. In the one tesserae outlier covered by altimetry, DEM, and VIRTIS, the height error could account for the observed emissivity variation. The radiances observed at 1.10 and 1.18μm have a different response to topography, mostly due to spectrally varying absorption in the overlying atmospheric column. Thus if the tesserae have the same emissivity as volcanic plains, its spectrum should be the same as that of plains of the correct surface elevation. In order to investigate this statistically, we create a database of all long exposure duration VIRTIS spectra in the range of 1 - 1.4μm. The spectra are corrected for the ubiquitous straylight from the dayside, based on analysis of spectra showing deep space. Because the 1.10 and 1.18μm peaks are narrow compared to the variation of instrument spectral registration, we fit each spectrum with a synthetic spectrum from an atmospheric radiative transfer model, using wavelength offset and bandwidths as parameters in addition to atmospheric variables. This dataset of ~28 million thermal emission spectra spans a wide range of southern latitudes and night local times, and thus may be useful for studies beyond the question of surface emissivity. A portion of this research was conducted at the Jet Propulsion

  1. Venus: Our Misunderstood Sister

    Science.gov (United States)

    Dyar, Darby; Smrekar, Suzanne E.

    2018-01-01

    Of all known bodies in the galaxy, Venus is the most Earth-like in size, composition, surface age, and incoming energy. As we search for habitable planets around other stars, learning how Venus works is critical to understanding how Earth evolved to host life, and whether rocky exoplanets in stars’ habitable zones are faraway Earths or Venuses. What caused Venus’ path to its present hostile environment, devoid of oceans, magnetic field, and plate tectonics? This talk reviews recent mission results, presents key unresolved science questions, and describes proposed missions to answer these questions.Despite its importance in understanding habitability, Venus is the least-explored rocky planet, last visited by NASA in 1994. Fundamental, unanswered questions for Venus include: 1. How did Venus evolve differently? 2. How have volatiles shaped its evolution? 3. Did Venus catastrophically resurface? 4. What geologic processes are active today? 5. Why does Venus lack plate tectonics?On Earth, plate tectonics supports long-term climate stability and habitability by cycling volatiles in and out of the mantle. New information on planetary volatiles disputes the long-held notion that Venus’ interior is dry; several lines of evidence indicate that planets start out wet, creating long-term atmospheres by outgassing. ESA’s Venus Express mission provided evidence for recent and ongoing volcanism and for Si-rich crust like Earth’s continents. New hypotheses suggest that lithospheric temperature can explain why Venus lacks tectonics, and are consistent with present-day initiation of subduction on Venus.New data are needed to answer these key questions of rocky planet evolution. Orbital IR data can be acquired through windows in Venus’ CO2-rich atmosphere, informing surface mineralogy, rock types, cloud variations, and active volcanism. High resolution gravity, radar, and topography data along with mineralogical constraints must be obtained. Mineralogy and geochemistry

  2. Meeting Venus

    Science.gov (United States)

    Sterken, Christiaan; Aspaas, Per Pippin

    2013-06-01

    On 2-3 June 2012, the University of Tromsoe hosted a conference about the cultural and scientific history of the transits of Venus. The conference took place in Tromsoe for two very specific reasons. First and foremost, the last transit of Venus of this century lent itself to be observed on the disc of the Midnight Sun in this part of Europe during the night of 5 to 6 June 2012. Second, several Venus transit expeditions in this region were central in the global enterprise of measuring the scale of the solar system in the eighteenth century. The site of the conference was the Nordnorsk Vitensenter (Science Centre of Northern Norway), which is located at the campus of the University of Tromsoe. After the conference, participants were invited to either stay in Tromsoe until the midnight of 5-6 June, or take part in a Venus transit voyage in Finnmark, during which the historical sites Vardoe, Hammerfest, and the North Cape were to be visited. The post-conference program culminated with the participants observing the transit of Venus in or near Tromsoe, Vardoe and even from a plane near Alta. These Proceedings contain a selection of the lectures delivered on 2-3 June 2012, and also a narrative description of the transit viewing from Tromsoe, Vardoe and Alta. The title of the book, Meeting Venus, refers the title of a play by the Hungarian film director, screenwriter and opera director Istvan Szabo (1938-). The autobiographical movie Meeting Venus (1991) directed by him is based on his experience directing Tannhauser at the Paris Opera in 1984. The movie brings the story of an imaginary international opera company that encounters a never ending series of difficulties and pitfalls that symbolise the challenges of any multicultural and international endeavour. As is evident from the many papers presented in this book, Meeting Venus not only contains the epic tales of the transits of the seventeenth, eighteenth and nineteenth centuries, it also covers the conference

  3. Venus Middle Atmosphere Chemistry

    Science.gov (United States)

    Mills, F. P.; Sundaram, M.; Slanger, T. G.; Allen, M.; Yung, Y. L.

    2005-08-01

    Venus is the most similar planet to Earth, and years of research have sought to understand their similarities and differences. Yet, it is still not clear what chemical processes maintain the long-term stability of Venus' primarily CO2 atmosphere. CO2 dissociates into CO and O after absorbing photons at wavelengths Express will be reviewed. Recent work evaluating newly proposed mechanisms for producing CO2, which could be important depending on the rates of poorly constrained reactions, will be described. This research was supported by funding from NASA's Planetary Atmospheres program and the Australian Research Council. Part of this work was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. [1] Nair, et al., Icarus 111, 124 (1994), [2] Trauger and Lunine, Icarus 55, 272 (1983), [3] Pernice, et al., PNAS 101, 14007 (2004)

  4. Sulfur dioxide in the Venus atmosphere: I. Vertical distribution and variability

    Science.gov (United States)

    Vandaele, A. C.; Korablev, O.; Belyaev, D.; Chamberlain, S.; Evdokimova, D.; Encrenaz, Th.; Esposito, L.; Jessup, K. L.; Lefèvre, F.; Limaye, S.; Mahieux, A.; Marcq, E.; Mills, F. P.; Montmessin, F.; Parkinson, C. D.; Robert, S.; Roman, T.; Sandor, B.; Stolzenbach, A.; Wilson, C.; Wilquet, V.

    2017-10-01

    Recent observations of sulfur containing species (SO2, SO, OCS, and H2SO4) in Venus' mesosphere have generated controversy and great interest in the scientific community. These observations revealed unexpected spatial patterns and spatial/temporal variability that have not been satisfactorily explained by models. Sulfur oxide chemistry on Venus is closely linked to the global-scale cloud and haze layers, which are composed primarily of concentrated sulfuric acid. Sulfur oxide observations provide therefore important insight into the on-going chemical evolution of Venus' atmosphere, atmospheric dynamics, and possible volcanism. This paper is the first of a series of two investigating the SO2 and SO variability in the Venus atmosphere. This first part of the study will focus on the vertical distribution of SO2, considering mostly observations performed by instruments and techniques providing accurate vertical information. This comprises instruments in space (SPICAV/SOIR suite on board Venus Express) and Earth-based instruments (JCMT). The most noticeable feature of the vertical profile of the SO2 abundance in the Venus atmosphere is the presence of an inversion layer located at about 70-75 km, with VMRs increasing above. The observations presented in this compilation indicate that at least one other significant sulfur reservoir (in addition to SO2 and SO) must be present throughout the 70-100 km altitude region to explain the inversion in the SO2 vertical profile. No photochemical model has an explanation for this behaviour. GCM modelling indicates that dynamics may play an important role in generating an inflection point at 75 km altitude but does not provide a definitive explanation of the source of the inflection at all local times or latitudes The current study has been carried out within the frame of the International Space Science Institute (ISSI) International Team entitled 'SO2 variability in the Venus atmosphere'.

  5. Investigating gravity waves evidences in the Venus upper atmosphere

    Science.gov (United States)

    Migliorini, Alessandra; Altieri, Francesca; Shakun, Alexey; Zasova, Ludmila; Piccioni, Giuseppe; Bellucci, Giancarlo; Grassi, Davide

    2014-05-01

    We present a method to investigate gravity waves properties in the upper mesosphere of Venus, through the O2 nightglow observations acquired with the imaging spectrometer VIRTIS on board Venus Express. Gravity waves are important dynamical features that transport energy and momentum. They are related to the buoyancy force, which lifts air particles. Then, the vertical displacement of air particles produces density changes that cause gravity to act as restoring force. Gravity waves can manifest through fluctuations on temperature and density fields, and hence on airglow intensities. We use the O2 nightglow profiles showing double peaked structures to study the influence of gravity waves in shaping the O2 vertical profiles and infer the waves properties. In analogy to the Earth's and Mars cases, we use a well-known theory to model the O2 nightglow emissions affected by gravity waves propagation. Here we propose a statistical discussion of the gravity waves characteristics, namely vertical wavelength and wave amplitude, with respect to local time and latitude. The method is applied to about 30 profiles showing double peaked structures, and acquired with the VIRTIS/Venus Express spectrometer, during the mission period from 2006-07-05 to 2008-08-15.

  6. Return to Venus of AKATSUKI, the Japanese Venus Orbiter

    Science.gov (United States)

    Nakamura, M.; Iwagami, N.; Satoh, T.; Taguchi, M.; Watanabe, S.; Takahashi, Y.; Imamura, T.; Suzuki, M.; Ueno, M.; Yamazaki, A.; Fukuhara, T.; Yamada, M.; Ishii, N.; Ogohara, K.

    2011-12-01

    Japanese Venus Climate Orbiter 'AKATSUKI' (PLANET-C) was proposed in 2001 with strong support by international Venus science community and approved as an ISAS mission soon after the proposal. AKATSUKI and ESA's Venus Express complement each other in Venus climate study. Various coordinated observations using the two spacecraft have been planned. Also participating scientists from US have been selected. Its science target is to understand the climate of Venus. The mission life we expected was more than 2 Earth years in Venus orbit. AKATSUKI was successfully launched at 06:58:22JST on May 21, by H-IIA F17. After the separation from H-IIA, the telemetry from AKATSUKI was normally detected by DSN Goldstone station (10:00JST) and the solar cell paddles' expansion was confirmed. AKATSUKI was put into the 3-axis stabilized mode in the initial operation from Uchinoura station and the critical operation was finished at 20:00JST on the same day. The malfunction, which happened during the Venus Orbit Insertion (VOI) on7 Dec, 2010 is as follows. We set all commands on Dec. 5. Attitude control for Venus orbit insertion (VOI) was automatically done on Dec. 6. Orbital maneuver engine (OME) was fired 08:49 JST on Dec. 7. 1min. after firing the spacecraft went into the occultation region and we had no telemetry, but we expected to continuous firing for 12min. Recording on the spacecraft told us later that, unfortunately the firing continued just 152sec. and stopped. The reason of the malfunction of the OME was the blocking of check valve of the gas pressure line to push the fuel to the engine. We failed to make the spacecraft the Venus orbiter, and it is rotating the sun with the orbital period of 203 days. As the Venus orbit the sun with the period of 225 days, AKATSUKI has a chance to meet Venus again in 5 or 6 years depending on the orbit correction plan. Let us summarize the present situation of AKATSUKI. Most of the fuel still remains. But the condition of the propulsion

  7. Venus's southern polar vortex reveals precessing circulation.

    Science.gov (United States)

    Luz, D; Berry, D L; Piccioni, G; Drossart, P; Politi, R; Wilson, C F; Erard, S; Nuccilli, F

    2011-04-29

    Initial images of Venus's south pole by the Venus Express mission have shown the presence of a bright, highly variable vortex, similar to that at the planet's north pole. Using high-resolution infrared measurements of polar winds from the Venus Express Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument, we show the vortex to have a constantly varying internal structure, with a center of rotation displaced from the geographic south pole by ~3 degrees of latitude and that drifts around the pole with a period of 5 to 10 Earth days. This is indicative of a nonsymmetric and varying precession of the polar atmospheric circulation with respect to the planetary axis.

  8. Venus cartography

    Science.gov (United States)

    Batson, R. M.; Kirk, R. L.; Edwards, Kathleen; Morgan, H. F.

    1994-01-01

    The entire surface of the planet Venus is being mapped at global and regional scales (1:50 million through 1:1.5 million) with synthetic aperture radar (SAR), radar altimeter, and radiometer measurements of physical properties from the Magellan spacecraft. The mapping includes SAR image mosaics, shaded relief maps, and topographic contour overlays made from altimetry data and by radargrammetric methods. Methods used include new techniques of radar image processing that became operational as a result of the Magellan mission. Special cartographic support products prepared by the USGS include: synthetic stereograms, color thematic maps of physical properties, digital shaded relief maps from opposite-look SAR, and topographic maps by radargrammetry. The area being mapped (at a resolution of 75 m/pixel) is roughly equivalent to that of Earth, including seafloors. The mapping is designed to support geologic and geophysical investigations.

  9. Scattering Properties of the Venusian Clouds Observed by the UV Imager on board Akatsuki

    Science.gov (United States)

    Lee, Y. J.; Yamazaki, A.; Imamura, T.; Yamada, M.; Watanabe, S.; Sato, T. M.; Ogohara, K.; Hashimoto, G. L.; Murakami, S.

    2017-08-01

    We analyze the albedo of Venus obtained from the UV Imager on board Akatsuki. A relative global mean albedo over phase angle is used in this study, and we confirm the glory feature at 283 and 365 nm in the data acquired in 2016 May. We successfully simulate the observation using a radiative transfer model. Our results show that cloud aerosols of {r}{eff}=1.26 μm and {v}{eff}=0.076 (mode 2) can explain the glory, consistent with a property of aerosols previously suggested by using the Venus Monitoring Camera on board Venus Express. We find that SO2 and the unknown UV absorber are necessary factors to explain the decreasing trend of the observed relative albedo at phase angles larger than 10°. We suggest a range of possible SO2 abundance from 80 to 400 ppbv at the cloud top level, depending on atmospheric conditions assumed.

  10. Venus Exploration opportunities within NASA's Solar System Exploration roadmap

    Science.gov (United States)

    Balint, Tibor; Thompson, Thomas; Cutts, James; Robinson, James

    2006-01-01

    Science goals to understand the origin, history and environment of Venus have been driving international space exploration missions for over 40 years. Past missions include the Magellan and Pioneer-Venus missions by the US; the Venera program by the USSR; and the Vega missions through international cooperation. Furthermore, the US National Research Council (NRC), in the 2003 Solar System Exploration (SSE) Decadal Survey, identified Venus as a high priority target, thus demonstrating a continuing interest in Earth's sister planet. In response to the NRC recommendation, the 2005 NASA SSE Roadmap included a number of potential Venus missions arching through all mission classes from small Discovery, to medium New Frontiers and to large Flagship class missions. While missions in all of these classes could be designed as orbiters with remote sensing capabilities, the desire for scientific advancements beyond our current knowledge - including what we expect to learn from the ongoing ESA Venus Express mission - point to in-situ exploration of Venus.

  11. Reassessment of planetary protection requirements for Venus missions

    Science.gov (United States)

    Szostak, J.; Riemer, R.; Smith, D.; Rummel, J.

    In 2005 the US Space Studies Board SSB was asked by NASA to reexamine the planetary protection requirements for spacecraft missions to Venus In particular the SSB was tasked to 1 Assess the surface and atmospheric environments of Venus with respect to their ability to support the survival and growth of Earth-origin microbial contamination by future spacecraft missions and 2 Provide recommendations related to planetary protection issues associated with the return to Earth of samples from Venus The task group established by the SSB to address these issues assessed the known aspects of the present-day environment of Venus and the ability of Earth organisms to survive in the physical and chemical conditions found on the planet s surface or in the clouds in the planet s atmosphere As a result of its deliberations the task group found compelling evidence against there being significant dangers of forward or reverse biological contamination as a result of contact between a spacecraft and the surface of Venus or the clouds in the atmosphere of Venus regardless of the current unknowns The task group did however conclude that Venus is a body of interest relative to the process of chemical evolution and the origin of life As a result the task group endorses NASA s current policy of subjecting missions to Venus to the requirements imposed by planetary protection Category II rather than the less restrictive Category I recommended by COSPAR

  12. Venus - Ishtar gravity anomaly

    Science.gov (United States)

    Sjogren, W. L.; Bills, B. G.; Mottinger, N. A.

    1984-01-01

    The gravity anomaly associated with Ishtar Terra on Venus is characterized, comparing line-of-sight acceleration profiles derived by differentiating Pioneer Venus Orbiter Doppler residual profiles with an Airy-compensated topographic model. The results are presented in graphs and maps, confirming the preliminary findings of Phillips et al. (1979). The isostatic compensation depth is found to be 150 + or - 30 km.

  13. Venus 2000 Mission Design

    Science.gov (United States)

    Folta, David; Marr, Greg; Vaughn, Frank; Houghton, Martin B.

    1997-01-01

    As part of the Discovery Program, National Aeronautics and Space Administration (NASA) has solicited proposals for inter-planetary research to conduct solar system exploration science investigations. A mission, called Venus 2000 (V2k), has been proposed for exploration of the Venus Atmosphere. This is NASAs first voyage to Venus to investigate key science objectives since Magellan and will be launched in summer 2002. In keeping with discovery program requirements to reduce total mission cost and utilize new technology, V2k mission design and control will focus on the use of innovative and proven trajectory analysis programs and control systems provided by the Goddard Space Flight Center (GSFC).

  14. Transits of Venus and Mercury as muses

    Science.gov (United States)

    Tobin, William

    2013-11-01

    Transits of Venus and Mercury have inspired artistic creation of all kinds. After having been the first to witness a Venusian transit, in 1639, Jeremiah Horrocks expressed his feelings in poetry. Production has subsequently widened to include songs, short stories, novels, novellas, sermons, theatre, film, engravings, paintings, photography, medals, sculpture, stained glass, cartoons, stamps, music, opera, flower arrangements, and food and drink. Transit creations are reviewed, with emphasis on the English- and French-speaking worlds. It is found that transits of Mercury inspire much less creation than those of Venus, despite being much more frequent, and arguably of no less astronomical significance. It is suggested that this is primarily due to the mythological associations of Venus with sex and love, which are more powerful and gripping than Mercury's mythological role as a messenger and protector of traders and thieves. The lesson for those presenting the night sky to the public is that sex sells.

  15. Venus Crater Database

    Data.gov (United States)

    National Aeronautics and Space Administration — This web page leads to a database of images and information about the 900 or so impact craters on the surface of Venus by diameter, latitude, and name.

  16. Venus Landsailing Rover

    Data.gov (United States)

    National Aeronautics and Space Administration — NASA Glenn has developed electronics and low-power photovoltaics that will continue to function even at the Venus temperature of 450°C. So the fundamental elements...

  17. Venus Elongation Measurements for the Transit of Venus, using the ...

    Indian Academy of Sciences (India)

    Home; Journals; Resonance – Journal of Science Education; Volume 9; Issue 11. Venus Elongation Measurements for the Transit of Venus, using the Historical Jantar Mantar Observatory. N Rathnasree. Classroom Volume 9 Issue 11 November 2004 pp 46-55 ...

  18. Mathematical adventures in performance analysis from storage systems, through airplane boarding, to express line queues

    CERN Document Server

    Bachmat, Eitan

    2014-01-01

    This monograph describes problems in the field of performance analysis, primarily the study of storage systems and the diverse mathematical techniques that are required for solving such problems. Topics covered include best practices for scheduling I/O requests to a disk drive, how this problem is related to airplane boarding, and how both problems can be modeled using space-time geometry. The author also explains how Riemann's proof of the analytic continuation and functional equation of the Riemann zeta function can be used to analyze express-line queues in a minimarket. Overall, the book reveals the surprising applicability of abstract mathematical ideas that are not usually associated with applied topics. Advanced undergraduate students or graduate students with an interest in the applications of mathematics will find this book a useful resource. It will also be of interest to professional mathematicians who want exposure to the surprising ways that theoretical mathematics may be applied to engineering pr...

  19. Venus Surface Composition Constrained by Observation and Experiment

    Science.gov (United States)

    Gilmore, Martha; Treiman, Allan; Helbert, Jörn; Smrekar, Suzanne

    2017-11-01

    New observations from the Venus Express spacecraft as well as theoretical and experimental investigation of Venus analogue materials have advanced our understanding of the petrology of Venus melts and the mineralogy of rocks on the surface. The VIRTIS instrument aboard Venus Express provided a map of the southern hemisphere of Venus at ˜1 μm allowing, for the first time, the definition of surface units in terms of their 1 μm emissivity and derived mineralogy. Tessera terrain has lower emissivity than the presumably basaltic plains, consistent with a more silica-rich or felsic mineralogy. Thermodynamic modeling and experimental production of melts with Venera and Vega starting compositions predict derivative melts that range from mafic to felsic. Large volumes of felsic melts require water and may link the formation of tesserae to the presence of a Venus ocean. Low emissivity rocks may also be produced by atmosphere-surface weathering reactions unlike those seen presently. High 1 μm emissivity values correlate to stratigraphically recent flows and have been used with theoretical and experimental predictions of basalt weathering to identify regions of recent volcanism. The timescale of this volcanism is currently constrained by the weathering of magnetite (higher emissivity) in fresh basalts to hematite (lower emissivity) in Venus' oxidizing environment. Recent volcanism is corroborated by transient thermal anomalies identified by the VMC instrument aboard Venus Express. The interpretation of all emissivity data depends critically on understanding the composition of surface materials, kinetics of rock weathering and their measurement under Venus conditions. Extended theoretical studies, continued analysis of earlier spacecraft results, new atmospheric data, and measurements of mineral stability under Venus conditions have improved our understanding atmosphere-surface interactions. The calcite-wollastonite CO2 buffer has been discounted due, among other things, to

  20. Venus Altitude Cycling Balloon Project

    Data.gov (United States)

    National Aeronautics and Space Administration — The ISTAR Group ( IG) and team mate Thin Red Line Aerospace (TRLA) propose a Venus altitude cycling balloon (Venus ACB), an innovative superpressure balloon...

  1. The Planet Venus

    Science.gov (United States)

    Luhmann, Janet

    This book is not so much for the space scientist looking for background material for research as it is for one interested in the history of planetary exploration. The first half (˜100 pps) is devoted to studies of Venus before the space age, starting at several hundred years BC. It is obvious from the multitude of detailed descriptions of observers' accounts that considerable library research went into this section. While sometimes tedious, this chronology of Venus research is punctuated with amusing facts. While many may know about the Velikovsky theory of the cometary origin of the planet, few may know that Lowell drew pictures of Cytherian canals similar to the canals of Mars or that Frederick the Great of Prussia proposed to name the (once suspected) satellite of Venus D'Alembert, after the mathematician. An equally amusing appendix shows the ups and downs of the rotation period of this planet with the invisible surface. Much attention is focused on early telescope observations, the ashen light, and transits of Venus. At the end of this half, one appreciates that Venus has played a fairly important role in history in the areas of religion, science, and technology.

  2. Entry at Venus

    Science.gov (United States)

    Venkatapathy, Ethiraj; Smith, Brandon

    2016-01-01

    This is lecture to be given at the IPPW 2016, as part of the 2 day course on Short Course on Destination Venus: Science, Technology and Mission Architectures. The attached presentation material is intended to be introduction to entry aspects of Venus in-situ robotic missions. The presentation introduces the audience to the aerodynamic and aerothermodynamic aspects as well as the loads, both aero and thermal, generated during entry. The course touches upon the system design aspects such as TPS design and both high and low ballistic coefficient entry system concepts that allow the science payload to be protected from the extreme entry environment and yet meet the mission objectives.

  3. From CERN to VENUS Express

    CERN Multimedia

    2005-01-01

    Participants in the 'Schweizer Jugendforscht' projects at CERN under the supervision of Günther Dissertori, professor at the Swiss Federal Institute of Technology (ETH Zürich) and other members of ETH Zürich, Werner Lustermann and Michael Dittmar. In Switzerland, as in many other countries, this year has seen a long list of activities, celebrating the centenary of Einstein's 'Annus mirabilis'. Having formerly employed Einstein, the Swiss Federal Institute of Intellectual Property in Bern made its contribution by sponsoring a special 'study week' for young high-school students, under the tutorship of 'Schweizer Jugendforscht', an organisation which supports the scientific activities of very talented young people. The organisers chose 'Mission to Jupiter's Moon, Europa' as the general theme for this study week. From 2 to 8 October 2005 several groups of students (between 16 and 19 years old) had to investigate some mission-related questions, ranging from the choice of the orbit and different ways of explor...

  4. Is Venus alive?

    Science.gov (United States)

    Taylor, Harry A., Jr.

    Apart from the earth, the near environment of only one other planet, Venus, has been the subject of sustained in situ investigations from space. Owing to the similarity in the physical characteristics of the two bodies, this is most appropriate in that it provides the opportunity to test the credo that through comparative analysis, planetary exploration holds the promise for better understanding of our earth environment.The Pioneer Venus Orbiter was placed into orbit about Venus in December 1978 and has provided a wealth of observations of the planet surface, its atmosphere and clouds, the ionosphere, and the interaction of the solar wind and interplanetary magnetic field with the planetary environment. Among these observations, perhaps the most potentially significant and yet controversial result has been the claimed evidence of extensive lightning and the coupled assertion that the lightning is stimulated by volcanic activity. This lightning- volcanism scenario has become widely publicized in films, books, and numerous journal and magazine articles. Also, these results have had considerable influence in stimulating ongoing research on the basis that active volcanic output might explain otherwise unanswered questions in wide-ranging disciplines, including atmospheric and cloud physics, geology, and plasma physics. Quite naturally, the question of whether Venus is geologically either living or dead is fundamentally significant for comparative planetary analysis.

  5. Geology of Venus

    International Nuclear Information System (INIS)

    Basilevsky, A.T.; Head, J.W. III.

    1988-01-01

    This paper summarizes the emerging picture of the surface of Venus provided by high-resolution earth-based radar telescopes and orbital radar altimetry and imaging systems. The nature and significance of the geological processes operating there are considered. The types of information needed to complete the picture are addressed. 71 references

  6. Venus Monitoring Camera (VMC/VEx) 1 micron emissivity and Magellan microwave properties of crater-related radar-dark parabolas and other terrains

    Science.gov (United States)

    Basilevsky, A. T.; Shalygina, O. S.; Bondarenko, N. V.; Shalygin, E. V.; Markiewicz, W. J.

    2017-09-01

    The aim of this work is a comparative study of several typical radar-dark parabolas, the neighboring plains and some other geologic units seen in the study areas which include craters Adivar, Bassi, Bathsheba, du Chatelet and Sitwell, at two depths scales: the upper several meters of the study object available through the Magellan-based microwave (at 12.6 cm wavelength) properties (microwave emissivity, Fresnel reflectivity, large-scale surface roughness, and radar cross-section), and the upper hundreds microns of the object characterized by the 1 micron emissivity resulted from the analysis of the near infra-red (NIR) irradiation of the night-side of the Venusian surface measured by the Venus Monitoring Camera (VMC) on-board of Venus Express (VEx).

  7. Sampling the Cloudtop Region on Venus

    Science.gov (United States)

    Limaye, Sanjay; Ashish, Kumar; Alam, Mofeez; Landis, Geoffrey; Widemann, Thomas; Kremic, Tibor

    2014-05-01

    The details of the cloud structure on Venus continue to be elusive. One of the main questions is the nature and identity of the ultraviolet absorber(s). Remote sensing observations from Venus Express have provided much more information about the ubiquitous cloud cover on Venus from both reflected and emitted radiation from Venus Monitoring Camera (VMC) and Visible InfraRed Imaging Spectrometer (VIRTIS) observations. Previously, only the Pioneer Venus Large Probe has measured the size distribution of the cloud particles, and other probes have measured the bulk optical properties of the cloud cover. However, the direct sampling of the clouds has been possible only below about 62 km, whereas the recent Venus Express observations indicate that the cloud tops extend from about 75 km in equatorial region to about 67 km in polar regions. To sample the cloud top region of Venus, other platforms are required. An unmanned aerial vehicle (UAV) has been proposed previously (Landis et al., 2002). Another that is being looked into, is a semi-buoyant aerial vehicle that can be powered using solar cells and equipped with instruments to not only sample the cloud particles, but also to make key atmospheric measurements - e.g. atmospheric composition including isotopic abundances of noble and other gases, winds and turbulence, deposition of solar and infrared radiation, electrical activity. The conceptual design of such a vehicle can carry a much more massive payload than any other platform, and can be controlled to sample different altitudes and day and night hemispheres. Thus, detailed observations of the surface using a miniature Synthetic Aperture Radar are possible. Data relay to Earth will need an orbiter, preferably in a low inclination orbit, depending on the latitude region selected for emphasis. Since the vehicle has a large surface area, thermal loads on entry are low, enabling deployment without the use of an aeroshell. Flight characteristics of such a vehicle have been

  8. Solar Wind Interaction and Impact on the Venus Atmosphere

    Science.gov (United States)

    Futaana, Yoshifumi; Stenberg Wieser, Gabriella; Barabash, Stas; Luhmann, Janet G.

    2017-11-01

    Venus has intrigued planetary scientists for decades because of its huge contrasts to Earth, in spite of its nickname of "Earth's Twin". Its invisible upper atmosphere and space environment are also part of the larger story of Venus and its evolution. In 60s to 70s, several missions (Venera and Mariner series) explored Venus-solar wind interaction regions. They identified the basic structure of the near-Venus space environment, for example, existence of the bow shock, magnetotail, ionosphere, as well as the lack of the intrinsic magnetic field. A huge leap in knowledge about the solar wind interaction with Venus was made possible by the 14-year long mission, Pioneer Venus Orbiter (PVO), launched in 1978. More recently, ESA's probe, Venus Express (VEX), was inserted into orbit in 2006, operated for 8 years. Owing to its different orbit from that of PVO, VEX made unique measurements in the polar and terminator regions, and probed the near-Venus tail for the first time. The near-tail hosts dynamic processes that lead to plasma energization. These processes in turn lead to the loss of ionospheric ions to space, slowly eroding the Venusian atmosphere. VEX carried an ion spectrometer with a moderate mass-separation capability and the observed ratio of the escaping hydrogen and oxygen ions in the wake indicates the stoichiometric loss of water from Venus. The structure and dynamics of the induced magnetosphere depends on the prevailing solar wind conditions. VEX studied the response of the magnetospheric system on different time scales. A plethora of waves was identified by the magnetometer on VEX; some of them were not previously observed by PVO. Proton cyclotron waves were seen far upstream of the bow shock, mirror mode waves were observed in magnetosheath and whistler mode waves, possibly generated by lightning discharges were frequently seen. VEX also encouraged renewed numerical modeling efforts, including fluid-type of models and particle-fluid hybrid type of models

  9. Venus gravity fields

    Science.gov (United States)

    Sjogren, W. L.; Ananda, M.; Williams, B. G.; Birkeland, P. W.; Esposito, P. S.; Wimberly, R. N.; Ritke, S. J.

    1981-01-01

    Results of Pioneer Venus Orbiter observations concerning the gravity field of Venus are presented. The gravitational data was obtained from reductions of Doppler radio tracking data for the Orbiter, which is in a highly eccentric orbit with periapsis altitude varying from 145 to 180 km and nearly fixed periapsis latitude of 15 deg N. The global gravity field was obtained through the simultaneous estimation of the orbit state parameters and gravity coefficients from long-period variations in orbital element rates. The global field has been described with sixth degree and order spherical harmonic coefficients, which are capable of resolving the three major topographical features on Venus. Local anomalies have been mapped using line-of-sight accelerations derived from the Doppler residuals between 40 deg N and 10 deg S latitude at approximately 300 km spatial resolution. Gravitational data is observed to correspond to topographical data obtained by radar altimeter, with most of the gravitational anomalies about 20-30 milligals. Simulations evaluating the isostatic states of two topographic features indicate that at least partial isostasy prevails, with the possibility of complete compensation.

  10. On the Ionospheric Holes of Venus

    Science.gov (United States)

    Collinson, G.; Fedorov, A.; Futaana, Y.; Masunaga, K.; Hartle, R. E.; Stenberg, G.; Budnik, E.; Grebowsky, J. M.; Holmstrom, M.; andre, N.; Barabash, S. V.; Zhang, T.

    2013-12-01

    One of the most intriguing unsolved mysteries that endures from the Pioneer Venus Orbiter is that of ~1000km wide ``Holes" in the nightside Ionosphere. The phenomena remains unexplained, despite their frequent observation during the first three years of the mission, and more than thirty years having elapsed since their first description in the literature. We present new observations by the ESA Venus Express of Ionospheric Holes at very high altitudes, providing us with the opportunity to study this fascinating phenomena with modern instrumentation. We discuss the insight that these new data give us into the effect of Ionospheric Holes on atmospheric escape, and the evidence that suggests that Ionospheric Holes are due to an internal planetary magnetic field.

  11. The Plains of Venus

    Science.gov (United States)

    Sharpton, V. L.

    2013-12-01

    Volcanic plains units of various types comprise at least 80% of the surface of Venus. Though devoid of topographic splendor and, therefore often overlooked, these plains units house a spectacular array of volcanic, tectonic, and impact features. Here I propose that the plains hold the keys to understanding the resurfacing history of Venus and resolving the global stratigraphy debate. The quasi-random distribution of impact craters and the small number that have been conspicuously modified from the outside by plains-forming volcanism have led some to propose that Venus was catastrophically resurfaced around 725×375 Ma with little volcanism since. Challenges, however, hinge on interpretations of certain morphological characteristics of impact craters: For instance, Venusian impact craters exhibit either radar dark (smooth) floor deposits or bright, blocky floors. Bright floor craters (BFC) are typically 100-400 m deeper than dark floor craters (DFC). Furthermore, all 58 impact craters with ephemeral bright ejecta rays and/or distal parabolic ejecta patterns have bright floor deposits. This suggests that BFCs are younger, on average, than DFCs. These observations suggest that DFCs could be partially filled with lava during plains emplacement and, therefore, are not strictly younger than the plains units as widely held. Because the DFC group comprises ~80% of the total crater population on Venus the recalculated emplacement age of the plains would be ~145 Ma if DFCs are indeed volcanically modified during plains formation. Improved image and topographic data are required to measure stratigraphic and morphometric relationships and resolve this issue. Plains units are also home to an abundant and diverse set of volcanic features including steep-sided domes, shield fields, isolated volcanoes, collapse features and lava channels, some of which extend for 1000s of kilometers. The inferred viscosity range of plains-forming lavas, therefore, is immense, ranging from the

  12. Venus Mobile Explorer with RPS for Active Cooling: A Feasibility Study

    Science.gov (United States)

    Leifer, Stephanie D.; Green, Jacklyn R.; Balint, Tibor S.; Manvi, Ram

    2009-01-01

    We present our findings from a study to evaluate the feasibility of a radioisotope power system (RPS) combined with active cooling to enable a long-duration Venus surface mission. On-board power with active cooling technology featured prominently in both the National Research Council's Decadal Survey and in the 2006 NASA Solar System Exploration Roadmap as mission-enabling for the exploration of Venus. Power and cooling system options were reviewed and the most promising concepts modeled to develop an assessment tool for Venus mission planners considering a variety of future potential missions to Venus, including a Venus Mobile Explorer (either a balloon or rover concept), a long-lived Venus static lander, or a Venus Geophysical Network. The concepts modeled were based on the integration of General Purpose Heat Source (GPHS) modules with different types of Stirling cycle heat engines for power and cooling. Unlike prior investigations which reported on single point design concepts, this assessment tool allows the user to generate either a point design or parametric curves of approximate power and cooling system mass, power level, and number of GPHS modules needed for a "black box" payload housed in a spherical pressure vessel.

  13. Technology perspectives in the future exploration of Venus

    Science.gov (United States)

    Cutts, James A.; Balint, Tibor S.; Chassefiere, Eric; Kolawa, Elizabeth A.

    Science goals to understand the origin, history and environment of Venus have been driving international space exploration missions for over 40 years. Today, Venus is still identified as a high priority science target in NASA's Solar System Exploration Roadmap, and clearly fits scientific objectives of ESA's Cosmic Vision Program in addition to the ongoing Venus Express mission, while JAXA is planning to launch its own Venus Climate Orbiter. Technology readiness has often been the pivotal factor in mission prioritization. Missions in all classes—small, medium or large—could be designed as orbiters with remote sensing capabilities, however, the desire for scientific advancements beyond our current knowledge point to in-situ exploration of Venus at the surface and lower atmosphere, involving probes, landers, and aerial platforms. High altitude balloons could circumnavigate Venus repeatedly; deep probes could operate for extended periods utilizing thermal protection technologies, pressure vessel designs and advancements in high temperature electronics. In situ missions lasting for over an Earth day could employ a specially designed dynamic Stirling Radioisotope Generator (SRG) power system, that could provide both electric power and active thermal control to the spacecraft. An air mobility platform, possibly employing metallic bellows, could allow for all axis control, long traversing and surface access at multiple desired locations, thus providing an advantage over static lander or rover based architectures. Sample return missions are also featured in all planetary roadmaps. The Venus exploration plans over the next three decades are anticipated to greatly contribute to our understanding of this planet, which subsequently would advance our overall knowledge about Solar System history and habitability.

  14. Short Large-Amplitude Magnetic Structures (SLAMS) at Venus

    Science.gov (United States)

    Collinson, G. A.; Wilson, L. B.; Sibeck, D. G.; Shane, N.; Zhang, T. L.; Moore, T. E.; Coates, A. J.; Barabash, S.

    2012-01-01

    We present the first observation of magnetic fluctuations consistent with Short Large-Amplitude Magnetic Structures (SLAMS) in the foreshock of the planet Venus. Three monolithic magnetic field spikes were observed by the Venus Express on the 11th of April 2009. The structures were approx.1.5->11s in duration, had magnetic compression ratios between approx.3->6, and exhibited elliptical polarization. These characteristics are consistent with the SLAMS observed at Earth, Jupiter, and Comet Giacobini-Zinner, and thus we hypothesize that it is possible SLAMS may be found at any celestial body with a foreshock.

  15. Laying bare Venus' dark secrets

    International Nuclear Information System (INIS)

    Allen, D.A.

    1987-01-01

    Ground-based IR observations of the dark side of Venus obtained in 1983 and 1985 with the Anglo-Australian Telescope are studied. An IR spectrum of Venus' dark side is analyzed. It is observed that the Venus atmosphere is composed of CO and radiation escapes only at 1.74 microns and 2.2 to 2.4 microns. The possible origin of the radiation, either due to absorbed sunlight or escaping thermal radiation, was investigated. These two hypotheses were eliminated, and it is proposed that the clouds of Venus are transparent and the radiation originates from the same stratum as the brighter portions but is weakened by the passage through the upper layer. The significance of the observed dark side markings is discussed

  16. Venus Suface Sampling and Analysis

    Data.gov (United States)

    National Aeronautics and Space Administration — This effort is developing the technology to transfer particulate samples from a Venus drill (being developed by Honeybee Robotics in a Phase 2 Small Business...

  17. Venus - Phoebe Region

    Science.gov (United States)

    1990-01-01

    This Magellan radar image is of part of the Phoebe region of Venus. It is a mosaic of parts of revolutions 146 and 147 acquired in the first radar test on Aug. 16, 1990. The area in the image is located at 291 degrees east longitude, 19 degrees south latitude. The image shows an area 30 kilometers (19.6 miles) wide and 76 km (47 miles) long. On the basis of Pioneer Venus and Arecibo data, it is known that two major rift zones occur in southern Phoebe Regio and that they terminate at about 20 to 25 degrees south latitude, about 2,000 km (1,240 miles) apart. This image is of an area just north of the southern end of the western rift zone. The region is characterized by a complex geologic history involving both volcanism and faulting. Several of the geologic units show distinctive overlapping or cross cutting relationships that permit identification and separation of geologic events and construction of the geologic history of the region. The oldest rocks in this image form the complexly deformed and faulted, radar bright, hilly terrain in the northern half. Faults of a variety of orientations are observed. A narrow fault trough (about one-half to one km (three tenths to six tenths of a mile) wide is seen crossing the bright hills near the lower part in the middle of the image. This is one of the youngest faults in the faulted, hilly unit as it is seen to cut across many other structures. The fault trough in turn appears to be embayed and flooded by the darker plains that appear in the south half of the image. These plains are interpreted to be of volcanic origin. The dark plains may be formed of a complex of overlapping volcanic flows. For example, the somewhat darker region of plains in the lower left (southwest) corner of the image may be a different age series of plains forming volcanic lava flows. Finally, the narrow bright line crossing the image in its lower part is interpreted to be a fault which cross cuts both plains units and is thus the youngest event in

  18. Mantle plumes on Venus revisited

    Science.gov (United States)

    Kiefer, Walter S.

    1992-01-01

    The Equatorial Highlands of Venus consist of a series of quasicircular regions of high topography, rising up to about 5 km above the mean planetary radius. These highlands are strongly correlated with positive geoid anomalies, with a peak amplitude of 120 m at Atla Regio. Shield volcanism is observed at Beta, Eistla, Bell, and Atla Regiones and in the Hathor Mons-Innini Mons-Ushas Mons region of the southern hemisphere. Volcanos have also been mapped in Phoebe Regio and flood volcanism is observed in Ovda and Thetis Regiones. Extensional tectonism is also observed in Ovda and Thetis Regiones. Extensional tectonism is also observed in many of these regions. It is now widely accepted that at least Beta, Atla, Eistla, and Bell Regiones are the surface expressions of hot, rising mantel plumes. Upwelling plumes are consistent with both the volcanism and the extensional tectonism observed in these regions. The geoid anomalies and topography of these four regions show considerable variation. Peak geoid anomalies exceed 90 m at Beta and Atla, but are only 40 m at Eistla and 24 m at Bell. Similarly, the peak topography is greater at Beta and Atla than at Eistla and Bell. Such a range of values is not surprising because terrestrial hotspot swells also have a side range of geoid anomalies and topographic uplifts. Kiefer and Hager used cylindrical axisymmetric, steady-state convection calculations to show that mantle plumes can quantitatively account for both the amplitude and the shape of the long-wavelength geoid and topography at Beta and Atla. In these models, most of the topography of these highlands is due to uplift by the vertical normal stress associated with the rising plume. Additional topography may also be present due to crustal thickening by volcanism and crustal thinning by rifting. Smrekar and Phillips have also considered the geoid and topography of plumes on Venus, but they restricted themselves to considering only the geoid-topography ratio and did not

  19. Rate of volcanism on Venus

    International Nuclear Information System (INIS)

    Fegley, B. Jr.; Prinn, R.G.

    1988-07-01

    The maintenance of the global H 2 SO 4 clouds on Venus requires volcanism to replenish the atmospheric SO 2 which is continually being removed from the atmosphere by reaction with calcium minerals on the surface of Venus. The first laboratory measurements of the rate of one such reaction, between SO 2 and calcite (CaCO 3 ) to form anhydrite (CaSO 4 ), are reported. If the rate of this reaction is representative of the SO 2 reaction rate at the Venus surface, then we estimate that all SO 2 in the Venus atmosphere (and thus the H 2 SO 4 clouds) will be removed in 1.9 million years unless the lost SO 2 is replenished by volcanism. The required rate of volcanism ranges from about 0.4 to about 11 cu km of magma erupted per year, depending on the assumed sulfur content of the erupted material. If this material has the same composition as the Venus surface at the Venera 13, 14 and Vega 2 landing sites, then the required rate of volcanism is about 1 cu km per year. This independent geochemically estimated rate can be used to determine if either (or neither) of the two discordant (2 cu km/year vs. 200 to 300 cu km/year) geophysically estimated rates is correct. The geochemically estimated rate also suggests that Venus is less volcanically active than the Earth

  20. IAEA Board of Governors recommends landmark budget increase. ElBaradei updates Board on IAEA work in Iraq and Iran; expresses concern about North Korea

    International Nuclear Information System (INIS)

    2003-01-01

    looting of nuclear material or radioactive sources. 'In view of recurrent media reports on the subject,' Dr. ElBaradei said, 'I trust that the Authority will monitor any impact on the safety and health of the surrounding population and will share its findings with the Agency' and added that 'the Agency stands ready to provide any assistance required.' Commenting on a future role for the IAEA in Iraq, Dr. ElBaradei said that 'although the Agency's mandate in Iraq under various Security Council resolutions still stands, the Council has stated in resolution 1483 that it will revisit that mandate and we are awaiting such a review.' Nonetheless, he emphasized that, 'irrespective of our mandate under Security Council resolutions, we have the continuing obligation under Iraq's NPT safeguards agreement with the Agency to ensure that, in accordance with that agreement, Iraq does not have any proscribed nuclear material or activities.' On his recent visit to Iran, Dr. ElBaradei reported that the purpose of the visit was to impress on the Iranian authorities the need to clarify outstanding safeguards issues and to urge them to sign an Additional Protocol to enable the Agency to conduct in-depth and comprehensive verification. 'I expressed the need for substantial progress without delay in light of the report being prepared for the Board in September,' he said. He noted that a technical meeting took place last week in Tehran with senior IAEA safeguards staff and Iranian counterparts. As well, an IAEA team will visit Tehran in the next few weeks to clarify certain aspects of the Additional Protocol. On North Korea, Dr. ElBaradei expressed his concern about the latest reports about its reprocessing of the fuel rods that were under safeguards in the DPRK. 'In my view, the situation in the DPRK is currently the most immediate and most serious threat to the nuclear non-proliferation regime,' he said, 'and I find it regrettable that little concrete progress on the issue appears to have

  1. Retrieval of Venus' cloud parameters from VIRTIS nightside spectra in the latitude band 25°-55°N

    Science.gov (United States)

    Magurno, Davide; Maestri, Tiziano; Grassi, Davide; Piccioni, Giuseppe; Sindoni, Giuseppe

    2017-09-01

    Two years of data from the M-channel of the Visible and InfraRed Thermal Imaging Spectrometer (VIRTIS), on board the European Space Agency mission Venus Express operating around the planet Venus, are analysed. Nocturnal data from a nadir viewpoint in the latitude band 25°N-55°N are selected for their configuration advantages and maximisation of the scene homogeneity. A reference model, and radiance spectrum, is defined based on average accepted values of the Venus main atmospheric and cloud parameters found in the literature. Extensive radiative transfer simulations are performed to provide a synthetic database of more than 10 000 VIRTIS radiances representing the natural variability of the system parameters (atmospheric temperature profile, cloud H2Osbnd H2SO4 solution concentration and vertical distribution, particle size distribution density and modal radius). A simulated-observed fitting algorithm of spectral radiances in window channels, based on a weighting procedure accounting for the latitudinal observed radiance variations, is used to derive the best atmosphere-cloud configuration for each observation. Results show that the reference Venus model does not adequately reproduce the observed VIRTIS spectra. In particular, the model accounting for a constant sulphuric acid concentration along the vertical extent of the clouds is never selected as a best fit. The 75%/96% and 84%/96% concentrations (the first values refer to the upper cloud layers and the second values to the lower ones) are the most commonly retrieved models representing more than 85% of the retrieved cases for any latitudinal band considered. It is shown that the assumption of stratified concentration of aqueous sulphuric acid allows to adequately fit the observed radiance, in particular the peak at 1.74 μm and around 4 μm. The analysis of the results concerning the microphysics suggests larger radii for the upper cloud layers in conjunction with a large reduction of their number density

  2. Identification of Postclassic Maya Constellations from the Venus Pages of the Dresden Codex

    Directory of Open Access Journals (Sweden)

    Changbom Park

    2010-01-01

    Full Text Available Ancient Mayan civilization, flourished from 1200 B.C. to 1500 A.D., has left numerous hieroglyphic texts on astronomical observations and calendar. In particular, the Dresden Codex contains the most details of such ancient Mayan heritage. Page 24 and those from 46 to 50 of the Dresden Codex describe the Mayan Venus calendar along with the augural descriptions. We note that the calendar in Dresden Codex is Venus-solar calendar. Our work focuses on the possibility that the calendar was made to work in conjunction with the periodic appearance of constellations on the sky. By analyzing the descriptions in the Venus pages, we propose that the columns in each page describe the motion of Venus with respect to major constellations at dates corresponding to special events while the calendar dates increase horizontally in the synodic period of Venus. We present twenty Mayan constellations identified from the Venus pages assuming that the first date of page 46 is February 6, 1228. We also report our understanding of verb expressions about the relative movement of constellations and Venus.La civilización maya, que floreció del 1200 a.C. a 1500 d.C., dejó numerosos textos jeroglíficos sobre el calendario y observaciones astronómicos. El Códice de Dresde, en particular, contiene el más detallado de dichos antiguos legados mayas. Las páginas 24 y 46 a 50 de dicho códice describen el calendario de Venus con los augurios correspondientes. Nosotros hemos notado que éste es un calendario Venus-Solar, y nuestro trabajo se enfoca sobre la posibilidad de que estuviera hecho para trabajar en conjunción con la aparición de determinadas constelaciones en el cielo. Es a través del análisis y descripción de las páginas de Venus que proponemos que las columnas en cada página describen el movimiento de Venus respecto de constelaciones mayores, en fechas que corresponden a eventos especiales, mientras que las fechas calendáricas se incrementan

  3. LIBS Testing in a Venus Environment Project

    Data.gov (United States)

    National Aeronautics and Space Administration — Configure LIBS system to view samples in the Venus chamber Confirm STP results for LIBS in Venus Chamber configuration Conduct high temperature/high pressure...

  4. Venus Atmospheric Maneuverable Platform (VAMP)

    Science.gov (United States)

    Griffin, K.; Sokol, D.; Lee, G.; Dailey, D.; Polidan, R.

    2013-12-01

    We have explored a possible new approach to Venus upper atmosphere exploration by applying recent Northrop Grumman (non-NASA) development programs to the challenges associated with Venus upper atmosphere science missions. Our concept is a low ballistic coefficient (gas, wing span, vehicle mass, power supply, propulsion, materials considerations, structural elements, subsystems, and packaging. The interaction between the VAMP vehicle and the supporting orbiter will also be discussed. In this context, we will specifically focus upon four key factors impacting the design and performance of VAMP: 1. Feasibility of and options for the deployment of the vehicle in space 2. Entry into the Venus atmosphere, including descent profile, heat rate, total heat load, stagnation temperature, control, and entry into level flight 3. Characteristics of flight operations and performance in the Venus atmosphere: altitude range, latitude and longitude access, day/night performance, aircraft performance (aerodynamics, power required vs. power available, propulsion, speed, percent buoyancy), performance sensitivity to payload weight 4. Science payload accommodation, constraints, and opportunities We will discuss interdependencies of the above factors and the manner in which the VAMP strawman's characteristics affect the CONOPs and the science objectives. We will show how the these factors provide constraints as well as enable opportunities for novel long duration scientific studies of the Venus upper atmosphere that support VEXAG goals 2 and 3. We will also discuss how the VAMP platform itself can facilitate some of these science measurements.

  5. Venus volcanism and El Chichon

    Science.gov (United States)

    Bell, Peter M.

    Reinterpretations of telemetry data returned to earth from the Pioneer Venus Orbiter suggest that the surface of Venus may be characterized by violent immense volcanic activity. L.W. Esposito has made an interactive analysis of Pioneer ultraviolet spectral data and similar data from the earth's atmosphere [Science, 223, 1072-1074, 1984]. Spacecraft analysis of sulfur dioxide in the earth's upper atmosphere, apparently released by El Chich[acu]on, Mexico, in March 1982 (EOS, June 14, 1983, p. 411, and August 16, 1983, p. 506) prompted reanalysis of accumulated Pioneer ultraviolet data. Massive injections of sulfur dioxide into the Venus atmosphere could be the result of volcanic eruptions about the size of the Krakatoa explosive eruption that took place between Java and Summatra in 1883.

  6. Venus project : experimentation at ENEA's pilot site

    International Nuclear Information System (INIS)

    Bargellini, M.L.; Fontana, F.; Niccolai, L.; Scavino, G.; Mancini, R.; Levialdi, S.

    1996-12-01

    The document describes the ENEA's (Italian Agency for New Technologies, Energy and the Environment) experience in the Venus Project (Esprit III 6398). Venus is an advanced visual interface based on icon representation that permits to end-user to inquiry databases. VENUS interfaces to ENEA's databases: cometa materials Module, Cometa Laboratories Module and European Programs. This report contents the results of the experimentation and of the validation carried out in ENEA's related to the Venus generations. Moreover, the description of the architecture, the user requirements syntesis and the validation methodology of the VENUS systems have been included

  7. Modeling Venus-Like Worlds Through Time

    OpenAIRE

    Way, M. J.; Del Genio, Anthony; Amundsen, David S.

    2018-01-01

    We explore the atmospheric and surface history of a hypothetical paleo-Venus climate using a 3-D General Circulation Model. We constrain our model with the in-situ and remote sensing Venus data available today. Given that Venus and Earth are believed to be similar geochemically some aspects of Earth's history are also utilized. We demonstrate that it is possible for ancient Venus and Venus-like exoplanetary worlds to exist within the liquid water habitable zone with insolations up to nearly 2...

  8. Venus Global Reference Atmospheric Model

    Science.gov (United States)

    Justh, Hilary L.

    2017-01-01

    Venus Global Reference Atmospheric Model (Venus-GRAM) is an engineering-level atmospheric model developed by MSFC that is widely used for diverse mission applications including: Systems design; Performance analysis; Operations planning for aerobraking, Entry, Descent and Landing, and aerocapture; Is not a forecast model; Outputs include density, temperature, pressure, wind components, and chemical composition; Provides dispersions of thermodynamic parameters, winds, and density; Optional trajectory and auxiliary profile input files Has been used in multiple studies and proposals including NASA Engineering and Safety Center (NESC) Autonomous Aerobraking and various Discovery proposals; Released in 2005; Available at: https://software.nasa.gov/software/MFS-32314-1.

  9. Males are from Mars, and females are from Venus: sex-specific fetal brain gene expression signatures in a mouse model of maternal diet-induced obesity.

    Science.gov (United States)

    Edlow, Andrea G; Guedj, Faycal; Pennings, Jeroen L A; Sverdlov, Deanna; Neri, Caterina; Bianchi, Diana W

    2016-05-01

    Maternal obesity is associated with adverse neurodevelopmental outcomes in children, including autism spectrum disorders, developmental delay, and attention-deficit hyperactivity disorder. The underlying mechanisms remain unclear. We previously identified second-trimester amniotic fluid and term cord blood gene expression patterns suggesting dysregulated brain development in fetuses of obese compared with lean women. We sought to investigate the biological significance of these findings in a mouse model of maternal diet-induced obesity. We evaluated sex-specific differences in fetal growth, brain gene expression signatures, and associated pathways. Female C57BL/6J mice were fed a 60% high-fat diet or 10% fat control diet for 12-14 weeks prior to mating. During pregnancy, obese dams continued on the high-fat diet or transitioned to the control diet. Lean dams stayed on the control diet. On embryonic day 17.5, embryos were weighed and fetal brains were snap frozen. RNA was extracted from male and female forebrains (10 per diet group per sex) and hybridized to whole-genome expression arrays. Significantly differentially expressed genes were identified using a Welch's t test with the Benjamini-Hochberg correction. Functional analyses were performed using ingenuity pathways analysis and gene set enrichment analysis. Embryos of dams on the high-fat diet were significantly smaller than controls, with males more severely affected than females (P = .01). Maternal obesity and maternal obesity with dietary change in pregnancy resulted in significantly more dysregulated genes in male vs female fetal brains (386 vs 66, P Maternal obesity with and without dietary change in pregnancy was associated with unique brain gene expression signatures for each sex, with an overlap of only 1 gene. Changing obese dams to a control diet in pregnancy resulted in more differentially expressed genes in the fetal brain than maternal obesity alone. Functional analyses identified common

  10. Males are from Mars, females are from Venus: sex-specific fetal brain gene expression signatures in a mouse model of maternal diet-induced obesity

    Science.gov (United States)

    EDLOW, Andrea G.; GUEDJ, Faycal; PENNINGS, Jeroen L.A.; SVERDLOV, Deanna; NERI, Caterina; BIANCHI, Diana W.

    2016-01-01

    BACKGROUND Maternal obesity is associated with adverse neurodevelopmental outcomes in children, including autism spectrum disorders, developmental delay, and attention deficit hyperactivity disorder. The underlying mechanisms remain unclear. We previously identified second trimester amniotic fluid and term cord blood gene expression patterns suggesting dysregulated brain development in fetuses of obese compared to lean women. OBJECTIVES We sought to investigate the biological significance of these findings in a mouse model of maternal diet-induced obesity. We evaluated sex-specific differences in fetal growth, brain gene expression signatures and associated pathways. STUDY DESIGN Female C57BL/6J mice were fed a 60% high-fat diet or 10% fat control diet for 12–14 weeks prior to mating. During pregnancy, obese dams continued on the high-fat diet (HFD/HFD), or transitioned to the CD (HFD/CD). Lean dams stayed on the control diet. On embryonic day 17.5, embryos were weighed and fetal brains were snap frozen. RNA was extracted from male and female forebrains (10/diet group/sex) and hybridized to whole genome expression arrays. Significantly differentially expressed genes were identified using Welch’s t-test with the Benjamini-Hochberg correction. Functional analyses were performed using Ingenuity Pathways Analysis and Gene Set Enrichment Analysis. RESULTS Embryos of HFD/HFD dams were significantly smaller than controls, with males more severely affected than females (p=0.01). Maternal obesity and maternal obesity with dietary change in pregnancy resulted in significantly more dysregulated genes in male versus female fetal brains (386 vs 66, pMaternal obesity with and without dietary change in pregnancy was associated with unique brain gene expression signatures for each sex, with overlap of only one gene. Changing obese dams to a control diet in pregnancy resulted in more differentially expressed genes in the fetal brain than maternal obesity alone. Functional

  11. Introduction to the special issue on Venus exploration

    Science.gov (United States)

    Svedhem, H.; Wilson, C.; Piccioni, G.

    2015-08-01

    Venus Express ended its mission in December 2014 after an extraordinary successful eight and a half years at Venus. The first years of the mission concentrated on the original objectives of the mission, namely to study the dynamics, structure and chemistry of the atmosphere, to investigate the plasma environment and its interaction with the solar wind, and to study certain topics of the surface and the surface atmosphere interaction. The latter part of the mission was focussing on dedicated campaigns for the study of specific topics, often in coordination with ground based observations. The highly elliptical polar orbit permitted a study of all latitudes, particularly of the polar regions. The optimised payload and orbit of the mission, together with the systematic and long-term observations of the atmosphere has enabled a wealth of data to be analysed. It has already resulted in many exciting new findings and a significantly improved understanding of Venus, even if only a part of the data has been analysed so far. In the last year of the mission a two month long aerobraking campaign was performed, resulting in a valuable data set on the structure of the atmosphere down to below 130 km - a region difficult to sample with remote techniques, before the fuel ran out at the end of November 2014. This campaign also provided a lot of engineering and operational experience, useful for future missions that may use aerobraking techniques at Venus or other planets.

  12. Venus and Mercury as Planets

    Science.gov (United States)

    1974-01-01

    A general evolutionary history of the solar planetary system is given. The previously observed characteristics of Venus and Mercury (i.e. length of day, solar orbit, temperature) are discussed. The role of the Mariner 10 space probe in gathering scientific information on the two planets is briefly described.

  13. Venus and Mercury as planets

    International Nuclear Information System (INIS)

    1974-01-01

    A general evolutionary history of the solar planetary system is given. The previously observed characteristics of Venus and Mercury (i.e. length of day, solar orbit, temperature) are discussed. The role of the Mariner 10 space probe in gathering scientific information on the two planets is briefly described

  14. Transits of Venus in Public Education and Contemporary Research

    Science.gov (United States)

    Pasachoff, J. M.

    2011-10-01

    Transits of Venus are among the rarest predictable astronomical event that humans can enjoy, and the 2012 transit will be visible by almost all the people on Earth. It is our job as educators to bring out the thrill of being able to see the tiny dot of Venus silhouetted against the solar disk even with just a simple eye-protection filter. My Website at http://www.transitofvenus.info brings together not only historical information about the five previous transits of Venus that were observed through the 20th century--1639, 1761, 1769, 1874, and 1882--but also the scientific work carried out at the 2004 transit and at recent transits of Mercury. Based on space observations of the 1999 transit of Mercury with NASA's Transition Region and Coronal Explorer (TRACE), Glenn Schneider and I provided proof of the contemporary explanation of the black-drop effect as an amalgam of instrumental point-spread and solar limb-darkening [1]. Based on observations of the changes in the total solar irradiance during the transit, we provided an analysis of this solar-system analogue to exoplanet transits [2]. High-resolution (0.5 arcsec pixels) observations of ingress and egress with TRACE during the 2004 transit provided information about the visibility of Venus's atmosphere through its refraction of sunlight, interpreted with Venus Express observations [3]. We anticipate observing the 2012 transit with groundbased facilities of the University of Hawaii at Haleakala, and of the National Solar Observatory at Sacramento Peak, and Kitt Peak, as well as with NASA and JAXA spacecraft, including Solar Dynamics Observatory, ACRIMsat, and Hinode. The Program Group on Public Education on the Occasions of Eclipses and Transits of Commission 46 on Education and Development of the International Astronomical Union, which I chair, looks forward to participating in Education and Public Outreach efforts related to the 2012 transit.

  15. Mars is close to venus--female reproductive proteins are expressed in the fat body and reproductive tract of honey bee (Apis mellifera L.) drones.

    Science.gov (United States)

    Colonello-Frattini, Nínive Aguiar; Guidugli-Lazzarini, Karina Rosa; Simões, Zilá Luz Paulino; Hartfelder, Klaus

    2010-11-01

    Vitellogenin (Vg) and lipophorin (Lp) are lipoproteins which play important roles in female reproductive physiology of insects. Both are actively taken up by growing oocytes and especially Vg and its receptor are considered as female-specifically expressed. The finding that the fat body of in honey bee (Apis mellifera) drones synthesizes Vg and is present in hemolymph has long been viewed as a curiosity. The recent paradigm change concerning the role played by Vg in honey bee life history, especially social division of labor, has now led us to investigate whether a physiological constellation similar to that seen in female reproduction may also be represented in the male sex. By means of Western blot analysis we could show that both Vg and Lp are present in the reproductive tract of adult drones, including the accessory (mucus) glands, but apparently are not secreted. Furthermore, we analyzed the transcript levels of the genes encoding these proteins (vg and lp), as well as their putative receptors (Amvgr and Amlpr) in fat body and accessory glands. Whereas lp, vg and Amlpr transcript levels decreased with age in both tissues, Amvgr mRNA levels increased with age in fat body. To our knowledge this is the first report that vitellogenin and its receptor are co-expressed in the reproductive system of a male insect. We interpret these findings as a cross-sexual transfer of a social physiological trait, associated with the rewiring of the juvenile hormone/vitellogenin circuitry that occurred in the female sex of honey bees. Copyright 2010 Elsevier Ltd. All rights reserved.

  16. Venus transits - A French view

    Science.gov (United States)

    Débarbat, Suzanne

    2005-04-01

    After a careful study of Mars observations obtained by Tycho Brahé (1546-1601), Kepler (1571-1630) discovered the now-called Kepler's third law. In 1627 he published his famous Tabulae Rudolphinae, a homage to his protector Rudolph II (1552-1612), tables (Kepler 1609, 1627) from which he predicted Mercury and Venus transits over the Sun. In 1629 Kepler published his Admonitio ad Astronomos Advertisement to Astronomers (Kepler 1630), Avertissement aux Astronomes in French Au sujet de phénomènes rares et étonnants de l'an 1631: l'incursion de Vénus et de Mercure sur le Soleil. This was the beginning of the interest of French astronomers, among many others, in such transits, mostly for Venus, the subject of this paper in which dates are given in the Gregorian calendar.

  17. How the Venus flytrap snaps

    Science.gov (United States)

    Forterre, Yoël; Skotheim, Jan M.; Dumais, Jacques; Mahadevan, L.

    2005-01-01

    The rapid closure of the Venus flytrap (Dionaea muscipula) leaf in about 100ms is one of the fastest movements in the plant kingdom. This led Darwin to describe the plant as ``one of the most wonderful in the world''. The trap closure is initiated by the mechanical stimulation of trigger hairs. Previous studies have focused on the biochemical response of the trigger hairs to stimuli and quantified the propagation of action potentials in the leaves. Here we complement these studies by considering the post-stimulation mechanical aspects of Venus flytrap closure. Using high-speed video imaging, non-invasive microscopy techniques and a simple theoretical model, we show that the fast closure of the trap results from a snap-buckling instability, the onset of which is controlled actively by the plant. Our study identifies an ingenious solution to scaling up movements in non-muscular engines and provides a general framework for understanding nastic motion in plants.

  18. The SPICAV-SOIR instrument probing the atmosphere of Venus: an overview

    Science.gov (United States)

    Trompet, Loïc; Mahieux, Arnaud; Wilquet, Valérie; Robert, Séverine; Chamberlain, Sarah; Thomas, Ian; Carine Vandaele, Ann; Bertaux, Jean-Loup

    2016-04-01

    The Solar Occultation in the Infrared (SOIR) channel mounted on top of the SPICAV instrument of the ESA's Venus Express mission has observed the atmosphere of Venus during more than eight years. This IR spectrometer (2.2-4.3 μm) with a high spectral resolution (0.12 cm-1) combined an echelle grating with an acousto-optic tunable filter for order selection. SOIR performed more than 1500 solar occultation measurements leading to about two millions spectra. The Royal Belgian Institute for Space Aeronomy (BIRA-IASB) was in charge of SOIR's development and operations as well as its data pipeline. BIRA-IASB carried out several studies on the composition of Venus mesosphere and lower thermosphere: carbon dioxide, carbon monoxide, hydrogen halide (HF, HCl, DF, DCl), sulfur dioxide, water (H2O, HDO) as well as sulphuric acid aerosols in the upper haze of Venus. Density and temperature profiles of the upper atmosphere of Venus (60 km to 170 km) at the terminator have been retrieved from SOIR's spectra using different assumptions, wherein the hydrostatic equilibrium and the local thermodynamical equilibrium in the radiative transfer calculations. These results allow us to produce an Atmospheric model of Venus called Venus Atmosphere from SOIR measurements at the Terminator (VAST). Data obtained by SOIR will also contribute to update the Venus International Reference Atmosphere (VIRA). Recently, the treatment of the raw data to transmittance has been optimized, and a new dataset of spectra has been produced. All raw spectra (PSA level 2) as well as calibrated spectra (PSA level 3) have been delivered to ESA's Planetary Science Archive (PDSPSA). Consequently the re-analysis of all spectra has been undergone. We will briefly present the improvements implemented in the data pipeline. We will also show a compilation of results obtained by the instrument considering the complete mission duration.

  19. An unusual volcano on Venus

    Science.gov (United States)

    Moore, H. J.; Plaut, J. J.; Schenk, P. M.; Head, J. W.

    1992-01-01

    Materials that issued from an unusual Venusian volcano produced (1) a complex domical structure about 100 km across with thick, broad flow lobes up to 41 wide, (2) an extensive sheet of thick flows, and (3) radar-bright surfaces that extend to 360-400 km from the volcano. Altimetry indicates that the relief of the domical structure is about 0.5-1.1 km. The lobes and flows have prominant regularly spaced ridges about 686-820 m apart. Thick flows with large ridge separations and broad lobes are rare on Venus. The viscosities of these flows were larger than those of most lava flows on Venus. Comparisons of the dimensions of the volcano's lobes with lava flows on earth suggest that the Venusian lavas may have large silica contents. Radar-bright surfaces around the volcano may represent the result of an explosive eruption or very thin deposits of low-viscosity lavas. Thus, the radar-bright surfaces and lavas of the volcano were derived from a magma that differentiated within the crust or mantle of Venus. The differentiation produced (1) a gas-rich low-viscosity phase, (2) high-viscosity lavas, and (3) a residual primary magma.

  20. Structure of High Energy, Heavy Ions in Venus' Upper Ionosphere

    Science.gov (United States)

    Persson, Moa; Futaana, Yoshifumi; Nilsson, Hans; Stenberg Wieser, Gabriella; Hamrin, Maria; Fedorov, Andrei; Barabash, Stas

    2017-04-01

    The solar wind interacts with the atmosphere of Venus, and can reach directly down to the ionosphere. The interaction has previously been studied using the Pioneer Venus mission (PVO) and is now known to cause variations in the density in the ionosphere [Taylor et al., 1980], a transport of ions towards the night side [Knudsen et al., 1980], and an outflow of ions from the atmosphere [Barabash et al., 2007]. Measurements made by PVO showed that the main constituents of Venus ionosphere in the altitude range 150-400 km is the O+ and O2+ ions, where the former dominates from 180 km and higher, and the latter dominates from 180 km down to 150 km [Taylor et al., 1980]. New measurements, made by the Ion Mass Analyzer (IMA) onboard the Venus Express spacecraft, reveal the high-energy (10 eV to 15 keV) plasma characteristics in the ionosphere of Venus. Using the data collected during the low altitude (down to 130 km) pericentre passages during the aerobraking time period, we are able to extract the height profile of the total heavy ion content (O+ and O2+ ions) of Venus ionosphere. The results show two scale heights separated at 200 km; 10 km for 200 km. We interpret the results as two heavy ion components, namely, the O+ ions are dominant for >200 km, while the O2+ is dominant for methods of mass separation, to extract the two ion components of the scale height profiles, (O+ and O2+). First method is to use the moderate mass separation capabilities of the IMA instrument. The individual mass spectra are fitted by two Gaussian curves, representing O+ and O2+, derived from ground calibration information. The second method uses the energy spectrum, which sometimes has two discrete peaks. By assuming the same velocity for different components in the spacecraft reference frame (resulting in different energy for different masses), we can separate the composition. We will discuss the results of the obtained mass separated height profiles.

  1. The need for New In Situ Measurements to Understand the Climate, Geology and Evolution of Venus.

    Science.gov (United States)

    Grinspoon, D. H.

    2017-12-01

    Many measurements needed to address outstanding questions about current processes and evolution of Venus can only be made from in situ platforms such as entry probes, balloons or landers. Among these are precise determination of the value and altitude dependence of the deuterium-to-hydrogen ratio, an important tracer of water history which, while clearly greatly elevated compared to the terrestrial ratio, is still unknown within a large range of uncertainty and appears, based on Venus Express results, to display an enigmatic altitude dependence. Rare gas abundances and isotopes provide clues to volatile sources and histories of outgassing and exospheric escape. Modern mass spectrometry at Venus would yield abundances of the eight stable xenon isotopes, bulk abundances of krypton, and isotopes of neon. Altitude profiles of sulfur-containing chemical species would illuminate global geochemical cycles, including cloud formation, outgassing rates and surface-atmosphere interactions. The altitude profile of wind speeds and radiation fluxes, interpreted in light of the Venus Express and Akatsuki data, would enrich understanding of the global circulation and climate dynamics of Venus. Descent and surface images of carefully chosen locations would lend ground truth to interpretations of the near-global Magellan data sets and provide context for global remote sensing data obtained by future orbiter missions. Landed instruments would provide refinement and calibration for chemical abundance measurements by historical missions as well as direct mineralogical measurements of Venusian surface and subsurface rocks. In concert with atmospheric measurements these would greatly constrain geologic history as well as the nature of surface-atmosphere interactions. Such a suite of measurements will deepen our understanding of the origin and evolution of Venus in the context of Solar System and extrasolar terrestrial planets, determine the level and style of current geological activity

  2. Gravity field of Venus - A preliminary analysis

    Science.gov (United States)

    Phillips, R. J.; Sjogren, W. L.; Abbott, E. A.; Smith, J. C.; Wimberly, R. N.; Wagner, C. A.

    1979-01-01

    The gravitational field of Venus obtained by tracking the Pioneer Venus Orbiter is examined. For each spacecraft orbit, two hours of Doppler data centered around periapsis were used to estimate spacecraft position and velocity and the velocity residuals obtained were spline fit and differentiated to produce line of sight gravitational accelerations. Consistent variations in line of sight accelerations from orbit to orbit reveal the presence of gravitational anomalies. A simulation of isostatic compensation for an elevated region on the surface of Venus indicates that the mean depth of compensation is no greater than about 100 km. Gravitational spectra obtained from a Fourier analysis of line of sight accelerations from selected Venus orbits are compared to the earth's gravitational spectrum and spherical harmonic gravitational potential power spectra of the earth, the moon and Mars. The Venus power spectrum is found to be remarkably similar to that of the earth, however systematic variations in the harmonics suggest differences in dynamic processes or lithospheric behavior.

  3. Composition and Chemistry of the Neutral Atmosphere of Venus

    Science.gov (United States)

    Marcq, Emmanuel; Mills, Franklin P.; Parkinson, Christopher D.; Vandaele, Ann Carine

    2018-02-01

    This paper deals with the composition and chemical processes occurring in the neutral atmosphere of Venus. Since the last synthesis, observers as well as modellers have emphasised the spatial and temporal variability of minor species, going beyond a static and uniform picture that may have prevailed in the past. The outline of this paper acknowledges this situation and follows closely the different dimensions along which variability in composition can be observed: vertical, latitudinal, longitudinal, temporal. The strong differences between the atmosphere below and above the cloud layers also dictate the structure of this paper. Observational constraints, obtained from both Earth and Venus Express, as well as 1D, 2D and 3D models results obtained since 1997 are also extensively referred and commented by the authors. An non-exhaustive list of topics included follows: modelled and observed latitudinal and vertical profiles of CO and OCS below the clouds of Venus; vertical profiles of CO and SO2 above the clouds as observed by solar occultation and modelled; temporal and spatial variability of sulphur oxides above the clouds. As a conclusion, open questions and topics of interest for further studies are discussed.

  4. Involvement of glutamatergic N-methyl-d-aspartate receptors in the expression of increased head-dipping behaviors in the hole-board tests of olfactory bulbectomized mice.

    Science.gov (United States)

    Hirose, Noritaka; Saitoh, Akiyoshi; Kamei, Junzo

    2016-10-01

    Olfactory bulbectomized (OB) mice produce agitated anxiety-like behaviors in the hole-board test, which was expressed by an increase in head-dipping counts and a decrease in head-dipping latencies. However, the associated mechanisms remain unclear. In the present study, MK-801 (10, 100μg/kg), a selective N-methyl-d-aspartate (NMDA) receptor antagonist, significantly and dose-dependently suppressed the increased head-dipping behaviors in OB mice, without affecting sham mice. Similar results were obtained with another selective NMDA receptor antagonist D-AP5 treatment in OB mice. On the other hand, muscimol, a selective aminobutyric acid type A (GABAA) receptor agonist produced no effects on these hyperemotional behaviors in OB mice at a dose (100μg/kg) that produced anxiolytic-like effects in sham mice. Interestingly, glutamine contents and glutamine/glutamate ratios were significantly increased in the amygdala and frontal cortex of OB mice compared to sham mice. Based on these results, we concluded that the glutamatergic NMDA receptors are involved in the expression of increased head-dipping behaviors in the hole-board tests of OB mice. Accordingly, the changes in glutamatergic transmission in frontal cortex and amygdala may play important roles in the expression of these abnormal behaviors in OB mice. Copyright © 2016. Published by Elsevier B.V.

  5. Board Charter

    International Development Research Centre (IDRC) Digital Library (Canada)

    TEST

    Senior Centre Staff participate in meetings and make presentations to allow. Governors to gain ... assist individual governors, part of the Board evaluation includes self-assessment. The Board. Evaluation ... oversee the Board's evaluation and self-assessment exercises and implementing change and improvements, as ...

  6. A statistical study of ionopause perturbation and associated boundary wave formation at Venus.

    Science.gov (United States)

    Chong, G. S.; Pope, S. A.; Walker, S. N.; Zhang, T.; Balikhin, M. A.

    2017-12-01

    In contrast to Earth, Venus does not possess an intrinsic magnetic field. Hence the interaction between solar wind and Venus is significantly different when compared to Earth, even though these two planets were once considered similar. Within the induced magnetosphere and ionosphere of Venus, previous studies have shown the existence of ionospheric boundary waves. These structures may play an important role in the atmospheric evolution of Venus. By using Venus Express data, the crossings of the ionopause boundary are determined based on the observations of photoelectrons during 2011. Pulses of dropouts in the electron energy spectrometer were observed in 92 events, which suggests potential perturbations of the boundary. Minimum variance analysis of the 1Hz magnetic field data for the perturbations is conducted and used to confirm the occurrence of the boundary waves. Statistical analysis shows that they were propagating mainly in the ±VSO-Y direction in the polar north terminator region. The generation mechanisms of boundary waves and their evolution into the potential nonlinear regime are discussed and analysed.

  7. Towards Understanding the Climate of Venus Applications of Terrestrial Models to Our Sister Planet

    CERN Document Server

    Bonnet, Roger-Maurice; Grinspoon, David; Koumoutsaris, Symeon; Lebonnois, Sebastien; Titov, Dmitri

    2013-01-01

    ESA’s Venus Express Mission has monitored Venus since April 2006, and scientists worldwide have used mathematical models to investigate its atmosphere and model its circulation. This book summarizes recent work to explore and understand the climate of the planet through a research program under the auspices of the International Space Science Institute (ISSI) in Bern, Switzerland. Some of the unique elements that are discussed are the anomalies with Venus’ surface temperature (the huge greenhouse effect causes the surface to rise to 460°C, without which would plummet as low as -40°C), its unusual lack of solar radiation (despite being closer to the Sun, Venus receives less solar radiation than Earth due to its dense cloud cover reflecting 76% back) and the juxtaposition of its atmosphere and planetary rotation (wind speeds can climb up to 200 m/s, much faster than Venus’ sidereal day of 243 Earth-days).

  8. VizieR Online Data Catalog: Horizontal temperature at Venus upper atmosphere (Peralta+, 2016)

    Science.gov (United States)

    Peralta, J.; Lopez-Valverde, M. A.; Gilli, G.; Piccialli, A.

    2015-11-01

    The dayside atmospheric temperatures in the UMLT of Venus (displayed in Figure 7A of this article) are listed as a CSV data file. These values consist of averages in bins of 5° in latitude and 0.25-hours in local time from dayside temperatures covering five years of data (from 2006/05/14 to 2011/06/05). These temperatures were inferred from the CO2 NLTE nadir spectra measured by the instrument VIRTIS-H onboard Venus Express (see article for full description of the procedure), and are representative of the atmospheric region between 10-2 to 10-5mb. Along with the temperatures, we also provide the corresponding error and the number of temperatures averaged in each bin. The format of the CSV file reasonably agrees with the expected format of the data files to be provided in the future version of the Venus International Reference Atmosphere (VIRA). (1 data file).

  9. Global Geological Map of Venus

    Science.gov (United States)

    Ivanov, M. A.

    2008-09-01

    Introduction: The Magellan SAR images provide sufficient data to compile a geological map of nearly the entire surface of Venus. Such a global and selfconsistent map serves as the base to address the key questions of the geologic history of Venus. 1) What is the spectrum of units and structures that makes up the surface of Venus [1-3]? 2) What volcanic/tectonic processes do they characterize [4-7]? 3) Did these processes operated locally, regionally, or globally [8- 11]? 4) What are the relationships of relative time among the units [8]? 5) At which length-scale these relationships appear to be consistent [8-10]? 6) What is the absolute timing of formation of the units [12-14]? 7) What are the histories of volcanism, tectonics and the long-wavelength topography on Venus? 7) What model(s) of heat loss and lithospheric evolution [15-21] do these histories correspond to? The ongoing USGS program of Venus mapping has already resulted in a series of published maps at the scale 1:5M [e.g. 22-30]. These maps have a patch-like distribution, however, and are compiled by authors with different mapping philosophy. This situation not always results in perfect agreement between the neighboring areas and, thus, does not permit testing geological hypotheses that could be addressed with a self-consistent map. Here the results of global geological mapping of Venus at the scale 1:10M is presented. The map represents a contiguous area extending from 82.5oN to 82.5oS and comprises ~99% of the planet. Mapping procedure: The map was compiled on C2- MIDR sheets, the resolution of which permits identifying the basic characteristics of previously defined units. The higher resolution images were used during the mapping to clarify geologic relationships. When the map was completed, its quality was checked using published USGS maps [e.g., 22-30] and the catalogue of impact craters [31]. The results suggest that the mapping on the C2-base provided a highquality map product. Units and

  10. 225 years of the Venus atmosphere investigations

    International Nuclear Information System (INIS)

    Barsukov, V.L.; Volkov, V.P.

    1986-01-01

    Historical review of investigation into the Venus atmosphere is given. It begins from the discovery of planetary atmosphere made by a great Russian scientist Lomonosov in 1761 till the latest atmosphere investigations by means of the Vega-1 and Vega-2 descent vehicles in 1985 within the framework of the international project for studying. The Venus planet and Halley comet. Results of investigation into physical properties and chemical composition of the planetary atmosphere and surface are present in short

  11. Space weather at planet Venus during the forthcoming BepiColombo flybys

    Science.gov (United States)

    McKenna-Lawlor, S.; Jackson, B.; Odstrcil, D.

    2018-03-01

    The BepiColombo (BC) Mission which will be launched in 2018, will include during its Cruise Phase two flybys of Venus and five Mercury flybys. It will then enter a one Earth year orbit about Mercury (with a possible one-year extension) during which two spacecraft, one provided by ESA (MPO) and one provided by JAXA (MMO), will perform both autonomous and coordinated observations of the Hermean environment at various separations. The measurements will take place during the minimum of solar cycle 24 and the rise of solar cycle 25. At the start of the minimum of solar cycle 23, four major flares, each associated with the production of MeV particle radiation and CME activity occurred. Predictions of the HAFv.2 model of the arrival of particle radiation and a travelling shock at Venus on 6 December 2006 were verified by in-situ measurements made aboard Venus Express (VEX) by the ASPERA 4 instrument. Interplanetary scintillation observations, as well as the ENLIL 3-D MHD model when employed separately or in combination, enable the making of predictions of the solar wind density and speed at various locations in the inner heliosphere. Both methods, which outdate HAFv.2, are utilized in the present paper to predict (retrospectively) the arrival of the flare related, interplanetary propagating shock recorded at Venus on 6 December 2006 aboard VEX with a view to putting in place the facility to make very reliable space weather predictions for BC during both its Cruise Phase and when in the Hermean environment itself. The successful matching of the December 2006 predictions with in-situ signatures recorded aboard Venus Express provide confidence that the predictive methodology to be adopted will be appropriate to provide space weather predictions for BepiColombo during its Venus flybys and throughout the mission.

  12. Geology of Maxwell Montes, Venus

    Science.gov (United States)

    Head, J. W.; Campbell, D. B.; Peterfreund, A. R.; Zisk, S. A.

    1984-01-01

    Maxwell Montes represent the most distinctive topography on the surface of Venus, rising some 11 km above mean planetary radius. The multiple data sets of the Pioneer missing and Earth based radar observations to characterize Maxwell Montes are analyzed. Maxwell Montes is a porkchop shaped feature located at the eastern end of Lakshmi Planum. The main massif trends about North 20 deg West for approximately 1000 km and the narrow handle extends several hundred km West South-West WSW from the north end of the main massif, descending down toward Lakshmi Planum. The main massif is rectilinear and approximately 500 km wide. The southern and northern edges of Maxwell Montes coincide with major topographic boundaries defining the edge of Ishtar Terra.

  13. Board game

    International Nuclear Information System (INIS)

    Brennan, N.S.

    1982-01-01

    A board game comprises a board, a number of counters and two dice. The board is marked to provide a central area, representing the nucleus of an atom, and six or more annular rings extending concentrically around the central area, the rings being divided into 2,8,18,32,48 and 72 squares. Each ring represents an electron shell, and some of the squares are numbered, the number representing the atomic number of different elements. (author)

  14. High Temperature Venus Drill and Sample Delivery System Project

    Data.gov (United States)

    National Aeronautics and Space Administration — We proposed to design, build and test a high temperature Pneumatic Drill and Trencher system for Venus subsurface exploration. The Venus Drill and Trencher will be...

  15. GALILEO ORBITER V POS VENUS TRAJECTORY V1.0

    Data.gov (United States)

    National Aeronautics and Space Administration — Galileo Orbiter 60 second sampled trajectory data from the Venus flyby in Venus Solar Orbital (VSO) coordinates. These data cover the interval 1990-02-09 00:00 to...

  16. SAEVe: A Long Duration Small Sat Class Venus Lander

    Science.gov (United States)

    Kremic, T.; Ghail, R.; Gilmore, M.; Kiefer, W.; Limaye, S.; Hunter, G.; Tolbert, C.; Pauken, M.; Wilson, C.

    2017-11-01

    SAEVe is a small Venus lander concept selected for further study by the PSDS3 call. SAEVe is an innovative approach to achieving Venus surface science by exploiting recent developments in high temperature electronics and unique operations scheme.

  17. VICI (Venus In Situ Composition Investigations): The Next Step in Understanding Venus Climate Evolution

    Science.gov (United States)

    Glaze, L. S.; Garvin, J. B.

    2017-12-01

    Venus provides a natural laboratory to explore an example of terrestrial planet evolution that may be cosmically ubiquitous. By better understanding the composition of the Venus atmosphere and surface, we can better constrain the efficiency of the Venusian greenhouse. VICI is a proposed NASA New Frontiers mission that delivers two landers to Venus on two separate Venus fly-bys. Following six orbital remote sensing missions to Venus (since 1978), VICI would be the first mission to land on the Venus surface since 1985, and the first U.S. mission to enter the Venus atmosphere in 49 years. The four major VICI science objectives are: Atmospheric origin and evolution: Understand the origin of the Venus atmosphere, how it has evolved, including how recently Venus lost its oceans, and how and why it is different from the atmospheres of Earth and Mars, through in situ measurements of key noble gases, nitrogen, and hydrogen. Atmospheric composition and structure: Reveal the unknown chemical processes and structure in Venus' deepest atmosphere that dominate the current climate through two comprehensive, in situ vertical profiles. Surface properties and geologic evolution: For the first time ever, explore the tessera from the surface, specifically to test hypotheses of ancient content-building cycles, erosion, and links to past climates using multi-point mineralogy, elemental chemistry, imaging and topography. Surface-atmosphere interactions: Characterize Venus' surface weathering environment and provide insight into the sulfur cycle at the surface-atmosphere interface by integrating rich atmospheric composition and structure datasets with imaging, surface mineralogy, and elemental rock composition. VICI is designed to study Venus' climate history through detailed atmospheric composition measurements not possible on earlier missions. In addition, VICI images the tessera surface during descent enabling detailed topography to be generated. Finally, VICI makes multiple elemental

  18. Geologic map of the Artemis Chasma quadrangle (V-48), Venus

    Science.gov (United States)

    Bannister, Roger A.; Hansen, Vicki L.

    2010-01-01

    . So although it seems clear what Artemis is not, there is little consensus about what Artemis is, much less how Artemis formed. Debate during the past decade has resulted in the proposal of at least four hypotheses for Artemis' formation. The first (herein referred to as H1) is that Artemis Chasma represents a zone of northwest-directed convergence and subduction. The second hypothesis (herein referred to as H2) is that Artemis consists of a composite structure with a part of its interior region marking the exposure of deformed ductile deep-crustal rocks analogous to a terrestrial metamorphic core complex. The third (herein referred to as H3) is that Artemis reflects the surface expression of an ancient (>3.5 Ga) huge bolide impact event on cold strong lithosphere. The fourth hypothesis (herein referred to as H4) is that Artemis marks the surface expression of a deep mantle plume. Each of these hypotheses holds different implications for Venus geodynamics and evolution processes, and for terrestrial planet processes in general. Viability of H1 would provide support that terrestrial-like plate-tectonic processes once occurred on Earth's sister planet. The feasibility of H2 would require high values of crustal extension and therefore imply that significant horizontal displacements occurred on Venus-displacement that may or may not be related to terrestrial-like plate-tectonic processes. The possibility of H3 would suggest that Venus' surface is extremely old, and that Venus has experienced very little dynamic activity for the last 3.5 billion years or more; this would further imply that Venus is essentially tectonically dead, and has been for most of its history. This view contrasts strongly with studies that highlight a rich history of Venus including activity at least as young as 750 million years ago, and quite likely up to the present. If H4 has credibility, then Artemis could provide clues to cooling mechanisms of Earth's sister planet. Each of these hypotheses

  19. Extreme Environments Technologies for Probes to Venus and Jupiter

    Science.gov (United States)

    Balint, Tibor S.; Kolawa, Elizabeth A.; Peterson, Craig E.; Cutts, James A.; Belz, Andrea P.

    2007-01-01

    This viewgraph presentation reviews the technologies that are used to mitigate extreme environments for probes at Venus and Jupiter. The contents include: 1) Extreme environments at Venus and Jupiter; 2) In-situ missions to Venus and Jupiter (past/present/future); and 3) Approaches to mitigate conditions of extreme environments for probes with systems architectures and technologies.

  20. Venus project : experimentation at ENEA`s pilot site

    Energy Technology Data Exchange (ETDEWEB)

    Bargellini, M.L.; Fontana, F. [ENEA, Centro Ricerche Casaccia, Rome (Italy). Dip. Innovazione; Bucci, C.; Ferrara, F.; Sottile, P.A. [GESI s.r.l., Rome (Italy); Niccolai, L.; Scavino, G. [Rome Univ. Sacro Cuore (Italy); Mancini, R.; Levialdi, S. [Rome Univ. La Sapienza (Italy). Dip. di Scienze dell`Informazione

    1996-12-01

    The document describes the ENEA`s (Italian Agency for New Technologies, Energy and the Environment) experience in the Venus Project (Esprit III ). Venus is an advanced visual interface based on icon representation that permits to end-user to inquiry databases. VENUS interfaces to ENEA`s databases: cometa materials Module, Cometa Laboratories Module and European Programs. This report contents the results of the experimentation and of the validation carried out in ENEA`s related to the Venus generations. Moreover, the description of the architecture, the user requirements syntesis and the validation methodology of the VENUS systems have been included.

  1. Venus - Volcano With Massive Landslides

    Science.gov (United States)

    1992-01-01

    This Magellan full-resolution mosaic which covers an area 143 by 146 kilometers (89 by 91 miles) is centered at 55 degrees north latitude, 266 degrees east longitude. The bright feature, slightly south of center is interpreted to be a volcano, 15-20 kilometers (9.3 to 12.4 miles) in diameter with a large apron of blocky debris to its right and some smaller aprons to its left. A preferred explanation is that several massive catastrophic landslides dropped down steep slopes and were carried by their momentum out into the smooth, dark lava plains. At the base of the east-facing or largest scallop on the volcano is what appears to be a large block of coherent rock, 8 to 10 kilometers (5 to 6 miles) in length. The similar margin of both the scallop and block and the shape in general is typical of terrestrial slumped blocks (masses of rock which slide and rotate down a slope instead of breaking apart and tumbling). The bright lobe to the south of the volcano may either be a lava flow or finer debris from other landslides. This volcanic feature, characterized by its scalloped flanks is part of a class of volcanoes called scalloped or collapsed domes of which there are more than 80 on Venus. Based on the chute-like shapes of the scallops and the existence of a spectrum of intermediate to well defined examples, it is hypothesized that all of the scallops are remnants of landslides even though the landslide debris is often not visible. Possible explanations for the missing debris are that it may have been covered by lava flows, the debris may have weathered or that the radar may not be recognizing it because the individual blocks are too small

  2. A Cubesat Mission to Venus: A Low-Cost Approach to the Investigation of Venus Lightning

    Science.gov (United States)

    Majid, W.; Duncan, C.; Kuiper, T.; Russell, C. T.; Hart, R. A.; Lightsey, E.

    2013-12-01

    The occurrence of Venus lightning has been detected by atmospheric probes and landers on Venus; by ionospheric satellites; by an orbiting visible spectrometer; at radio frequencies by the Galileo spacecraft while flying by Venus; and by an Earth-based telescope. However, none of these detectors has enabled us to determine the global occurrence rate of lightning in the atmosphere of Venus, nor the altitude at which this lightning is generated. Such measurements are needed in order to determine the processes that generate Venus lightning and to establish the importance of Venus lightning in controlling the chemical composition of the Venus atmosphere. A simple and affordable mission to perform this mapping could be achieved with CubeSat technology. A mother spacecraft with at least three CubeSat partners using RF detection could map the occurrence of lightning globally and determine its altitude of origin, with triangulation of precisely timed RF event arrivals. Such a mission would provide space for complementary investigations and be affordable under the Discovery mission program. We are embarking on a program to develop CubeSat-based instrumentation for such a mission. The initial task is to develop a lightning detector in a CubeSat development kit using a software defined radio (SDR) operating at decameter wavelengths (5-50 MHz). This involves algorithm development as well as selecting or developing radio hardware for a CubeSat. Two units will be tested on the ground in a lightning zone such as New Mexico, where the Long Wavelength Array operates in the same frequency range. When the concept has been proven, flight subsystems such as solar panels, attitude sensing and communication radios will be added to the CubeSats to test performance in low Earth orbit. Experience gained from flight would enable a cluster of sensors to be proposed for a future Venus mission.

  3. The puzzling transition region of Venus atmosphere studied by a ground-to-thermosphere 3D model

    Science.gov (United States)

    Gilli, Gabriella; Lebonnois, Sebastien; Machado, Pedro; Gonçalves, Ruben

    2017-10-01

    The middle/upper atmosphere of Venus, notably between 70 and 120 km, is the so-called “transition region” between the retrograde superrotating zonal flow dominating below 65 km, and the day-to-night circulation created by inhomogeneous heating by solar radiation above 120 km. Venus Express observations (2006-2014) showed that this region is more variable than expected, with latitude and day-to-day variations of temperature up to 80 K above 100 km at the terminator (Mahieux et al. 2015), and apparent zonal wind velocities measured around 96 km on the Venus nightime, highly changing in space and time (Soret et al. 2014). Those variations are not fully explained by current 3D models and specific processes (e.g. GW propagation, thermal tides, large scale planetary waves) responsible for driving them are still under investigation.We propose here to use the current improved version of the LMD Venus General Circulation Models (VGCM) (Lebonnois et al. 2016, Gilli et al. 2017) to yield insight into the global circulation of this region by fostering data-model synergies. Zonal wind predictions above 60 km by our VGCM showed to be consistent with available measurements (Peralta et al. 2017). On-going ground-based Venus observation on the cloud tops (~70 km) and below (Machado et al. 2017) will add complementary information to understand the coupling between the lower and upper atmosphere of Venus. In addition, observed O2(1Δ) nightglow, CO and O density (Gilli et al. 2015, Vandaele et al. 2016, Gerard et al. 2009), usually considered as sensitive transport tracers in the upper atmosphere of Venus where no direct wind measurements are available, will be interpret with the help of 3D model results.

  4. Effect Of Spaceflight On Microbial Gene Expression And Virulence: Preliminary Results From Microbe Payload Flown On-Board STS-115

    Science.gov (United States)

    Wilson, J. W.; HonerzuBentrup, K,; Schurr, M. J.; Buchanan, K.; Morici, L.; Hammond, T.; Allen, P.; Baker, C.; Ott, C. M.; Nelman-Gonzalez M.; hide

    2007-01-01

    Human presence in space, whether permanent or temporary, is accompanied by the presence of microbes. However, the extent of microbial changes in response to spaceflight conditions and the corresponding changes to infectious disease risk is unclear. Previous studies have indicated that spaceflight weakens the immune system in humans and animals. In addition, preflight and in-flight monitoring of the International Space Station (ISS) and other spacecraft indicates the presence of opportunistic pathogens and the potential of obligate pathogens. Altered antibiotic resistance of microbes in flight has also been shown. As astronauts and cosmonauts live for longer periods in a closed environment, especially one using recycled water and air, there is an increased risk to crewmembers of infectious disease events occurring in-flight. Therefore, understanding how the space environment affects microorganisms and their disease potential is critically important for spaceflight missions and requires further study. The goal of this flight experiment, operationally called MICROBE, is to utilize three model microbial pathogens, Salmonella typhimurium, Pseudomonas aeruginosa, and Candida albicans to examine the global effects of spaceflight on microbial gene expression and virulence attributes. Specifically, the aims are (1) to perform microarray-mediated gene expression profiling of S. typhimurium, P. aeruginosa, and C. albicans, in response to spaceflight in comparison to ground controls and (2) to determine the effect of spaceflight on the virulence potential of these microorganisms immediately following their return from spaceflight using murine models. The model microorganisms were selected as they have been isolated from preflight or in-flight monitoring, represent different degrees of pathogenic behavior, are well characterized, and have sequenced genomes with available microarrays. In particular, extensive studies of S. typhimurium by the Principal Investigator, Dr. Nickerson

  5. 10. The surface and interior of venus

    Science.gov (United States)

    Masursky, H.; Kaula, W.M.; McGill, G.E.; Pettengill, G.H.; Phillips, R.J.; Russell, C.T.; Schubert, G.; Shapiro, I.I.

    1977-01-01

    Present ideas about the surface and interior of Venus are based on data obtained from (1) Earth-based radio and radar: temperature, rotation, shape, and topography; (2) fly-by and orbiting spacecraft: gravity and magnetic fields; and (3) landers: winds, local structure, gamma radiation. Surface features, including large basins, crater-like depressions, and a linear valley, have been recognized from recent ground-based radar images. Pictures of the surface acquired by the USSR's Venera 9 and 10 show abundant boulders and apparent wind erosion. On the Pioneer Venus 1978 Orbiter mission, the radar mapper experiment will determine surface heights, dielectric constant values and small-scale slope values along the sub-orbital track between 50??S and 75??N. This experiment will also estimate the global shape and provide coarse radar images (40-80 km identification resolution) of part of the surface. Gravity data will be obtained by radio tracking. Maps combining radar altimetry with spacecraft and ground-based images will be made. A fluxgate magnetometer will measure the magnetic fields around Venus. The radar and gravity data will provide clues to the level of crustal differentiation and tectonic activity. The magnetometer will determine the field variations accurately. Data from the combined experiments may constrain the dynamo mechanism; if so, a deeper understanding of both Venus and Earth will be gained. ?? 1977 D. Reidel Publishing Company.

  6. Practical Observations of the Transit of Venus

    Indian Academy of Sciences (India)

    Home; Journals; Resonance – Journal of Science Education; Volume 9; Issue 5. Practical Observations of the Transit of Venus. B S Shyalaja. Classroom Volume 9 Issue 5 May 2004 pp 79-83. Fulltext. Click here to view fulltext PDF. Permanent link: https://www.ias.ac.in/article/fulltext/reso/009/05/0079-0083 ...

  7. Venus Clouds: A dirty hydrochloric acid model

    Science.gov (United States)

    Hapke, B.

    1971-01-01

    The spectral and polarization data for Venus are consistent with micron-sized, aerosol cloud particles of hydrochloric acid containing soluble and insoluble iron compounds, whose source could be volcanic or crustal dust. The ultraviolet features could arise from variations in the Fe-HCl concentration in the cloud particles.

  8. Abrir una Venus: Hablar con ella

    Directory of Open Access Journals (Sweden)

    Ginnette Barrantes Sáenz

    2013-09-01

    Se propone a Alicia como la Venus abierta que  incita, mediante  la  cita cinematográfica del cine mudo en el cine de Almodóvar, la no tan conocida figura de  amar a una  dormida( Allouch, 2005

  9. Solar Airplane Concept Developed for Venus Exploration

    Science.gov (United States)

    Landis, Geoffrey A.

    2004-01-01

    An airplane is the ideal vehicle for gathering atmospheric data over a wide range of locations and altitudes, while having the freedom to maneuver to regions of scientific interest. Solar energy is available in abundance on Venus. Venus has an exoatmospheric solar flux of 2600 W/m2, compared with Earth's 1370 W/m2. The solar intensity is 20 to 50 percent of the exoatmospheric intensity at the bottom of the cloud layer, and it increases to nearly 95 percent of the exoatmospheric intensity at 65 km. At these altitudes, the temperature of the atmosphere is moderate, in the range of 0 to 100 degrees Celsius, depending on the altitude. A Venus exploration aircraft, sized to fit in a small aeroshell for a "Discovery" class scientific mission, has been designed and analyzed at the NASA Glenn Research Center. For an exploratory aircraft to remain continually illuminated by sunlight, it would have to be capable of sustained flight at or above the wind speed, about 95 m/sec at the cloud-top level. The analysis concluded that, at typical flight altitudes above the cloud layer (65 to 75 km above the surface), a small aircraft powered by solar energy could fly continuously in the atmosphere of Venus. At this altitude, the atmospheric pressure is similar to pressure at terrestrial flight altitudes.

  10. Tidal constraints on the interior of Venus

    Science.gov (United States)

    Dumoulin, C.; Tobie, G.; Verhoeven, O.; Rosenblatt, P.; Rambaux, N.

    2017-12-01

    As a prospective study for a future exploration of Venus, we compute the tidal response of Venus' interior assuming various mantle compositions and temperature profiles representative of different scenarios of Venus' formation and evolution. The mantle density and seismic velocities are modeled from thermodynamical equilibria of mantle minerals and used to predict the moment of inertia, Love numbers, and tide-induced phase lag characterizing the signature of the internal structure in the gravity field. The viscoelasticity of the mantle is parameterized using an Andrade rheology. From the models considered here, the moment of inertia lies in the range of 0.327 to 0.342, corresponding to a core radius of 2900 to 3450 km. Viscoelasticity of the mantle strongly increases the potential Love number relative to previously published elastic models. Due to the anelasticity effects, we show that the possibility of a completely solid metal core inside Venus cannot be ruled out based on the available estimate of k2 from the Magellan mission (Konopliv and Yoder, 1996). A Love number k2 lower than 0.27 would indicate the presence of a fully solid iron core, while for larger values, solutions with an entirely or partially liquid core are possible. Precise determination of the Love numbers, k2 and h2, together with an estimate of the tidal phase lag, are required to determine the state and size of the core, as well as the composition and viscosity of the mantle.

  11. Venus: A contrast in evolution to Earth

    International Nuclear Information System (INIS)

    Kaula, W.M.

    1990-01-01

    Of the planets, Venus and Earth are by far the most similar in primary properties, yet they differ markedly in secondary properties. A great impact into Earth is believed to have created its moon and removed its atmosphere; the lack of such an impact into Venus apparently led to a greatly differing atmospheric evolution. The lack of an ocean on Venus prevents the recycling of volatiles and inhibits subduction, so that its crust is probable more voluminous than Earth's, although distorted and quite variable in thickness. Venus's upper mantle appears to be depleted in both volatiles and energy sources because, in addition to the lack of volatile recycling, melts of mantel rocks are more dense than their solid matrix at pressures above 8 gigapascals and hence sink if they occur at depths below 250 kilometers. Appreciable energy sources persist at great depths to sustain the few great mountain complexes. The greatest current problem is reconciling the likelihood of a voluminous crust with indications of considerable strength at shallow depths of 20 to 100 kilometers

  12. Venus: No Breaks from an Extended Childhood

    Science.gov (United States)

    Moore, W. B.; Kankanamge, D. G. J.

    2017-05-01

    High surface temperatures lead to lower heat flow and lower stress as planets transition out of the heat-pipe mode into subsolidus convection. This causes Venus to miss the window for plate tectonics due to an extended heat-pipe childhood.

  13. Sulfuric acid in the Venus clouds.

    Science.gov (United States)

    Sill, G. T.

    1972-01-01

    The extremely dry nature of the Venus upper atmosphere appears to demand the presence of an efficient desiccating agent as the chief constituent of the clouds of Venus. On the basis of polarization measures it is to be expected that this substance is present as spherical droplets, 1 to 2 microns in diameter, with a refractive index n of 1.46 plus or minus 0.02 at 3500A in the observed region of the atmosphere, with T about equal to 235 K. This substance must have ultraviolet, visible, and infrared reflection properties not inconsistent with the observed spectrum of Venus. Sulfuric acid, of about 86% by weight composition, roughly fulfills the first of these properties. The visible and ultraviolet transmission features of a thin layer of elemental bromine and hydrobromic acid dissolved in sulfuric acid somewhat resemble the Venus spectrum, up to 14 microns. The chemical process postulated for forming sulfuric acid involves the oxidation of sulfur and its compounds to sulfuric acid through the agency of elemental bromine produced by the photolytic decomposition of hydrogen bromide.

  14. Venus Global Reference Atmospheric Model Status and Planned Updates

    Science.gov (United States)

    Justh, H. L.; Cianciolol, A. M. Dwyer

    2017-01-01

    The Venus Global Reference Atmospheric Model (Venus-GRAM) was originally developed in 2004 under funding from NASA's In Space Propulsion (ISP) Aerocapture Project to support mission studies at the planet. Many proposals, including NASA New Frontiers and Discovery, as well as other studies have used Venus-GRAM to design missions and assess system robustness. After Venus-GRAM's release in 2005, several missions to Venus have generated a wealth of additional atmospheric data, yet few model updates have been made to Venus-GRAM. This paper serves to address three areas: (1) to present the current status of Venus-GRAM, (2) to identify new sources of data and other upgrades that need to be incorporated to maintain Venus-GRAM credibility and (3) to identify additional Venus-GRAM options and features that could be included to increase its capability. This effort will de-pend on understanding the needs of the user community, obtaining new modeling data and establishing a dedicated funding source to support continual up-grades. This paper is intended to initiate discussion that can result in an upgraded and validated Venus-GRAM being available to future studies and NASA proposals.

  15. Venus: The Atmosphere, Climate, Surface, Interior and Near-Space Environment of an Earth-Like Planet

    Science.gov (United States)

    Taylor, Fredric W.; Svedhem, Håkan; Head, James W.

    2018-02-01

    This is a review of current knowledge about Earth's nearest planetary neighbour and near twin, Venus. Such knowledge has recently been extended by the European Venus Express and the Japanese Akatsuki spacecraft in orbit around the planet; these missions and their achievements are concisely described in the first part of the review, along with a summary of previous Venus observations. The scientific discussions which follow are divided into three main sections: on the surface and interior; the atmosphere and climate; and the thermosphere, exosphere and magnetosphere. These reports are intended to provide an overview for the general reader, and also an introduction to the more detailed topical surveys in the following articles in this issue, where full references to original material may be found.

  16. Scene From The Birth Of Venus: Kajian Karya Fotografi

    Directory of Open Access Journals (Sweden)

    Agra Locita

    2016-01-01

    Full Text Available Scene From The Birth Of Venus is a photographic artwork that created in 1949. The artwork was the result of collaboration between Salvador Dali and two photographers, Baron George Hoyningen-Huene and George Platt Lynes. They created Birth of Venus differently with first painting whom created by Bottocelli Sandro. He depicted the goddess Venus graceful and shy, but it recreated by Salvador Dali in an imaginative photographic artwork. In Scene From The Birth Of Venus, the goddess Venus depicted as half human and fish. Two creations in different way but still in the birth of the goddess Venus theme.  Key words: photography, painting, imaginative

  17. Laboratory simulations of volcanic ash charging and conditions for volcanic lightning on Venus

    Science.gov (United States)

    Airey, Martin; Warriner-Bacon, Elliot; Aplin, Karen

    2017-04-01

    Lightning may be important in the emergence of life on Earth and elsewhere, as significant chemical reactions occur in the superheated region around the lightning channel. This, combined with the availability of phosphates in volcanic clouds, suggests that volcanic lightning could have been the catalyst for the formation of biological compounds on the early Earth [1]. In addition to meteorological lightning, volcanic activity also generates electrical discharges within charged ash plumes, which can be a significant contributor to atmospheric electricity on geologically active planets. The physical properties of other planetary atmospheres, such as that of Venus, have an effect on the processes that lead to the generation of volcanic lightning. Volcanism is known to have occurred on Venus in the past, and recent observations made by ESA's Venus Express satellite have provided evidence for currently active volcanism [2-4], and lightning discharges [e.g. 5]. Venusian lightning could potentially be volcanic in origin, since no meteorological mechanisms are known to separate charge effectively in its clouds [6]. The hunt for further evidence for lightning at Venus is ongoing, for example by means of the Lightning and Airglow Camera (LAC) [7] on Akatsuki, the current JAXA mission at Venus. Our laboratory experiments simulate ash generation and measure electrical charging of the ash under typical atmospheric conditions on Earth and Venus. The study uses a 1 litre chamber, which, when pressurised and heated, can simulate the high-pressure, high-temperature, carbon dioxide-dominated atmosphere of Venus at 10 km altitude ( 5 MPa, 650 K). A key finding of previous work [8] is that ash plume-forming eruptions are more likely to occur at higher altitudes such as these on Venus. The chamber contains temperature/pressure monitoring and logging equipment, a rock collision apparatus (based on [9]) to generate the charged rock fragments, and charge measurement electrodes connected

  18. MEETING VENUS. A Collection of Papers presented at the Venus Transit Conference Tromsoe 2012

    Science.gov (United States)

    Sterken, Christiaan; Aspaas, Per Pippin

    2013-05-01

    On 2-3 June 2012, the University of Tromsoe hosted a conference about the cultural and scientific history of the transits of Venus. The conference took place in Tromsoe for two very specific reasons. First and foremost, the last transit of Venus of this century lent itself to be observed on the disc of the Midnight Sun in this part of Europe during the night of 5 to 6 June 2012. Second, several Venus transit expeditions in this region were central in the global enterprise of measuring the scale of the solar system in the eighteenth century. The site of the conference was the Nordnorsk Vitensenter (Science Centre of Northern Norway), which is located at the campus of the University of Tromsoe. After the conference, participants were invited to either stay in Tromsoe until the midnight of 5-6 June, or take part in a Venus transit voyage in Finnmark, during which the historical sites Vardoe, Hammerfest, and the North Cape were to be visited. The post-conference program culminated with the participants observing the transit of Venus in or near Tromsoe, Vardoe and even from a plane near Alta. These Proceedings contain a selection of the lectures delivered on 2-3 June 2012, and also a narrative description of the transit viewing from Tromsoe, Vardoe and Alta. The title of the book, Meeting Venus, refers the title of a play by the Hungarian film director, screenwriter and opera director Istvan Szabo (1938-). The autobiographical movie Meeting Venus (1991) directed by him is based on his experience directing Tannhauser at the Paris Opera in 1984. The movie brings the story of an imaginary international opera company that encounters a never ending series of difficulties and pitfalls that symbolise the challenges of any multicultural and international endeavour. As is evident from the many papers presented in this book, Meeting Venus not only contains the epic tales of the transits of the seventeenth, eighteenth and nineteenth centuries, it also covers the conference

  19. The Venus Emissivity Mapper - gaining a global perspective on the surface composition of Venus

    Science.gov (United States)

    Helbert, Joern; Dyar, Melinda; Widemann, Thomas; Marcq, Emmanuel; Maturilli, Alessandro; Mueller, Nils; Kappel, David; Ferrari, Sabrina; D'Amore, Mario; Tsang, Constantine; Arnold, Gabriele; Smrekar, Suzanne; VEM Team

    2017-10-01

    The permanent cloud cover of Venus prohibits observations of the surface with traditional imaging techniques over much of the EM spectral range, leading to the false notion that information about the composition of Venus’ surface could only be derived from lander missions. However, harsh environmental conditions on the surface cause landed missions to be sole site, highly complex, and riskier than orbiting missions.It is now known that 5 transparency windows occur in the Venus atmosphere, ranging from 0.86 µm to 1.18 µm. Recent advances in high temperature laboratory spectroscopy at the PSL at DLR these windows are highly diagnostic for surface mineralogy. Mapping of the southern hemisphere of Venus with VIRTIS on VEX in the 1.02 µm band was a proof-of-concept for an orbital remote sensing approach to surface composition and weathering studies[1-3]. The Venus Emissivity Mapper [4] proposed for the NASA’s Venus Origins Explorer (VOX) and the ESA EnVision proposal builds on these recent advances. It is the first flight instrument specially designed with a sole focus on mapping the surface of Venus using the narrow atmospheric windows around 1 µm. Operating in situ from Venus orbit, VEM will provide a global map of surface composition as well as redox state of the surface, providing a comprehensive picture of surface-atmosphere interaction and support for landing site selection. Continuous observation of the thermal emission of the Venus will provide tight constraints on the current day volcanic activity[5]. This is complemented by measurements of atmospheric water vapor abundance as well as cloud microphysics and dynamics. These data will allow for accurate correction of atmospheric interference on the surface measurements, which provide highly valuable science on their own. A mission combining VEM with a high-resolution radar mapper such as VOX or EnVision in a low circular orbit will provide key insights into the divergent evolution of Venus.1. Smrekar, S

  20. The escape of natural satellites from Mercury and Venus

    International Nuclear Information System (INIS)

    Kumar, S.S.

    1977-01-01

    It is suggested that the slow rotations of Mercury and Venus may be connected with the absence of natural satellites around them. If Mercury or Venus possessed a satellite at the time of formation, the tidal evolution would have caused the satellite to recede. At a sufficiently large distance from the planet, the Sun's gravitational influence makes the satellite orbit unstable. The natural satellites of Mercury and Venus might have escaped as a consequence of this instability. (Auth.)

  1. Venus transit 2004: An international education program

    Science.gov (United States)

    Mayo, L.; Odenwald, S.

    2003-04-01

    December 6th, 1882 was the last transit of the planet Venus across the disk of the sun. It was heralded as an event of immense interest and importance to the astronomical community as well as the public at large. There have been only six such occurrences since Galileo first trained his telescope on the heavens in 1609 and on Venus in 1610 where he concluded that Venus had phases like the moon and appeared to get larger and smaller over time. Many historians consider this the final nail in the coffin of the Ptolemaic, Earth centered solar system. In addition, each transit has provided unique opportunities for discovery such as measurement and refinement of the detection of Venus' atmosphere, calculation of longitudes, and calculation of the astronomical unit (and therefore the scale of the solar system). The NASA Sun Earth Connection Education Forum (SECEF) in partnership with the Solar System Exploration (SSE) and Structure and Evolution of the Universe (SEU) Forums, AAS Division for Planetary Sciences (DPS), and a number of NASA space missions and science centers are developing plans for an international education program centered around the June 8, 2004 Venus transit. The transit will be visible in its entirety from Europe and partially from the East Coast of the United States. We will use a series of robotic observatories including the Telescopes In Education (TIE) network distributed in latitude to provide observations of the transit that will allow middle and high school students to calculate the A.U. through application of parallax. We will compare the terrestrial planets in terms of the evolutionary processes that define their magnetic fields, their widely differing interactions with the solar wind, and the implications this has for life on Earth and elsewhere in the universe. We will also use Venus transit as a probe of episodes in American history (e.g. 1769: revolutionary era, 1882: post civil war era, and 2004: modern era). Museums and planetariums in

  2. Venus y el fin del mundo

    Directory of Open Access Journals (Sweden)

    Gonzalo Munévar

    2006-01-01

    Full Text Available Este artículo busca demostrar que los argumentos generales acerca de la exploración científica valen también para las ciencias espaciales. El trabajo se basa en el ejemplo de la exploración de Venus y lo que esta nos dice acerca de nuestro propio planeta. Argumenta que el concepto de la probabilidad de Leslie es incorrecto, como también lo son las dudas sobre la evidencia Venusiana. Así mismo, concluye que no se puede rechazar la importancia que tienen los descubrimientos inesperados que han resultado de la exploración de Venus para ayudarnos a comprender nuestro propio planeta. Y que si van a ser rechazados estos descubrimientos debe ser por razones científicas, no por intuiciones acerca de la probabilidad.

  3. The cartography of Venus with Magellan data

    Science.gov (United States)

    Kirk, R. L.; Morgan, H. F.; Russell, J. F.

    1993-01-01

    Maps of Venus based on Magellan data are being compiled at 1:50,000,000, 1:5,000,000 and 1:1,500,000 scales. Topographic contour lines based on radar altimetry data are overprinted on the image maps, along with feature nomenclature. Map controls are based on existing knowledge of the spacecraft orbit; photogrammetric triangulation, a traditional basis for geodetic control for bodies where framing cameras were used, is not feasible with the radar images of Venus. Preliminary synthetic aperture radar (SAR) image maps have some data gaps and cosmetic inconsistencies, which will be corrected on final compilations. Eventual revision of geodetic controls and of the adopted Venusian spin-axis location will result in geometric adjustments, particularly on large-scale maps.

  4. On the Geological History of Venus

    Science.gov (United States)

    Basilevsky, A. T.; Head, J. W.

    2008-09-01

    mostly based on the analysis of data acquired by the Magellan mission: SAR images with 100-200 m resolution and the maps of topography, surface radar reflectivity, emissivity, roughness and gravity anomalies [1]. After initial analysis of the data summarized in [2, 3] several groups of researchers continued to study the geology and geophysics of the planet, resulting in numerous publications, some of which are referenced below. Very important for the studies emphasizing the geologic history of Venus was, and still is, a program of 1:5,000,000 geologic mapping coordinated by the US Geological Survey [4]. A recent summary of these studies can be found in [5]. Observations and analysis: All researchers in this study area analyze the same data sets and follow the same guidelines [4, 6] so geologic units identified by them and their time sequences are generally similar, although different researchers may name the same units differently and may interpret differently some details of local time sequences. Figure 1 shows a time sequence of geologic units suggested by [7, 8]: materials of tessera terrain (tt), densely fractured plains (pdf), fractured and ridged plains (pfr), shield plains (psh), plains with wrinkle ridges (pwr), lobate (pl) and smooth (ps) plains as well as materials of radar-dark craterassociated parabolas (cdp). These are material units. In addition, some researchers identify and map structural units. In Figure 1 examples of these are fracture belts (fb) and rifted terrain (rt). synchronous on a global scale. The first option can be visualized with Figure 1, suggesting that it is applicable for Venus globally. This option was suggested by Basilevsky and Head [e.g., 7, 8] as well as by Ivanov and Head [e.g., 9]. The second option, first clearly formulated by [10], can be visualized by the upper part of Figure 2 showing the situation in three different hypothetical geologic provinces on Venus. In these provinces the unit time sequences are the same: tt

  5. Venus clouds - A dirty hydrochloric acid model.

    Science.gov (United States)

    Hapke, B.

    1972-01-01

    The spectral and polarization data for Venus are consistent with micrometer-sized aerosol cloud particles of hydrochloric acid with soluble and insoluble iron compounds, whose source could be volcanic or crustal dust. The yellow color of the clouds could be due to absorption bands in the near UV involving ferric iron and chlorine complexes. It is pointed out that the UV features could arise from variations in the concentrations of iron and hydrochloric acid in the cloud particles.

  6. Probing the Interior Structure of Venus

    OpenAIRE

    Stevenson, David J.; Cutts, James A.; Mimoun, David; Arrowsmith, Stephen; Banerdt, W. Bruce; Blom, Philip; Brageot, Emily; Brissaud, Quentin; Chin, Gordon; Gao, Peter; Garcia, Raphael; Hall, Jeffrey L.; Hunter, Gary; Jackson, Jennifer M.; Kerzhanovich, V. V.

    2015-01-01

    The formation, evolution, and structure of Venus remain a mystery more than 50 years after the first visit by a robotic spacecraft. Radar images have revealed a surface that is much younger than those of the Moon, Mercury, and Mars as well as a variety of enigmatic volcanic and tectonic features quite unlike those we are familiar with on Earth. What are the dynamic processes that shape these features, in the absence of any plate tectonics? What is their relationship with the de...

  7. Energetics of the dayside ionosphere of Venus

    Science.gov (United States)

    Dobe, Zoltan; Nagy, Andrew F.; Brace, Larry H.; Cravens, Thomas E.; Luhmann, Janet G.

    1993-01-01

    A reanalysis of the Pioneer Venus electron temperature data base showed a strong correlation between elevated electron temperatures and induced magnetic fields in the dayside ionosphere above about 200 km. These results suggest, although not conclusively, that the elevated temperatures are the result of reduced vertical conductivities caused by the horizontal, induced fields with a possible contribution from energy deposition by magnetosheath electrons moving along the field from the tail region.

  8. Present Status of Janaese Venus Climate Orbiter

    Science.gov (United States)

    Nakamura, M.; Imamura, T.; Ishii, N.; Satoh, T.; Abe, T.; Ueno, M.; Suzuki, M.; Yamazaki, A.

    2007-08-01

    The start of the Japanese Venus Exploration program was in 2001, and last year (2006) we moved it to Phase C after PDR in August.We would like to report the present status of our Venus Climate Orbiter. Planet-C is the project name in ISAS/JAXA. The launch vehicle is changed from M-V to H-IIA. It will be launched from Tanegashima Space Center (TNSC) in Kagoshima. With this modification, we changed some minor design of the spacecraft and the total weight is slightly heavier than before, but the basic design has not been modified. The launch window will be kept in summer in 2010 and it will arrive at Venus in December 2010. The spacecraft will be directly put into the interplanetary orbit. Now we are preparing the Mechanical and Thermal engineering Model (MTM) which will end in middle of 2007 and will shake it and do the thermal vacuum test. Later this model will be modified to the flight model and the final integration test will be in 2009 which takes 1 year. Development of all the science instruments are going well. The first integration test of science instruments will be in August this year. We can report the results of it in the meeting.

  9. Buddy Board

    DEFF Research Database (Denmark)

    Enggaard, Helle; Moselund, Lene

    2015-01-01

    Projekt ’BuddyBoard’ er kommet i stand via et samarbejde mellem Frederikshavn kommune, Bunker43 og Lab. X. Afdeling en ’Havly’ på Sæby Ældrecenter fungerer som living lab, hvilket betyder, at det udgør et levende laboratorium for udvikling og afprøvning af teknologi (Schultz, 2013). Projektet er....... Bunker43 har udviklet en teknologi (BuddyBoard) til hurtig formidling af billeder fra pårørende og personale til beboere på institutioner. Pårørende og personale uploader billeder via en APP eller en hjemmeside og har mulighed for at tilføje en kort forklarende tekst til hvert billede. Beboeren ser...... billederne via en tablet. Systemet bygger på et simpelt og brugervenligt design, så ældre med kognitive og/eller fysiske funktionsnedsættelser kan anvende teknologien. BuddyBoard fungerer via internettet, og billederne gemmes på en sikret server hos udbyderen, som er Bunker43. Intentionerne med BuddyBoard er...

  10. SAEVe: A Long Duration Small Sat Class Venus Lander - Seismic and Atmospheric Exploration of Venus

    Science.gov (United States)

    Kremic, Tibor; Ghail, Richard; Gilmore, Martha; Hunter, Gary; Kiefer, Walter; Limaye, Sanjay; Pauken, Michael; Tolbert, Carol; Wilson, Colin

    2017-01-01

    NASA's science mission directorate has put increasing emphasis on innovative, smaller, and lower cost missions to achieve their science objectives. One example of this was the recent call by the Planetary Science Division for cube and small satellite concepts expected to cost $100M or less, not including launch and weighing less than 180kg. Over 100 proposals were submitted suggesting that indeed this is a size of mission worthy of being considered in future planning. Nineteen missions were selected for study, one being a long-lived Venus mission called SAEVe, for Seismic and Atmospheric Exploration of Venus. The science objectives and relevance of SAEVe include: Is Venus seismically active? What can we learn about its crust (thickness and composition) and its interior (lithosphere, mantle, and core)? What can be learned about its evolutionary history or about the planet / atmosphere interactions? SAEVe begins to address these science questions with simple, but capable, instrumented probes that can survive on the surface of Venus and take temporal measurements over months something never attempted before. The data returned will further our understanding of the solar system and Earth, and aid in meeting the NASA Science Plan goal to ascertain the content, origin, and evolution of the solar system and the chemical and physical processes in our solar system. SAEVe is delivered to Venus as a ride-along on another mission to Venus. Its two small probes are placed into the Venus atmosphere via a single Stardust-like entry capsule, are ejected at different times, free fall, and decelerate in the thickening atmosphere to touchdown under 8 m/s2 or less. The probes will begin taking measurements and transmitting important parameters at or near the surface and will focus on measurements like seismic activity, heat flux, wind speed and direction, basic chemical abundances, temperature, and pressure. At preset intervals, the probes acquire the science measurements and beam the

  11. Long-term Behaviour Of Venus Winds At Cloud Level From Virtis/vex Observations

    Science.gov (United States)

    Hueso, Ricardo; Peralta, J.; Sánchez-Lavega, A.; Pérez-Hoyos, S.; Piccioni, G.; Drossart, P.

    2009-09-01

    The Venus Express (VEX) mission has been in orbit to Venus for more than three years now. The VIRTIS instrument onboard VEX observes Venus in two channels (visible and infrared) obtaining spectra and multi-wavelength images of the planet. Images in the ultraviolet range are used to study the upper cloud at 66 km while images in the infrared (1.74 μm) map the opacity of the lower cloud deck at 48 km. Here we present an analysis of the overall dynamics of Venus’ atmosphere at both levels using observations that cover a large fraction of the VIRTIS dataset. We will present our latest results concerning the zonal winds, the overall stability in the lower cloud deck motions and the variability in the upper cloud. Meridional winds are also observed in the upper and lower cloud in the UV and IR images obtained with VIRTIS. While the upper clouds present a net meridional motion consistent with the upper branch of a Hadley cell the lower cloud present more irregular, variable and less intense motions in the meridional direction. Acknowledgements This work has been funded by Spanish MEC AYA2006-07735 with FEDER support and Grupos Gobierno Vasco IT-464-07. RH acknowledges a "Ramón y Cajal” contract from MEC.

  12. Evolution of a Coronal Mass Ejection from the Sun to Mercury, Venus, Earth and Beyond

    Science.gov (United States)

    Wang, Y.; Shen, C.; Liu, J.; Mengjiao, X.; Guo, J.

    2017-12-01

    A clear magnetic cloud was observed by Messenger at Mercury. By using coronagraph images from SOHO/LASCO and STEREO/COR and the in-situ data from Wind near the Earth, we estimated its propgation velocity and identified the possible CME candidate in the corona and its counterpart recorded by Venus Express near Venus. By applying the CME's DIPS (Deflection in InterPlanetary Space) model, we show that the CME's arrivals at the three different heliocentric distance can be well reproduced. By extending the trajectory of the CME to the orbitor of Mars, we predict the arrival of the CME at Mars, which is in agreement with a significant Forbush decrease observed by MSL. We use uniformly-twisted force-free flux rope model to fit the in-situ measurements at Mercury, Venus and the Earth to study the evolution of the magnetic flux rope, and find that both axial magnetic flux and twist significantly decreased, suggesting that a significant erosion process was on-going and might change the averaged twist of the magnetic flux rope.

  13. Structural evolution of western Fortuna Tessera, Venus

    Science.gov (United States)

    Pritchard, M. E.; Hansen, V. L.; Willis, J. J.

    1997-09-01

    Western Fortuna Tessera, Ishtar Terra, records polyphase deformation. Structures include: ribbons forming long, narrow, steep-sided troughs that reflect surface layer extension; N-trending folds related to Maxwell Montes deformation; short, wide, NW-trending graben that reflect late local extension; and, within the southwestern map area, gentle, E-trending warps, which postdate ribbon structures. Flood lava flows postdate deformation. Ribbon structures change orientation radially from NNE to WNW. These observations caution against the correlation of Fortuna Tessera with tessera elsewhere on Venus and against the proposal that tessera forms a global stratigraphic layer.

  14. Venus gravity - Analysis of Beta Regio

    Science.gov (United States)

    Esposito, P. B.; Sjogren, W. L.; Mottinger, N. A.; Bills, B. G.; Abbott, E.

    1982-01-01

    Radio tracking data acquired over Beta Regio were analyzed to obtain a surface mass distribution from which a detailed vertical gravity field was derived. In addition, a corresponding vertical gravity field was evaluated solely from the topography of the Beta region. A comparison of these two maps confirms the strong correlation between gravity and topography which was previously seen in line-of-sight gravity maps. It also demonstrates that the observed gravity is a significant fraction of that predicted from the topography alone. The effective depth of complete isostatic compensation for the Beta region is estimated to be 330 km, which is somewhat deeper than that found for other areas of Venus.

  15. Analysis of VENUS-3 benchmark experiment

    International Nuclear Information System (INIS)

    Kodeli, I.; Sartori, E.

    1998-01-01

    The paper presents the revision and the analysis of VENUS-3 benchmark experiment performed at CEN/SCK, Mol (Belgium). This benchmark was found to be particularly suitable for validation of current calculation tools like 3-D neutron transport codes, and in particular of the 3D sensitivity and uncertainty analysis code developed within the EFF project. The compilation of the integral experiment was integrated into the SINBAD electronic data base for storing and retrieving information about the shielding experiments for nuclear systems. SINBAD now includes 33 reviewed benchmark descriptions and several compilations waiting for the review, among them many benchmarks relevant for pressure vessel dosimetry system validation.(author)

  16. HIGH-RESOLUTION SATELLITE IMAGING OF THE 2004 TRANSIT OF VENUS AND ASYMMETRIES IN THE CYTHEREAN ATMOSPHERE

    International Nuclear Information System (INIS)

    Pasachoff, Jay M.; Schneider, Glenn; Widemann, Thomas

    2011-01-01

    This paper presents the only space-borne optical-imaging observations of the 2004 June 8 transit of Venus, the first such transit visible from Earth since AD 1882. The high-resolution, high-cadence satellite images we arranged from NASA's Transition Region and Coronal Explorer (TRACE) reveal the onset of visibility of Venus's atmosphere and give further information about the black-drop effect, whose causes we previously demonstrated from TRACE observations of a transit of Mercury. The atmosphere is gradually revealed before second contact and after third contact, resulting from the changing depth of atmospheric layers refracting the photospheric surface into the observer's direction. We use Venus Express observations to relate the atmospheric arcs seen during the transit to the atmospheric structure of Venus. Finally, we relate the transit images to current and future exoplanet observations, providing a sort of ground truth showing an analog in our solar system to effects observable only with light curves in other solar systems with the Kepler and CoRoT missions and ground-based exoplanet-transit observations.

  17. Speech and Expression Outside the Classroom as Elements of a School Board's Determination of Teaching Fitness: A Case Study of a Gay Activist.

    Science.gov (United States)

    Rizzi, Joseph A.; Jacobs, Robert M.

    Via a case study, this paper explores the legal question of whether a local school board's inquiry into the fitness of its teachers can extend outside the classroom. This issue is discussed within the framework of two divergent views concerning the absolute nature of First Amendment rights on the one hand and a compelling state interest that may…

  18. FINANCE BOARD, MANAGEMENT BOARD AND COLLABORATION BOARD

    CERN Multimedia

    M. Della Negra

    Common Meeting FB/MB/CB (FMC20) Electronics Issues The key dates for the Low Voltage Power distribution were presented. It is critical that the uninterruptible power supply be installed. There is a programme of installation underground leading up to the start of commissioning underground in March 2007, when all detectors should be read out underground. The overall status of the Electronics production was presented. The Low Voltage power supplies remain a concern and close cooperation with the manufacturers will be essential to have deliveries as needed. The failure of some components are mostly understood now. There are new proposals for the SLHC machine parameters, where it is essential that CMS give feed-back. A CMS Expression of Interest is almost complete and will be circulated to the Collaboration the following week. It will be submitted to the LHCC in December 2006. The Letter of Intent, a larger document, will be submitted in summer 2007. Technical Issues The main issue is the schedule, which h...

  19. Geologic processes on Venus: an update

    Science.gov (United States)

    Masursky, H.

    Studies of Venera 15 and 16 radar image and altimetry data and reevaluation of Pioneer Venus and earlier Venera data have greatly expanded the perception of the variety and complexity of geologic processes on Venus. PV data have discriminated four highland regions (each different in geomorphic appearance), a large upland rolling plains region, and smaller areas of lowland plains. Two highland volcanic centers were identified that may be presently active, as suggested by their geomorphologic appearance combined with positive gravity anomalies, lightning strike clusters, and a change in SO2 content in the upper atmosphere. Geochemical data obtained by the Venera landers have indicated that one upland area and nearby rolling plains are composed of volcanic rocks, probably basalts or syenites. New Venera radar images of the Ishtar Terra region show folded and/or faulted linear terrain and associated volcanic features that may have been deformed by both compressional and extensional forces. Lowland surfaces resemble the mare basaltic lava flows that fill basins on the Moon, Mars and Earth. Ubiquitous crater like forms may be of either volcanic or impact origin; the origin of similar lunar features was determined by the character of their ejecta deposits.

  20. Geology of the Venus equatorial region from Pioneer Venus radar imaging

    International Nuclear Information System (INIS)

    Senske, D.A.; Head, J.W.

    1989-01-01

    The surface characteristics and morphology of the equatorial region of Venus were first described by Masursky et al. who showed this part of the planet to be characterized by two topographic provinces, rolling plains and highlands, and more recently by Schaber who described and interpreted tectonic zones in the highlands. Using Pioneer Venus (PV) radar image data (15 deg S to 45 deg N), Senske and Head examined the distribution, characteristics, and deposits of individual volcanic features in the equatorial region, and in addition classified major equatorial physiographic and tectonic units on the basis of morphology, topographic signature, and radar properties derived from the PV data. Included in this classification are: plains (undivided), inter-highland tectonic zones, tectonically segmented linear highlands, upland rises, tectonic junctions, dark halo plains, and upland plateaus. In addition to the physiographic units, features interpreted as coronae and volcanic mountains have also been mapped. The latter four of the physiographic units along with features interpreted to be coronae

  1. Geology of the Venus equatorial region from Pioneer Venus radar imaging

    Science.gov (United States)

    Senske, D. A.

    1990-01-01

    The data collected by Pioneer Venus have been used to map the broad radar characteristics of the equatorial region on the basis of radar brightness and texture. Seven units are defined and are used to assess the geologic character of the equatorial region. The correspondence between features in the 15 deg region of overlap between Pioneer Venus ans Venera 15/16 images is examined and used to extend units mapped in the northern high latitudes into the equatorial region. Using the properties of rms slope, reflectivity, the scattering behavior of the surface, and topographic signature, seven physiographic units are mapped on the basis of the distribution of the radar units in the equatorial region and are identified by increasing complexity as plains, dark halo plains, upland rises, upland plateaus, interhighland tectonic zones, tectonically segmented linear highlands, and tectonic junctions. The distribution of larger circular structures interpreted as coronae is also examined.

  2. Experimental reconstruction of Lomonosov's discovery of Venus's atmosphere with antique refractors during the 2012 transit of Venus

    Science.gov (United States)

    Koukarine, A.; Nesterenko, I.; Petrunin, Yu.; Shiltsev, V.

    2013-11-01

    In 1761, the Russian polymath Mikhail Vasilievich Lomonosov (1711-1765) discovered the atmosphere of Venus during its transit over the Sun's disc. In this paper we report on experimental reenactments of Lomonosov's discovery with antique refractors during the transit of Venus June 5-6, 2012. We conclude that Lomonosov's telescope was fully adequate to the task of detecting the arc of light around Venus off the Sun's disc during ingress or egress provided proper experimental techniques as described by Lomonosov in his 1761 report are employed.

  3. Venus surface peeking through the atmosphere - gaining a global perspective on the surface composition through near infrared observations

    Science.gov (United States)

    Helbert, J.; Dyar, M. D.; Maturilli, A.; D'Amore, M.; Ferrari, S.; Mueller, N. T.; Smrekar, S. E.

    2017-12-01

    Venus is the most Earth-like of the terrestrial planets, though very little is known about its surface composition. Thanks to recent advances in laboratory spectroscopy and spectral analysis techniques, this is about to change. Although the atmosphere prohibits observations of the surface with traditional imaging techniques over much of the EM spectral range, five transparent windows between 0.86 µm and 1.18 µm occur in the atmosphere's CO2 spectrum. New high temperature laboratory spectra from the Planetary Spectroscopy Laboratory at DLR show that spectra in these windows are highly diagnostic for surface mineralogy [1]. The Venus Emissivity Mapper (VEM) [2] builds on these recent advances. It is proposed for NASA's Venus Origins Explorer where a radar will provided the needed high-resolution altimetry and ESA's EnVision would provide stereo topography instead. VEM is the first flight instrument specially designed to focus solely on mapping Venus' surface using the windows around 1 µm. Operating in situ from Venus orbit, VEM will provide a global map of composition as well as redox state of the surface, enabling a comprehensive picture of surface-atmosphere interaction on Venus. VEM will return a complex data set containing surface, atmospheric, cloud, and scattering information. Total planned data volume for a typical mission scenario exceeds 1TB. Classical analysis techniques have been successfully used for VIRTIS on Venus Express [3-5] and could be employed with the VEM data. However, application of machine learning approaches to this rich dataset is vastly more efficient, as has already been confirmed with laboratory data. Binary classifiers [6] demonstrate that at current best estimate errors, basalt spectra are confidently discriminated from basaltic andesites, andesites, and rhyolite/granite. Applying the approach of self-organizing maps to the increasingly large set of laboratory measurements allows searching for additional mineralogical indicators

  4. Development of Venus Balloon Seismology Missions Through Earth Analog Experiments

    Science.gov (United States)

    Krishnamoorthy, S.; Komjathy, A.; Cutts, J. A.; Pauken, M. T.; Garcia, R. F.; Mimoun, D.; Jackson, J. M.; Kedar, S.; Smrekar, S. E.; Hall, J. L.

    2017-11-01

    The study of a planet’s seismic activity is central to the understanding of its internal structure. We discuss advances made through Earth analog testing for performing remote seismology on Venus using balloons floated in the mid-atmosphere.

  5. Plumes as a Mechanism for Equilibrium Resurfacing of Venus

    Science.gov (United States)

    Hansen, V. L.; Young, D. A.

    2004-03-01

    End member hypotheses catastrophic- and equilibrium-volcanic-resurfacing fall short in addressing Venus' crater database, and both assume crater removal by burial. We propose an alternative hypothesis that includes crater destruction by annealing.

  6. In Situ Partial Melt on Venus: Evidence for Ancient Water?

    Science.gov (United States)

    Hansen, V. L.

    2003-03-01

    Shield terrain comprises countless tiny lava flows that coalesced to form an ultra-thin discontinuous regionally extensive mechanically strong layer; lava represents point-source crustal partial melt and may provide evidence for ancient Venus water.

  7. Venus Preserves a Rare Record of Early Terrestrial Planet Processes

    Science.gov (United States)

    Hansen, V. L.; López, I.

    2009-03-01

    Geologic relations and thermal modeling indicate that ribbon tessera terrain (rtt) records a unique and ancient era of Venus evolution. A new global geologic map of rtt preserves a rare record of early terrestrial planet evolution processes.

  8. Harsh Environment Gas Sensor Array for Venus Atmospheric Measurements Project

    Data.gov (United States)

    National Aeronautics and Space Administration — Makel Engineering and the Ohio State University propose to develop a harsh environment tolerant gas sensor array for atmospheric analysis in future Venus missions....

  9. Dynamics of the atmosphere. [spacecraft observations of Venus

    Science.gov (United States)

    Elson, L. S.

    1982-01-01

    Observations of and possible explanations for the dynamics of the Venus atmosphere as revelaed by Pioneer Venus and the Venera spacecraft are discussed. An important observation was that the entire atmosphere moves in the same retrograde (westward) direction at average speeds of up to about 110 m/sec, which may be explained by zonal jets arising from interactions of meridional cells, viscosity and solar heating. Atmospheric thermal tides, temperature and wind perturbations caused by solar heating were also observed which may have influences on tidal winds and warming at the poles. In addition, atmospheric waves with periods of 5.3 and 2.9 earth days have been detected between the Venus cloud tops, and calculations of baroclinically unstable waves on Venus have been made with a general circulation model.

  10. Sapphire Viewports for a Venus Probe, Phase I

    Data.gov (United States)

    National Aeronautics and Space Administration — The proposed Phase 1 program will demonstrate that sapphire viewports are feasible for use in Venus probes. TvU's commercial viewport products have demonstrated that...

  11. Thermal Insulator for a Venus Lander, Phase I

    Data.gov (United States)

    National Aeronautics and Space Administration — A lander on the surface of Venus is heated by the 460 C surface temperature, which, even with the best current designs using passive insulation, cause its...

  12. Earth-type planets (Mercury, Venus, and Mars)

    Science.gov (United States)

    Marov, M. Y.; Davydov, V. D.

    1975-01-01

    Spacecraft- and Earth-based studies on the physical nature of the planets Mercury, Venus, and Mars are reported. Charts and graphs are presented on planetary surface properties, rotational parameters, atmospheric compositions, and astronomical characteristics.

  13. Transit of Venus: Quantitative Observing with Simple Equipment The ...

    Indian Academy of Sciences (India)

    gmail.com. The possibilities of quantitative student observations during the transit of Venus, using simple equipment, are discussed. The equipment could ... These observations could have been by naked eye and the above reference seems to ...

  14. Power System for Venus Surface Exploration

    Science.gov (United States)

    Landis, Geoffrey A.; Mellott, Kenneth

    2002-01-01

    A radioisotope power and cooling system is designed to provide electrical power for a probe operating on the surface of Venus. Most foreseeable electronics devices and sensors cannot operate at the 450 C ambient surface temperature of Venus. Because the mission duration is substantially long and the use of thermal mass to maintain an operable temperature range is likely impractical, some type of active refrigeration may be required to keep electronic components at a temperature below ambient. The fundamental cooling parameters are the cold sink temperature, the hot sink temperature, and the amount of heat to be removed. In this instance, it is anticipated that electronics would have a nominal operating temperature of 300 C. Due to the highly thermal convective nature of the high-density (90 bar CO2) atmosphere, the hot sink temperature was assumed to be 50 C, which provided a 500 C temperature of the cooler's heat rejecter to the ambient atmosphere. The majority of the heat load on the cooler is from the high temperature ambient surface environment on Venus, with a small contribution of heat generation from electronics and sensors. Both thermoelectric (RTG) and dynamic power conversion systems were analyzed, based on use of a standard isotope (General-purpose heat source, or GPHS) brick. For the radioisotope Stirling power converter configuration designed, the Sage model predicts a thermodynamic power output capacity of 478.1 watts, which slightly exceeds the required 469.1 watts. The hot sink temperature is 1200 C, and the cold sink temperature is 500 C. The required heat input is 1740 watts. This gives a thermodynamic efficiency of 27.48 %. It is estimated that the mechanical efficiency of the power converter design is on the order of 85 %, based on experimental measurements taken from 500-watt power class, laboratory-tested Stirling engines. The overall efficiency is calculated to be 23.36 %. The mass of the power converter is estimated at approximately 21.6 kg

  15. Venus Surface Power and Cooling System Design

    Science.gov (United States)

    Landis, Geoffrey A.; Mellott, Kenneth D.

    2004-01-01

    A radioisotope power and cooling system is designed to provide electrical power for the a probe operating on the surface of Venus. Most foreseeable electronics devices and sensors simply cannot operate at the 450 C ambient surface temperature of Venus. Because the mission duration is substantially long and the use of thermal mass to maintain an operable temperature range is likely impractical, some type of active refrigeration may be required to keep certain components at a temperature below ambient. The fundamental cooling requirements are comprised of the cold sink temperature, the hot sink temperature, and the amount of heat to be removed. In this instance, it is anticipated that electronics would have a nominal operating temperature of 300 C. Due to the highly thermal convective nature of the high-density atmosphere, the hot sink temperature was assumed to be 50 C, which provided a 500 C temperature of the cooler's heat rejecter to the ambient atmosphere. The majority of the heat load on the cooler is from the high temperature ambient surface environment on Venus. Assuming 5 cm radial thickness of ceramic blanket insulation, the ambient heat load was estimated at approximately 77 watts. With an estimated quantity of 10 watts of heat generation from electronics and sensors, and to accommodate some level of uncertainty, the total heat load requirement was rounded up to an even 100 watts. For the radioisotope Stirling power converter configuration designed, the Sage model predicts a thermodynamic power output capacity of 478.1 watts, which slightly exceeds the required 469.1 watts. The hot sink temperature is 1200 C, and the cold sink temperature is 500 C. The required heat input is 1740 watts. This gives a thermodynamic efficiency of 27.48 %. The maximum theoretically obtainable efficiency is 47.52 %. It is estimated that the mechanical efficiency of the power converter design is on the order of 85 %, based on experimental measurements taken from 500 watt power

  16. Lessons Learned from Radiative Transfer Simulations of the Venus Atmosphere

    Science.gov (United States)

    Arney, G.; Meadows, V. S.; Lincowski, A.

    2017-01-01

    The Venus atmosphere is extremely complex, and because of this the spectrum of Earths sister planet is likewise intricate and a challenge to model accurately. However, accurate modeling of Venus spectrum opens up multiple opportunities to better understand the planet next door, and even for understanding Venus-like planets beyond our solar system. Near-infrared (1-2.5 um, NIR) spectral windows observable on the Venus nigthside present the opportunity to probe beneath the Venusian cloud deck and measure thermal emission from the surface and lower atmosphere remotely from Earth or from orbit. These nigthside spectral windows were discovered by Allen and Crawford (1984) and have since been used measure trace gas abundances in the Venus lower atmosphere (less than 45 km), map surface emissivity varisions, and measure properties of the lower cloud deck. These windows sample radiation from below the cloud base at roughly 45 km, and pressures in this region range from roughly Earthlike (approx. 1 bar) up to 90 bars at the surface. Temperatures in this region are high: they range from about 400 K at the base of the cloud deck up to about 740 K at the surface. This high temperature and pressure presents several challenges to modelers attempting radiative transfer simulations of this region of the atmosphere, which we will review. Venus is also important to spectrally model to predict the remote observables of Venus-like exoplanets in anticipation of data from future observatories. Venus-like planets are likely one of the most common types of terrestrial planets and so simulations of them are valuable for planning observatory and detector properties of future telescopes being designed, as well as predicting the types of observations required to characterize them.

  17. The Venus-Earth-Jupiter spin-orbit coupling model

    Science.gov (United States)

    Wilson, I. R. G.

    2013-12-01

    A Venus-Earth-Jupiter spin-orbit coupling model is constructed from a combination of the Venus-Earth-Jupiter tidal-torquing model and the gear effect. The new model produces net tangential torques that act upon the outer convective layers of the Sun with periodicities that match many of the long-term cycles that are found in the 10Be and 14C proxy records of solar activity.

  18. The Venus Emissivity Mapper - Investigating the Atmospheric Structure and Dynamics of Venus' Polar Region

    Science.gov (United States)

    Widemann, T.; Marcq, E.; Tsang, C.; Mueller, N. T.; Kappel, D.; Helbert, J.; Dyar, M. D.; Smrekar, S. E.

    2017-12-01

    Venus' climate evolution is driven by the energy balance of its global cloud layers. Venus displays the best-known case of polar vortices evolving in a fast-rotating atmosphere. Polar vortices are pervasive in the Solar System and may also be present in atmosphere-bearing exoplanets. While much progress has been made since the early suggestion that the Venus clouds are H2O-H2SO4 liquid droplets (Young 1973), several cloud parameters are still poorly constrained, particularly in the lower cloud layer and optically thicker polar regions. The average particle size is constant over most of the planet but increases toward the poles. This indicates that cloud formation processes are different at latitudes greater than 60°, possibly as a result of the different dynamical regimes that exist in the polar vortices (Carlson et al. 1993, Wilson et al. 2008, Barstow et al. 2012). Few wind measurements exist in the polar region due to unfavorable viewing geometry of currently available observations. Cloud-tracking data indicate circumpolar circulation close to solid-body rotation. E-W winds decrease to zero velocity close to the pole. N-S circulation is marginal, with extremely variable morphology and complex vorticity patterns (Sanchez-Lavega et al. 2008, Luz et al. 2011, Garate-Lopez et al. 2013). The Venus Emissivity Mapper (VEM; Helbert et al., 2016) proposed for NASA's Venus Origins Explorer (VOX) and the ESA M5/EnVision orbiters has the capability to better constrain the microphysics (vertical, horizontal, time dependence of particle size distribution, or/and composition) of the lower cloud particles in three spectral bands at 1.195, 1.310 and 1.510 μm at a spatial resolution of 10 km. Circular polar orbit geometry would provide an unprecedented study of both polar regions within the same mission. In addition, VEM's pushbroom method will allow short timescale cloud dynamics to be assessed, as well as local wind speeds, using repeated imagery at 90 minute intervals

  19. The Reappearance of Venus Observed 8 October 2015

    Science.gov (United States)

    Dunham, David W.; Dunham, Joan B.

    2018-01-01

    The reappearance of Venus on October 8, 2015 offered a unique opportunity to attempt observation of the ashen light of Venus as the unlit side of Venus emerged from behind the dark side of the Moon. The dark side of Venus would be offered to observers without interference from the bright side of Venus or of the Moon. Observations were made from Alice Springs, Australia visually with a 20-cm Schmidt-Cassegrain and with a low-light level surveillance camera on a 25-cm reflector. No evidence of the dark side was noted by the visual observer, the video shows little indication of Venus prior to the bright side reappearance. The conclusion reached is that the ashen light, as it was classically defined, is not observable visually or with small telescopes in the visual regime.The presentation describes the prediction, observation technique, and various analyses by the authors and others to draw conclusions from the data.To date, the authors have been unable to locate any reports of others attempting to observe this unique event. That is a pity since, not only was it interesting for an attempt to verify past observations of the ashen light, it was also a visually stunning event.

  20. An Encounter between the Sun and Venus

    CERN Multimedia

    2004-01-01

    The astronomical event of the year will take place on Tuesday, 8 June, when Venus transits across the disk of the sun. In the framework of CERN's 50th anniversary celebrations, the CERN Astronomy Club and the Orion Club invite you to attend their observation of the event on the car park of the Val-Thoiry shopping centre (France) between 7.15 a.m. and 1.30 p.m. Various instruments will be set up in a special tent so that the event can be observed without any risk of damage to the eyes. As the observation of this astronomical event will depend on the weather forecast, confirmation of the above arrangements will be given on the 50th anniversary website the day before.

  1. Nuclear instrumentation in VENUS-F

    Directory of Open Access Journals (Sweden)

    Wagemans J.

    2018-01-01

    Full Text Available VENUS-F is a fast zero power reactor with 30 wt% U fuel and Pb/Bi as a coolant simulator. Depending on the experimental configuration, various neutron spectra (fast, epithermal, and thermal islands are present. This paper gives a review of the nuclear instrumentation that is applied for reactor control and in a large variety of physics experiments. Activation foils and fission chambers are used to measure spatial neutron flux profiles, spectrum indices, reactivity effects (with positive period and compensation method or the MSM method and kinetic parameters (with the Rossi-alpha method. Fission chamber calibrations are performed in the standard irradiation fields of the BR1 reactor (prompt fission neutron spectrum and Maxwellian thermal neutron spectrum.

  2. Nuclear instrumentation in VENUS-F

    Science.gov (United States)

    Wagemans, J.; Borms, L.; Kochetkov, A.; Krása, A.; Van Grieken, C.; Vittiglio, G.

    2018-01-01

    VENUS-F is a fast zero power reactor with 30 wt% U fuel and Pb/Bi as a coolant simulator. Depending on the experimental configuration, various neutron spectra (fast, epithermal, and thermal islands) are present. This paper gives a review of the nuclear instrumentation that is applied for reactor control and in a large variety of physics experiments. Activation foils and fission chambers are used to measure spatial neutron flux profiles, spectrum indices, reactivity effects (with positive period and compensation method or the MSM method) and kinetic parameters (with the Rossi-alpha method). Fission chamber calibrations are performed in the standard irradiation fields of the BR1 reactor (prompt fission neutron spectrum and Maxwellian thermal neutron spectrum).

  3. Transits of Venus and Colonial India

    Science.gov (United States)

    Kochhar, Rajesh

    2012-09-01

    Astronomical expeditions during the colonial period had a political and national significance also. Measuring the earth and mapping the sky were activities worthy of powerful and power- seeking nations. Such was the sanctity of global astronomical activity that many other agendas could be hidden under it. An early astronomy-related expedition turned out to be extremely beneficial, to botany. The expedition sent by the French Government in 1735 to South America under the leadership of Charles Marie de la Condamine (1701--1774) ostensibly for the measurement of an arc of the meridian at Quito in Ecuador surreptitiously collected data that enabled Linnaeus to describe the genus cinchona in 1742. When the pair of transits of Venus occurred in 1761 and 1769, France and England were engaged in a bitter rivalry for control of India. The observation of the transits became a part of the rivalry. A telescope presented by the British to a South Indian King as a decorative toy was borrowed back for actual use. Scientifically the transit observations were a wash out, but the exercise introduced Europe to details of living Indian tradition of eclipse calculations. More significantly, it led to the institutionalization of modern astronomy in India under the auspices of the English East India Company (1787). The transits of Venus of 1874 and 1882 were important not so much for the study of the events as for initiating systematic photography of the Sun. By this, Britain owned most of the world's sunshine, and was expected to help European solar physicists get data from its vast Empire on a regular basis. This and the then genuinely held belief that a study of the sun would help predict failure of monsoons led to the institutionalization of solar physics studies in India (1899). Of course, when the solar physicists learnt that solar activity did not quite determine rainfall in India, they forgot to inform the Government.

  4. Venus Interior Probe Using In-situ Power and Propulsion (VIP-INSPR), Phase I

    Data.gov (United States)

    National Aeronautics and Space Administration — We envision a novel architecture for Venus Interior Probes based on in-situ resources for power generation (VIP-INSPR). Proposed Venus probe is based on the...

  5. Topography of Venus and earth - A test for the presence of plate tectonics

    Science.gov (United States)

    Head, J. W.; Yuter, S. E.; Solomon, S. C.

    1981-01-01

    Comparisons of earth and Venus topography by use of Pioneer/Venus radar altimetry are examined. Approximately 93% of the Venus surface has been mapped with a horizontal resolution of 200 km and a vertical resolution of 200 m. Tectonic troughs have been indicated in plains regions which cover 65% of Venus, and hypsometric comparisons between the two planets' elevation distributions revealed that while the earth has a bimodal height distribution, Venus displays a unimodal configuration, with 60% of the planet surface within 500 m of the modal planet radius. The effects of mapping the earth at the same resolution as the Venus observations were explored. Continents and oceans were apparent, and although folded mountains appeared as high spots, no indications of tectonic activity were discernible. A NASA Venus Orbiting Imaging radar is outlined, which is designed to detect volcanoes, folded mountain ranges, craters, and faults, and thereby allow definition of possible plate-tectonic activity on Venus.

  6. The Creation of a Beneficial Bioshpere from Co2 in the Clouds of Venus

    Science.gov (United States)

    Linaraki, D. L.; Oungrinis, K. A.

    2017-02-01

    This research resulted in an architectural design for a Venus colony based on multiple factors combination, such as psychology of space, predicted near-future technology, and the identified environmental conditions on Venus.

  7. PIONEER 12 VENUS ORBITING RADAR DERIVED RADAR IMAGES V1.0

    Data.gov (United States)

    National Aeronautics and Space Administration — This data set consists of five VICAR2 format images of Venus derived from Pioneer Venus radar altimeter measurements. Data are presented in simple cylindrical...

  8. Cloning, purification, crystallization and preliminary X-ray analysis of a bacterial GABA receptor with a Venus flytrap fold

    International Nuclear Information System (INIS)

    Moréra, Solange; Gueguen-Chaignon, Virginie; Raffoux, Aurélie; Faure, Denis

    2008-01-01

    A 1.35 Å resolution data set was collected from a crystal of the periplasmic GABA receptor Atu2422 from A. tumefaciens. Atu2422 adopts a closed Venus flytrap conformation. In response to infection by the pathogen Agrobacterium tumefaciens, plants synthesize several stress amino acids, including γ-aminobutyric acid (GABA), which modulates the expression of bacterial virulence factors. GABA penetrates into the bacterial cytoplasm via an ABC transporter that is associated with the periplasmic receptor Atu2422. Mature receptor Atu2422 (without its signal peptide) was overexpressed in Escherichia coli, purified and crystallized. A complete data set was collected to 1.35 Å resolution at 100 K. The crystals belonged to the monoclinic space group C2 and contained one molecule in the asymmetric unit. Molecular replacement was performed and the initial electron-density maps revealed a closed form of this Venus flytrap (VFT) receptor, suggesting the presence of an endogenous E. coli ligand

  9. Sulfur dioxide - Episodic injection shows evidence for active Venus volcanism

    Science.gov (United States)

    Esposito, L. W.

    1984-03-01

    Pioneer Venus ultraviolet spectra from the first 5 years of operation show a decline (by more than a factor of 10) in sulfur dioxide abundance at the cloud tops and in the amount of submicron haze above the clouds. At the time of the Pioneer Venus encounter, the values for both parameters greatly exceeded earlier upper limits. However, Venus had a similar appearance in the late 1950's, implying the episodic injection of sulfur dioxide possibly caused by episodic volcanism. The amount of haze in the Venus middle atmosphere is about ten times that found in earth's stratosphere after the most recent major volcanic eruptions, and the thermal energy required for this injection on Venus is greater by about an order of magnitude than the largest of these recent earth eruptions and about as large as the Krakatoa eruption of 1883. The episodic behavior of sulfur dioxide implies that steady-state models of the chemistry and dynamics of cloud-top regions may be of limited use.

  10. Sulfur dioxide: episodic injection shows evidence for active venus volcanism.

    Science.gov (United States)

    Esposito, L W

    1984-03-09

    Pioneer Venus ultraviolet spectra from the first 5 years of operation show a decline (by more than a factor of 10) in sulfur dioxide abundance at the cloud tops and in the amount of submicron haze above the clouds. At the time of the Pioneer Venus encounter, the values for both parameters greatly exceeded earlier upper limits. However, Venus had a similar appearance in the late 1950's, implying the episodic injection of sulfur dioxide possibly caused by episodic volcanism. The amount of haze in the Venus middle atmosphere is about ten times that found in Earth's stratosphere after the most recent major volcanic eruptions, and the thermal energy required for this injection on Venus is greater by about an order of magnitude than the largest of these recent Earth eruptions and about as large as the Krakatoa eruption of 1883. The episodic behavior of sulfur dioxide implies that steady-state models of the chemistry and dynamics of cloud-top regions may be of limited use.

  11. Venus: The First Habitable World of Our Solar System?

    Science.gov (United States)

    Way, Michael Joseph; Del Genio, Anthony; Kiang, Nancy; Sohl, Linda; Clune, Tom; Aleinov, Igor; Kelley, Maxwell

    2015-01-01

    A great deal of effort in the search for life off-Earth in the past 20+ years has focused on Mars via a plethora of space and ground based missions. While there is good evidence that surface liquid water existed on Mars in substantial quantities, it is not clear how long such water existed. Most studies point to this water existing billions of years ago. However,those familiar with the Faint Young Sun hypothesis for Earth will quickly realize that this problem is even more pronounced for Mars. In this context recent simulations have been completed with the GISS 3-D GCM (1) of paleo Venus (approx. 3 billion years ago) when the sun was approx. 25 less luminous than today. A combination of a less luminous Sun and a slow rotation rate reveal that Venus could have had conditions on its surface amenable to surface liquid water. Previous work has also provided bounds on how much water Venus could have had using measured DH ratios. It is possible that less assumptions have to be made to make Venus an early habitable world than have to be made for Mars, even thoughVenus is a much tougher world on which to confirm this hypothesis.

  12. Late Veneer consequences on Venus' long term evolution

    Science.gov (United States)

    Gillmann, C.; Golabek, G.; Tackley, P. J.; Raymond, S. N.

    2017-12-01

    Modelling of Venus' evolution is able to produce scenarios consistent with present-day observation. These results are however heavily dependent on atmosphere escape and initial volatile inventory. This primordial history (the first 500 Myr) is heavily influenced by collisions. We investigate how Late Veneer impacts change the initial state of Venus and their consequences on its coupled mantle/atmosphere evolution. We focus on volatile fluxes: atmospheric escape and mantle degassing. Mantle dynamics is simulated using the StagYY code. Atmosphere escape covers both thermal and non-thermal processes. Surface conditions are calculated with a radiative-convective model. Feedback of the atmosphere on the mantle through surface temperature is included. Large impacts are capable of contributing to atmospheric escape, volatile replenishment and energy transfer. We use the SOVA hydrocode to take into account volatile loss and deposition during a collision. Large impacts are not numerous enough to substantially erode Venus' atmosphere. Single impacts don't have enough eroding power. Swarms of small bodies (lack of plate tectonics and volatile recycling in the interior of Venus, Late Veneer collisions could help explain why Venus seems dry today.

  13. Impacts of the cloud structure's latitudinal variation on the general circulation of the Venus atmosphere as modeled by the LMD-GCM

    Science.gov (United States)

    Garate-Lopez, Itziar; Lebonnois, Sébastien

    2017-04-01

    232, 232-248. Hueso R., Peralta J., Garate-Lopez I., et al., 2015. Six years of Venus winds at the upper cloud level from UV, visible and near infrared observations from VIRTIS on Venus express. Planet. Space Sci. 113-114, 78-99. Lebonnois S., Sugimoto N., and Gilli G., 2016. Wave analysis in the atmosphere of Venus below 100km altitude, simulated by the LMD Venus GCM. Icarus 278, 38-51.

  14. Tectonic evolution of Lavinia Planitia, Venus

    Science.gov (United States)

    Squyres, Steven W.; Frank, Sharon L.; Mcgill, George E.; Solomon, Sean C.

    1991-01-01

    High resolution radar images from the Magellan spacecraft have revealed the first details of the morphology of the Lavinia Planitia region of Venus. Lavinia is a broad lowland over 2000 km across, centered at about 45 deg S latitude, 345 deg E longitude. Herein, the tectonic evolution of Lavinia is discussed, and its possible relationship to processes operating in the planet's interior. The discussion is restricted to the region from 37.3 to 52.6 deg S latitude and from about 340 to 0 deg E longitude. One of the most interesting characteristics of Lavinia is that the entire region possesses a regional tectonic framework of striking regularity. Lavinia is also transected by a complex pattern of belts of intense tectonic deformation known as ridge belts. Despite the gross topographic similarity of all of the ridge belts in Lavinia, they exhibit two rather distinct styles of near surface deformation. One is composed of sets of broad, arch-like ridges rising above the surrounding plains. In the other type, obvious fold-like ridges are rare to absent in the radar images. Both type show evidence for small amounts of shear distributed across the belts.

  15. Doppler Lidar for Wind Measurements on Venus

    Science.gov (United States)

    Singh, Upendra N.; Emmitt, George D.; Yu, Jirong; Kavaya, Michael J.

    2010-01-01

    NASA Langley Research Center has a long history of developing 2-micron laser transmitter for wind sensing. With support from NASA Laser Risk Reduction Program (LRRP) and Instrument Incubator Program (IIP), NASA Langley Research Center has developed a state-of-the-art compact lidar transceiver for a pulsed coherent Doppler lidar system for wind measurement. The transmitter portion of the transceiver employs the high-pulse-energy, Ho:Tm:LuLiF, partially conductively cooled laser technology developed at NASA Langley. The transceiver is capable of 250 mJ pulses at 10 Hz. It is very similar to the technology envisioned for coherent Doppler lidar wind measurements from Earth and Mars orbit. The transceiver is coupled to the large optics and data acquisition system in the NASA Langley VALIDAR mobile trailer. The large optics consists of a 15-cm off-axis beam expanding telescope, and a full-hemispheric scanner. Vertical and horizontal vector winds are measured, as well as relative backscatter. The data acquisition system employs frequency domain velocity estimation and pulse accumulation. It permits real-time display of the processed winds and archival of all data. This lidar system was recently deployed at Howard University facility in Beltsville, Mary-land, along with other wind lidar systems. Coherent Doppler wind lidar ground-based wind measurements and comparisons with other sensors will be presented. A simulation and data product for wind measurement at Venus will be presented.

  16. Variability of dayside electron temperature at Venus

    Science.gov (United States)

    Mahajan, K. K.; Ghosh, S.; Paul, R.; Hoegy, W. R.

    1994-01-01

    Langmuir probe measurements on Pioneer Venus Orbiter show that electron temperature (Te) profiles exhibit two distinct regions. The lower, but more extended region is in the main ionosphere where Te increases slowly with altitude. The other, less extended region is in the ionopause, where Te rise sharply with altitude. If horizontal magnetic fields and flux ropes in the ionosphere inhibit vertical thermal conductivity sufficiently, then the observed Te profile could be explained with EUV as the major heat source (Cravens et al., 1980). The rise in Te in the ionopause region has generally been attributed to solar wind heating (Brace and Kliore, 1991). We suggest that this sharp rise in Te is due primarily to the steep fall in electron density, Ne. If the heating rate is essentially unchanged and heat conduction is not of primary importance, then a steep rise in Te will maintain a constant electron cooling rate for a steeply falling Ne. We have observed large orbit to orbit variations in Te in the ionopause region which are found to be inversely related to changes in Ne. Variations in solar wind dynamic pressure do not seem to have a direct effect on Te, rather the effect is indirect coming through the sharp decrease in Ne.

  17. Departmental Appeals Board Decisions

    Data.gov (United States)

    U.S. Department of Health & Human Services — Decisions issued by the Chair and Board Members of the Departmental Appeals Board concerning determinations in discretionary, project grant programs, including...

  18. Pilot Boarding Areas

    Data.gov (United States)

    National Oceanic and Atmospheric Administration, Department of Commerce — Pilot boarding areas are locations at sea where pilots familiar with local waters board incoming vessels to navigate their passage to a destination port. Pilotage is...

  19. Poludnista Dorsa, Venus: History and context of a deformation belt

    Science.gov (United States)

    Young, D. A.; Hansen, V. L.

    2005-03-01

    Rolling lowlands comprise 80% of Venus's surface, and thus developing a geological understating of resurfacing and tectonism is critical for our understanding of Venus' evolution. In this paper, global, regional, and local approaches to interpreting Magellan synthetic aperture radar and altimetry radar data are used to constrain modes of lowland evolution, convection processes, and lithospheric structure. Detailed geologic mapping is combined with altimetry data test models of deformation belt evolution in Venus's lowlands. Poludnista Dorsa, a complex 2000-km-long deformation belt, is highly segmented and broadly time transgressive. Long-wavelength deformation is spatially independent of local short-wavelength deformation within the deformation belt and temporally predates regional deformation marked by wrinkle ridges. A mechanically layered lithosphere of regional extent is not required by the local geologic history; local lithospheric thinning or progressive regional thickening of the mechanical layer better explains the observed sequence of events.

  20. Impact-induced atmospheres and oceans on earth and Venus

    Science.gov (United States)

    Matsui, T.; Abe, Y.

    1986-01-01

    The effects of planetesimal-impact induced atmosphere formation on the earth and Venus are modeled to gain an indication why the two planets, at relatively equal distances from the sun, evolved so differently. Both planets gained approximately 10 to the 21 kg of water from the impacts. The water mass of the accreting planetesimals would have remained, initially, as a hot atmosphere. A two-stream approximation is defined for the temperature profile of a plane parallel atmosphere in radiative equilibrium. It is shown that the Venus atmosphere did not, as happened on earth, condense into a hot ocean after the impact epoch. Instead, the greenhouse effect caused the Venus equilibrium thermal structure to remain higher than the vapor pressure, keepinig the atmosphere in a vapor phase until the vapor dissociated and H2 atoms eventually escaped into space.

  1. Reorientation Histories of Mercury, Venus, the Moon, and Mars

    Science.gov (United States)

    Keane, J. T.; Matsuyama, I.

    2017-09-01

    The spins of planets are not constant with time. Impacts, volcanos, and other large geologic features can reorient planets (a process known as true polar wander). True polar wander can have important implications for the climate, volatiles, and tectonics of planets and moons. However, despite its importance, it has been difficult to study true polar wander for objects beyond the Earth. Here we present the results of the first comprehensive, data-driven investigation into the true polar wander histories of Mercury, Venus, the Moon, and Mars. We find that Mercury and the Moon have both reoriented in response to large impacts, while the spins of Mars and Venus are more strongly affected by volcanism. Venus, in particular, has been subject to some very dramatic episodes of true polar wander in the past.

  2. Venus Aerosol Properties from Modelling and Akatsuki IR2 Observations

    Science.gov (United States)

    McGouldrick, K.

    2017-09-01

    I am creating computer simulations of the clouds of Venus. In these simulations, I make changes to the properties of the aerosols that affect their ability to form, grow, evaporate, or combine with other particles. I then use the results of these models to predict how bright or dark Venus might appear when viewed at infrared wavelengths. By comparing this calculated brightness with the infrared observations made by the IR2 infrared camera on the Akatsuki spacecraft (currently orbiting Venus since its arrival in December 2015, built by the Japan Aerospace Exploration Agency (JAXA)), I hope to explain the causes for the changes that are seen to occur in the clouds via these and other images.

  3. Earth's Atmospheric Electricity Parameter Response During Venus Transit

    Directory of Open Access Journals (Sweden)

    Syam Sundar De

    2015-01-01

    Full Text Available Venus transited across the Sun on 06 June 2012, introducing significant contribution to the tidal characteristics of the solar atmosphere. _ atmosphere was perturbed due to an anomalous Coronal Mass Ejection (CME and γ-radiationγ-radiation influenced by the solar tide due to Venus transit, thereby the Earth-ionosphere waveguide characteristics were changed. In this anomalous situation we measured some atmospheric electricity parameters such as Schumann resonance (SR amplitude, very low frequency (VLF sferics, subionospheric transmitted signals and the point discharge current (PDC along with the vertical electrical potential gradient (PG at the ground surface on the day of transit. The results showed some remarkable variations during the transit as well as pre- and post-transit periods. The observed anomalies in the recorded data were interpreted in terms of the anomalous solar tidal effects initiated due to Venus transit.

  4. Terrestrial subaqueous seafloor dunes: Possible analogs for Venus

    Science.gov (United States)

    Neakrase, Lynn D. V.; Klose, Martina; Titus, Timothy N.

    2017-06-01

    Dunes on Venus, first discovered with Magellan Synthetic Aperture Radar (SAR) in the early 1990s, have fueled discussions about the viability of Venusian dunes and aeolian grain transport. Confined to two locations on Venus, the existence of the interpreted dunes provides evidence that there could be transportable material being mobilized into aeolian bedforms at the surface. However, because of the high-pressure high-temperature surface conditions, laboratory analog studies are difficult to conduct and results are difficult to extrapolate to full-sized, aeolian bedforms. Field sites of desert dunes, which are well-studied on Earth and Mars, are not analogous to what is observed on Venus because of the differences in the fluid environments. One potentially underexplored possibility in planetary science for Venus-analog dune fields could be subaqueous, seafloor dune fields on Earth. Known to the marine geology communities since the early 1960s, seafloor dunes are rarely cited in planetary aeolian bedform literature, but could provide a necessary thick-atmosphere extension to the classically studied aeolian dune environment literature for thinner atmospheres. Through discussion of the similarity of the two environments, and examples of dunes and ripples cited in marine literature, we provide evidence that subaqueous seafloor dunes could serve as analogs for dunes on Venus. Furthermore, the evidence presented here demonstrates the usefulness of the marine literature for thick-atmosphere planetary environments and potentially for upcoming habitable worlds and oceanic environment research program opportunities. Such useful cross-disciplinary discussion of dune environments is applicable to many planetary environments (Earth, Mars, Venus, Titan, etc.) and potential future missions.

  5. Cupid's Arrow: An Innovative Nanosat to Sample Venus' Upper Atmosphere

    Science.gov (United States)

    Bienstock, Bernie; Darrach, Murray; Madzunkov, Stojan; Sotin, Christophe

    2016-01-01

    In NASA's Discovery 2014 AO, the opportunity to propose a Technology Demonstration Opportunity (TDO) to enhance the primary mission was specified. For the Venus Emissivity, Radio Science, InSAR, Topography, and Spectroscopy (VERITAS) mission, we elected to include the Cupid's Arrow nanosat TDO to sample and measure the abundances of noble gases and their isotopic ratios in Venus's upper atmosphere below the homopause. This paper will provide a basic overview of the VERITAS mission, with a focus on the Cupid's Arrow concept including a description of the mission, spacecraft design, and JPL's quadrupole ion trap mass spectrometer (QITMS) instrument specifications and design. In previous planetary entry probe mission designs, particularly at Venus, engineers w ere focused on entry and descent. A landed probe was also proposed for the New Frontiers SAGE mission. For Cupid's Arrow, the nanosat is designed to skim through the upper atmosphere, just below the homopause, in order to sample the atmosphere, perform the analysis, and then exit the atmosphere to transmit its data to the orbiting VERITAS spacecraft. Cupid's Arrow is a compelling addition to the VERITAS geology mission. A key missing link in our understanding of Venus' evolution is the noble gas abundances and their isotopic ratios. Not since Pioneer Venus have these measurements been made in the Venus atmosphere and never in the upper atmosphere, just below the homopause, to the degree of accuracy that will be accomplished by VERITAS' Cupid's Arrow nanosat.Such measurements were ranked as the number 1 investigation of the number 1 objective of the goal "Atmospheric Formation, Evolution, and Climate History ".

  6. Possible Signs of Fauna and Flora on Venus

    Science.gov (United States)

    Ksanfomality, Leonid V.; Selivanov, Arnold S.; Gektin, Yuryi M.

    2015-08-01

    Habitability of planets is a fundamental question of science. Some of exoplanets possess physical conditions close to those of Venus. The planet Venus, despite its dense and hot (735 K) oxygen-free atmosphere of CO2, having a high pressure of 9.2 MPa at the surface, can be a natural laboratory for this kind of studies. The only existing data on the planet’s surface are still the results obtained by the Soviet VENERA landers.The TV experiments of Venera-9 and 10 (October, 1975) and Venera-13 and 14 (March, 1982) delivered 41 panoramas of Venus surface (or their fragments). The experiments were of extreme technical complexity. There have not been any similar missions to Venus in the subsequent 40 and 33 years. In the absence of new landing missions to Venus, the VENERA panoramas have been re-processed by modern means. The results of these missions are studied anew. A dozen of relatively large objects, from a decimeter to half a meter in size, with an unusual morphology have been found which moved very slowly or changed slightly their shape. Certain unusual findings that have a structure similar to the Earth’ fauna and flora were found in different areas of the planet. There are more then 30 papers on the topic published in 2012-2014 (e.g., “Acta Astronautica”, 2014, V. 105, pp. 521-533). Due to the availability of up to eight duplicates of the images obtained and their low level of masking noise, the VENERA archive panoramas permit identifying and exploring some types of hypothetical life forms of Venus. Analysis of treated once again VENERA panoramic images revealed objects that might indicate the presence of about 12 hypothetical forms of Venusian flora and fauna. Among them is ‘amisada’ that stands out with its unusual lizard shape against the stone plates surrounding it.

  7. Scrum Board Game

    Science.gov (United States)

    van den Oord, Stefan; van de Goor, Wim

    The Scrum Board Game is a workshop for beginners. It is for people with any role (customer, developer, tester, etc.), who don’t exactly know what a Scrum Board is, or how to create one themselves. The workshop teaches the benefits of a Scrum Board, how to use it, and how to introduce it in projects.

  8. Contrasts in near-IR images of the Venus clouds (VMC/VEx) and their probable causes

    Science.gov (United States)

    Shalygina, O. S.; Petrova, E. V.; Markiewicz, W. J.

    2017-09-01

    Contrasts in near-IR images of the Venus clouds (Venus Monitoring Camera VMC/Venus Express) and their probable causes were studied. The comparison of the measured phase profiles to the single-scattering phase functions of particles with different sizes and refractive indices and the phase profiles of clouds modeled with the radiative-transfer code has shown that in most cases, the sizes of particles in the NIR-dark and NIR-bright features are the same; in the NIR images (as well as in the visible ones) the higher brightness may be caused by a higher refractive index of particles in the clouds or/and the higher optical depth of the clouds; the effect of the higher refractive index on the UV profiles is opposite due to absorption; the presence of small submicron particles in the clouds and, especially, above them produces a considerable effect on brightness in UV and visible, while its influence on the NIR brightness is very weak.

  9. High Altitude Venus Operations Concept Trajectory Design, Modeling and Simulation

    Science.gov (United States)

    Lugo, Rafael A.; Ozoroski, Thomas A.; Van Norman, John W.; Arney, Dale C.; Dec, John A.; Jones, Christopher A.; Zumwalt, Carlie H.

    2015-01-01

    A trajectory design and analysis that describes aerocapture, entry, descent, and inflation of manned and unmanned High Altitude Venus Operation Concept (HAVOC) lighter-than-air missions is presented. Mission motivation, concept of operations, and notional entry vehicle designs are presented. The initial trajectory design space is analyzed and discussed before investigating specific trajectories that are deemed representative of a feasible Venus mission. Under the project assumptions, while the high-mass crewed mission will require further research into aerodynamic decelerator technology, it was determined that the unmanned robotic mission is feasible using current technology.

  10. Board of Directors or Supervisory Board

    DEFF Research Database (Denmark)

    Werlauff, Erik

    2009-01-01

    The article analyses the legal consequences of the choice now available to Danish public limited companies, which can now opt for a two-tier management structure, in which the management board undertakes both the day-to-day and the overall management, while a supervisory board exercises control...... over the management board, including its appointment and dismissal. The article considers which companies a two-tier structure may be relevant for, and reviews the consequences for the composition, election and functioning of the company organs....

  11. Expression

    Directory of Open Access Journals (Sweden)

    Wang-Xia Wang

    2014-02-01

    Full Text Available The miR-15/107 family comprises a group of 10 paralogous microRNAs (miRNAs, sharing a 5′ AGCAGC sequence. These miRNAs have overlapping targets. In order to characterize the expression of miR-15/107 family miRNAs, we employed customized TaqMan Low-Density micro-fluid PCR-array to investigate the expression of miR-15/107 family members, and other selected miRNAs, in 11 human tissues obtained at autopsy including the cerebral cortex, frontal cortex, primary visual cortex, thalamus, heart, lung, liver, kidney, spleen, stomach and skeletal muscle. miR-103, miR-195 and miR-497 were expressed at similar levels across various tissues, whereas miR-107 is enriched in brain samples. We also examined the expression patterns of evolutionarily conserved miR-15/107 miRNAs in three distinct primary rat brain cell preparations (enriched for cortical neurons, astrocytes and microglia, respectively. In primary cultures of rat brain cells, several members of the miR-15/107 family are enriched in neurons compared to other cell types in the central nervous system (CNS. In addition to mature miRNAs, we also examined the expression of precursors (pri-miRNAs. Our data suggested a generally poor correlation between the expression of mature miRNAs and their precursors. In summary, we provide a detailed study of the tissue and cell type-specific expression profile of this highly expressed and phylogenetically conserved family of miRNA genes.

  12. Whistler mode waves from lightning on Venus: Magnetic control of ionospheric access

    Science.gov (United States)

    Russell, C. T.; Zhang, T. L.; Wei, H. Y.

    2008-09-01

    The fluxgate magnetometer on Venus Express samples the magnetic field near periapsis at 128 Hz. Bursts of plane-polarized magnetic waves in the vicinity of 100 Hz are observed propagating at small angles to the magnetic field. The magnetic field is generally horizontal in the region around periapsis, located at high northern latitudes. When the magnetic field remains within 15° of horizontal during the 2-min periapsis pass, no such waves are observed; but when there are brief periods during which the local magnetic field dips into the atmosphere by more than 15°, the bursts begin to appear. Such radial excursions of the magnetic field occur 25% of the time in the region around periapsis. The bursts are seen only on passes with these excursions. We interpret this magnetic control in terms of the coupling between the electromagnetic wave from lightning discharges refracted vertically by the increasing electron density and the nearly horizontal ionospheric magnetic field along which the energy is guided to the spacecraft. The inferred rate of electric discharges in the Venus atmosphere is about 20% of that seen in the Earth's atmosphere.

  13. Variations in Near-Infrared Emissivity of Venus Surface Observed by the Galileo Near-Infrared Mapping Spectrometer

    Science.gov (United States)

    Hashimoto, G. L.; Roos-Serote, M.; Sugita, S.

    2004-11-01

    We evaluate the spatial variation of venusian surface emissivity at a near-infrared wavelength using multispectral images obtained by the Near-Infrared Mapping Spectrometer (NIMS) on board the Galileo spacecraft. The Galileo made a close flyby to Venus in February 1990. During this flyby, NIMS observed the nightside of Venus with 17 spectral channels, which includes the well-known spectral windows at 1.18, 1.74, and 2.3 μ m. The surface emissivity is evaluated at 1.18 μ m, at which thermal radiation emitted from the planetary surface could be detected. To analyze the NIMS observations, synthetic spectra have been generated by means of a line-by-line radiative transfer program which includes both scattering and absorption. We used the discrete ordinate method to calculate the spectra of vertically inhomogeneous plane-parallel atmosphere. Gas opacity is calculated based on the method of Pollack et al. (1993), though binary absorption coefficients for continuum opacity are adjusted to achieve an acceptable fit to the NIMS data. We used Mie scattering theory and a cloud model developed by Pollack et al. (1993) to determine the single scattering albedo and scattering phase function of the cloud particles. The vertical temperature profile of Venus International Reference Atmosphere (VIRA) is used in all our calculations. The procedure of the analysis is the followings. We first made a correction for emission angle. Then, a modulation of emission by the cloud opacities is removed using simultaneously measured 1.74 and 2.3 μ m radiances. The resulting images are correlated with the topographic map of Magellan. To search for variations in surface emissivity, this cloud corrected images are divided by synthetic radiance maps that were created from the Magellan data. This work has been supported by The 21st Century COE Program of Origin and Evolution of Planetary Systems of Ministry of Education, Culture, Sports, Science and Technology (MEXT).

  14. Aerobraking at Venus: A science and technology enabler

    Science.gov (United States)

    Hibbard, Kenneth; Glaze, Lori; Prince, Jill

    2012-04-01

    Venus remains one of the great unexplored planets in our solar system, with key questions remaining on the evolution of its atmosphere and climate, its volatile cycles, and the thermal and magmatic evolution of its surface. One potential approach toward answering these questions is to fly a reconnaissance mission that uses a multi-mode radar in a near-circular, low-altitude orbit of ∼400 km and 60-70° inclination. This type of mission profile results in a total mission delta-V of ∼4.4 km/s. Aerobraking could provide a significant portion, potentially up to half, of this energy transfer, thereby permitting more mass to be allocated to the spacecraft and science payload or facilitating the use of smaller, cheaper launch vehicles.Aerobraking at Venus also provides additional science benefits through the measurement of upper atmospheric density (recovered from accelerometer data) and temperature values, especially near the terminator where temperature changes are abrupt and constant pressure levels drop dramatically in altitude from day to night.Scientifically rich, Venus is also an ideal location for implementing aerobraking techniques. Its thick lower atmosphere and slow planet rotation result in relatively more predictable atmospheric densities than Mars. The upper atmosphere (aerobraking altitudes) of Venus has a density variation of 8% compared to Mars' 30% variability. In general, most aerobraking missions try to minimize the duration of the aerobraking phase to keep costs down. These short phases have limited margin to account for contingencies. It is the stable and predictive nature of Venus' atmosphere that provides safer aerobraking opportunities.The nature of aerobraking at Venus provides ideal opportunities to demonstrate aerobraking enhancements and techniques yet to be used at Mars, such as flying a temperature corridor (versus a heat-rate corridor) and using a thermal-response surface algorithm and autonomous aerobraking, shifting many daily ground

  15. An Exo-Venus in the Solar Neighborhood

    Science.gov (United States)

    Kohler, Susanna

    2017-04-01

    A size comparison of Venus and Earth. Though they are nearly the same size and density, these two planets evolved very differently. [NASA]Earth is great place for life but Venus definitely isnt. Both planets have similar masses and densities. So why did one evolve to support life, while the other turned into a barren and inhospitable hothouse? This is a question we might be able to answer if we can gather observations of other planets similar to Earth and Venus. The recent discovery of an exo-Venus in our solar neighborhood brings us one step closer to thisgoal!A New NeighborA team of scientists led by Isabel Angelo (SETI Institute, NASA Ames Research Center, and UC Berkeley) has announced the discovery of Kepler-1649b, an exoplanet transiting a star located just 219 light-years away from us. Kepler-1649b is unique in being roughly the same size as Earth and Venus and also receiving a similar amount of starlight as Venus does from our Sun.Phase-folded light curve showing the transit of Kepler-1649b. [Angelo et al. 2017]Angelo and collaborators conducted follow-up observations after Keplers detection of 1649b to verify its planetary nature and pin down its properties. They found that Kepler-1649b has a radius of 1.08 times that of Earth, and it receives an incident flux of 2.3 times Earths which is very similar to the incident flux received by Venus. Kepler-1649b orbits a star thats only a quarter of our Suns radius, however, and it therefore orbits significantly closer to its star in order to receive the same flux, circling its host once every 8.7 days.Differences Due to a Small HostIts worth identifying howthis planet might differ from Venus. The authors suggest a few key factors:Kepler-1649b may be more prone to effects of host-star variability. M-dwarf stars like this one are typically more magnetically active than our Sun, and Kepler-1649b is orbiting very close to its star.Kepler-1649b receives comparatively low-energy radiation, compared to Venus. This is

  16. How did Earth not End up like Venus?

    Science.gov (United States)

    Jellinek, M.; Lenardic, A.; Weller, M. B.

    2017-12-01

    Recent geodynamic calculations show that terrestrial planets forming with a chondritic initial bulk composition at order 1 AU can evolve to be either "Earth-like" or "Venus-like": Both mobile- and stagnant-lid tectonic regimes are permitted, neither solution is an explicitly stronger attractor and effects related to differences in Sun-Earth distance are irrelevant. What factors might then cause the thermal evolutionary paths of Earth and Venus to diverge dynamically at early times? At what point in Earth's evolution did plate tectonics emerge and when and how did this tectonic mode gain sufficient resilience to persist over much of Earth's evolution? What is the role of volatile cycling and climate: To what extent have the stable climate of Earth and the greenhouse runaway climate of Venus enforced their distinct tectonic regimes over time? In this talk I will explore some of the mechanisms potentially governing the evolutionary divergence of Earth and Venus. I will first review observational constraints that suggest that Earth's entry into the current stable plate tectonic mode was far from assured by 2 Ga. Next I will discuss how models have been used to build understanding of some key dynamical controls. In particular, the probability of "Earth-like" solutions is affected by: 1) small differences in the initial concentrations of heat producing elements (i.e., planetary initial conditions); 2) long-term climate change; and 3) the character of a planet's early evolutionary path (i.e., tectonic hysteresis).

  17. Technology development for long-lived Venus landers.

    Science.gov (United States)

    Ekonomov, 1.; Korablev, O.; Zasova, L.

    2007-08-01

    Simultaneously with many successful lander missions on Venus in 1972-1985 Soviet Union began develop long-lived lander on surface of Venus. The basic problem were extreme conditions on a surface: P=10MPa, T=500 C . Then operations have been stopped and have renewed in 2006 already in new Russia. Mission "VENERA (VENUS) - D" is included into the Federal space program of Russia on 2006 - 2015 with launch in 2016. To this date Russia alone can't create a reliable electronics for 500 C, but we have got examples GaN electronics for 350 C. Cooling technology with boiling water is offered for interior devices of lander at pressure 10 MPa and temperature 310 C. As the power source of an electronics we use high-temperature galvanic cells on the base of Li4Si [LiCl, KCl, LiF] FeS2 which are released in Russia as reserve power sources. They are capable to work directly on a surface of Venus without any thermal protection. At lander two kinds of vacuum technology can be used: 1) in multilayer (MLI ) thermal blanket for lander, 2) in electro-vacuum devices, for example transmitter . For creation and maintenance of vacuum at temperature 400-500 C: chemical gas absorbers ( getter materials ) are used, they actively absorb both carbon dioxide and nitrogen .

  18. Venus Transit 2004, A New Experiment For Education And Communication

    Science.gov (United States)

    Stavinschi, M.; Mioc, V.; Maris, G.

    On June 8, 2004, the Venus transit in front of the Sun took place. It was a rare astronomical phenomenon, because the last Venus transit took place in 1882 and was only partially visible in Europe. Such a rare phenomenon mobilized all who are curious about the sky, but it also was a good opportunity for specialists to spread some knowledge about the universe in public. IAAR adhered to the International Consortium Venus-2004 acting as a National Node. The Romanian researchers in astronomy, together with the amateur astronomers and teachers, set up an ambitious national programme addressed to the school young people as well as to the public. National meetings and conferences, activities for informing the public, contests with astronomical subjects for children were organised in order to make known the Venus transit event. Organisms with large impact on the public (mass media) and even factors of decision were contacted in order to get a correct understanding of the phenomenon. We try to show here how a such a event become a new experiment for education and communication, ending with some particular conclusions.

  19. Ribbon terrain formation and implications for lithosphere evolution, Venus

    Science.gov (United States)

    Hansen, V. L.; Willis, J. J.

    1997-03-01

    Venus terrain ribbons comprise a fabric of alternating, parallel, closely-spaced, radar-dark/bright lineaments showing a distinct dark-bright pairing. It is presently argued that the opening of tensile fractures within a brittle layer above a sharp brittle ductile transition over a ductile substrate can account for the formation of the observed geometric characteristics of ribbon terrain.

  20. Results of Equilibrium Resurfacing Monta Carlo Models on Venus

    Science.gov (United States)

    Bjonnes, E. E.; Hansen, V. L.; Swenson, J. B.

    2008-03-01

    Previous equilibrium resurfacing tests failed to include increments between 10 and 0.03%. We tested this parameter space and found that there is no statistical evidence that equilibrium resurfacing cannot meet the two key observations of Venus' impact crater data set.

  1. The transit of Venus enterprise in Victorian Britain

    CERN Document Server

    Ratcliff, Jessica

    2008-01-01

    In nineteenth century, the British Government spent money measuring the distance between the earth and the sun using observations of the transit of Venus. This book presents a narrative of the two Victorian transit programmes. It draws out their cultural significance and explores the nature of 'big science' in late-Victorian Britain.

  2. Plant Physiology: The Venus Flytrap Counts on Secretion.

    Science.gov (United States)

    Brownlee, Colin

    2017-08-07

    The Venus flytrap effectively detects, traps, digests and absorbs insect prey. A recent study links the mechanical stimulation of sensory hair cells with short- and long-term signalling giving rise to different downstream secretion events that bring about conditions for prey digestion. Copyright © 2017 Elsevier Ltd. All rights reserved.

  3. Transit of Venus: Quantitative Observing with Simple Equipment

    Indian Academy of Sciences (India)

    Home; Journals; Resonance – Journal of Science Education; Volume 17; Issue 5. Transit of Venus: Quantitative Observing with Simple Equipment. N Rathnasree Pritpal Kaur. Classroom Volume 17 Issue 5 May 2012 pp 497-504. Fulltext. Click here to view fulltext PDF. Permanent link:

  4. Cleopatra Crater, a Circular Portal to the Soul of Venus

    Science.gov (United States)

    Herrick, R. R.

    2014-05-01

    Cleopatra is on the flanks of Maxwell Montes, the tallest mountain range on Venus. Inside the peak ring is a 60-km wide, flat area that represents a relatively safe area to obtain a sample of tessera, plus the geology of the area is important.

  5. Venus näitas lillekleite / Regina Hansen

    Index Scriptorium Estoniae

    Hansen, Regina

    2001-01-01

    Sunflower Beauty Contest esitles ööklubis Venus eluslilledest valmistatud kleite. Parimaks tunnistati kaupluse Annilill floristid tööga "My Bunny", teiseks tunnistati Katrin Pedaru ja Ninell Soosaare "C'est la vie", kolmanda koha pälvis Karina Saberi töö "Unistus"

  6. The 1761 discovery of Venus' atmosphere: Lomonosov and others

    Science.gov (United States)

    Shiltsev, Vladimir

    2014-03-01

    Russian polymath Mikhail Vasil'evich Lomonosov claimed to have discovered the atmosphere of Venus during the planet's transit over the Sun's disc in 1761. Although several other astronomers observed similar effects during the 1761 and 1769 transits, Lomonosov's claim for priority is the strongest as he was the first to publish a comprehensive scientific report, and the first to offer a detailed explanation of the aureole around Venus at ingress and egress, which was caused by refraction of the sunlight through Venus' atmosphere. His observations, moreover, were successfully reconstructed experimentally using antique telescopes during the 2012 transit. In this paper we review details of Lomonosov's observations (which usually are poorly covered by commentators and often misunderstood); compare other reports of the eighteenth century transit observations, and summarize their findings in a comprehensive table; and address recent calls to reconsider Lomonosov's priority. After reviewing the available documentation we conclude that everything we learned before, during and after the twenty-first century transits only supports further the widely-accepted attribution of the discovery of Venus' atmosphere to Lomonosov.

  7. Transit of Venus: Quantitative Observing with Simple Equipment The ...

    Indian Academy of Sciences (India)

    a graph sheet and counting the millimeter squares. Better analysis becomes possible, of course, through the usage of software like. MATLAB or any other software that would allow processing the images of the Sun to determine the fractional area of the sunspot. (or Venus or Mercury during transit) occupied on the projected.

  8. Simulation of Venus Atmosphere Dynamics With an Earth Climate GCM

    Science.gov (United States)

    Parish, H. F.; Schubert, G.; Covey, C. C.; Grossman, A.

    2008-12-01

    We describe the results of initial simulations of the Venusian atmosphere, using the Community Atmosphere Model (CAM). The CAM model is a descendant of the NCAR Community Climate Model, and is defined as one of two "high-end" models designated by the US Climate Change Science Program for basic research. It may also be the most widely used 3D climate model in the US. CAM has grown substantially in complexity and Earth-specificity since the original version was released in 1983, and many of these Earth based physics parameterizations need to be adjusted to simulate the Venus atmosphere. Other groups are adapting CAM to simulate the atmospheres of Mars and Titan, thereby promising CAM simulation for all four terrestrial planets known to have substantial atmospheres. Studying these worlds together will provide calibration of Earth-centric studies of climate changes like global warming. It will also provide context for future searches for Earth-like planets orbiting other stars. In this work we will focus on Venus. The Venus atmosphere represents an extreme environment, strongly influenced by the greenhouse effect, and studying the Venus atmosphere may therefore be relevant to the possible future direction of the Earth's climate. The dynamical processes which occur in the Venusian atmosphere are not well understood, including the cause of the strong superrotation of the atmosphere, in which the planetary surface rotates with a period of around 243 days, but the atmosphere near the cloud tops has a rotational period of only around 4 days. We show the results of initial simulations of the dynamics of the Venus atmosphere, using a version of the CAM model with most of the Earth related processes, such as the cloud physics, removed. A simplified form of heating has been applied, similar to the thermal forcing approach used recently by other authors. We investigate the sensitivity of the model results to changes in the physics parameterizations we have used, including

  9. Geologic map of the Ganiki Planitia quadrangle (V-14), Venus

    Science.gov (United States)

    Grosfils, Eric B.; Long, Sylvan M.; Venechuk, Elizabeth M.; Hurwitz, Debra M.; Richards, Joseph W.; Drury, Dorothy E.; Hardin, Johanna

    2011-01-01

    Vinmara Planitia), a geologic map of the region may yield insight into a wide array of important problems in Venusian geology. The current mapping effort and analysis complements previous efforts to characterize aspects of the region’s geology, for example stratigraphy near parabolic halo crater sites, volcanic plains emplacement, wrinkle ridges, volcanic feature distribution, volcano deformation, coronae characteristics, lithospheric flexure, and various features along a 30±7.58° N. geotraverse. Our current research focuses on addressing four specific questions. Has the dominant style of volcanic expression within the quadrangle varied in a systematic fashion over time? Does the tectonic deformation within the quadrangle record significant regional patterns that vary spatially or temporally, and if so what are the scales, orientations and sources of the stress fields driving this deformation? If mantle upwelling and downwelling have played a significant role in the formation of Atla Regio and Atalanta Planitia as has been proposed, does the geology of Ganiki Planitia record evidence of northwest-directed lateral mantle flow connecting the two sites? Finally, can integration of the tectonic and volcanic histories preserved within the quadrangle help constrain competing resurfacing models for Venus?

  10. Search for HBr and bromine photochemistry on Venus

    Science.gov (United States)

    Krasnopolsky, Vladimir A.; Belyaev, Denis A.

    2017-09-01

    HBr (1-0) R2 2605.8/6.2 cm-1, the strongest line of the strongest band of HBr, was observed when searching for this species on Venus. The observation was conducted using the NASA IRTF and a high-resolution long-slit spectrograph CSHELL with resolving power of 4 × 104. 101 spectra of Venus were analyzed, and the retrieved HBr abundances varied from -8 to + 5 ppb. Their mean value is -1.2 ppb, standard deviation is 2.5 ppb, and uncertainty of the mean is 0.25 ppb. The negative value presumes a systematic error, and the estimated upper limit of the HBr mixing ratio at the cloud tops of Venus is ∼1 ppb. From the simultaneously retrieved CO2 abundances, this corresponds to an altitude of 78 km for the uniform distribution of HBr. A simplified version of the bromine photochemistry is included into the photochemical model (Krasnopolsky 2012, Icarus 218, 230-246). Photolysis of HBr and its reactions with O and H deplete the HBr mixing ratio at 70-80 km relative to that below 60 km by a factor of ≈300. Reanalysis of the observational data with the calculated profile of HBr gives an upper limit of 20-70 ppb for HBr below 60 km and the aerosol optical depth of 0.7 at 70 km and 3.84 μm. The bromine chemistry may be effective on Venus even under the observed upper limit. However, if a Cl/Br ratio in the Venus atmosphere is similar to that in the Solar System, then HBr is ≈1 ppb in the lower atmosphere and the bromine chemistry is insignificant. Thermodynamic calculations based on the chemical kinetic model (Krasnopolsky 2013, Icarus 225, 570-580) predict HBr as a major bromine species in the lower atmosphere.

  11. New perspectives on the accretion and internal evolution of Venus

    Science.gov (United States)

    O'Rourke, J. G.

    2017-12-01

    Dichotomous conditions on Earth and Venus present one of the most compelling mysteries in our Solar System. Ongoing debate centers on how the internal dynamics of Venus have shaped its atmospheric composition, surface features, and even habitability over geologic time. In particular, Venus may have resembled Earth for billions of years before suffering catastrophic transformation, or perhaps some accretionary process set these twin planets on divergent paths from the beginning. Unfortunately, the limited quality of decades-old data—particularly the low resolution of radar imagery and global topography from NASA's Magellan mission—harms our ability to draw definite conclusions. But some progress is possible given recent advances in modeling techniques and improved topography derived from stereo images that are available for roughly twenty percent of the surface. Here I present simulations of the interior evolution of Venus consistent with all available constraints and, more importantly, identify future measurements that would dramatically narrow the range of acceptable scenarios. Obtaining high-resolution imagery and topography, along with any information about the temporal history of a magnetic field, is extremely important. Deformation of geologic features constrains the surface heat flow and lithospheric rheology during their formation. Determining whether craters with radar-dark floors (which comprise 80% of the population) are actually embayed by lava flows would finally settle the controversy over catastrophic versus equilibrium resurfacing. If the core of Venus has completely solidified, then the lack of an internally generated magnetic field today is unsurprising. We might expect dynamo action in the past since relatively high mantle temperatures may increase the rate of core cooling—unless a lack of giant impacts during accretion permitted chemical stratification that resists convection. In any case, uncertainty about our celestial cousin reveals a

  12. Board Task Performance

    DEFF Research Database (Denmark)

    Minichilli, Alessandro; Zattoni, Alessandro; Nielsen, Sabina

    2012-01-01

    influence board tasks, and how the context moderates the relationship between processes and tasks. Our hypotheses are tested on a survey-based dataset of 535 medium-sized and large industrial firms in Italy and Norway, which are considered to substantially differ along legal and cultural dimensions...... identify three board processes as micro-level determinants of board effectiveness. Specifically, we focus on effort norms, cognitive conflicts and the use of knowledge and skills as determinants of board control and advisory task performance. Further, we consider how two different institutional settings...

  13. 7 CFR 1250.304 - Egg Board or Board.

    Science.gov (United States)

    2010-01-01

    ... AGREEMENTS AND ORDERS; MISCELLANEOUS COMMODITIES), DEPARTMENT OF AGRICULTURE EGG RESEARCH AND PROMOTION Egg Research and Promotion Order Definitions § 1250.304 Egg Board or Board. Egg Board or Board or other designatory term adopted by such Board, with the approval of the Secretary, means the administrative body...

  14. Building better boards.

    Science.gov (United States)

    Nadler, David A

    2004-05-01

    Companies facing new requirements for governance are scrambling to buttress financial-reporting systems, overhaul board structures--whatever it takes to comply. But there are limits to how much good governance can be imposed from the outside. Boards know what they ought to be: seats of challenge and inquiry that add value without meddling and make CEOs more effective but not all-powerful. A board can reach that goal only if it functions as a high-performance team, one that is competent, coordinated, collegial, and focused on an unambiguous goal. Such entities don't just evolve; they must be constructed to an exacting blueprint--what the author calls board building. In this article, Nadler offers an agenda and a set of tools that boards can use to define and achieve their objectives. It's important for a board to conduct regular self-assessments and to pay attention to the results of those analyses. As a first step, the directors and the CEO should agree on which of the following common board models best fits the company: passive, certifying, engaged, intervening, or operating. The directors and the CEO should then analyze which business tasks are most important and allot sufficient time and resources to them. Next, the board should take inventory of each director's strengths to ensure that the group as a whole possesses the skills necessary to do its work. Directors must exert more influence over meeting agendas and make sure they have the right information at the right time and in the right format to perform their duties. Finally, the board needs to foster an engaged culture characterized by candor and a willingness to challenge. An ambitious board-building process, devised and endorsed both by directors and by management, can potentially turn a good board into a great one.

  15. Comparison of dayside current layers in Venus' ionosphere and earth's equatorial electrojet

    Science.gov (United States)

    Cole, Keith D.

    1993-01-01

    The major physical aspects of the equatorial electrojet of Earth and the dayside ionospheric current layers of Venus are compared, viz., the electric current intensity and total current, roles of electric field, pressure and gravity, diffusion time scales, and the Bernouille effect. The largest potential differences, of the order of 10 volts, horizontally across the dayside ionosphere of Venus, have important implications for possible dynamo action in the Venus ionosphere and the application of an electric field from the lower atmosphere or from the solar wind. An upper limit to the horizontal scale of vertical magnetic fields in the Venus ionosphere is estimated thereby for the first time. New upper limits on the velocity in, and thickness of, a possible S layer at Venus are presented. If an S layer exists, it is only for extreme conditions of the solar wind. A mechanism for formation of magnetic ropes in the Venus ionosphere is also proposed.

  16. Dynamics and chemistry of Venus' large and complex cloud system : a science case for an in-situ long-term chemical laboratory

    Science.gov (United States)

    Widemann, Thomas; Määttänen, Anni; Wilquet, Valérie; McGouldrick, Kevin; Jessup, Kandis Lea; Wilson, Colin; Limaye, Sanjay; EuroVenus Consortium, the

    2014-05-01

    The planet Venus is the closest to the planet Earth both geographically and geometrically, with an average solar distance only 0.3AU smaller than that of Earth and an equatorial radius that is only 5% smaller than Earth's. But the similarities appear to end there. How did the environments of Venus and Earth become so divergent? The answer to this question relies upon an understanding of Venus' origins, the nature of its present atmosphere, and the role that the clouds have played in evolution and current state of Venus. Venus' clouds are composed of highly concentrated solutions of sulfuric acid and water. The sulfuric acid is produced photochemically from reactions involving water vapor and various sulfur species such as SO2 in the upper atmosphere around 62 km. The region from 50-60 km altitude is convectively unstable, suggesting that most of the cloud formation here is convectively driven, as are cumulus clouds on Earth but with sulfuric acid taking the place of water as the main condensable species. The clouds of Venus are ubiquitous, play a significant role in the radiative balance of the planet, are used as tracers to probe the atmospheric circulation, and are a key part of a global sulfurohydrological cycle that redistributes key greenhouse gasses such as SO2 and H2O. Thus understanding the clouds of Venus holds the key to understanding how Venus itself came to be the world of extremes that it is today. ESA's Venus Express mission, launched in Nov. 2005, has significantly improved our knowledge about the atmosphere of Venus by providing global long-term remote sensing observations with complete coverage in latitude and local solar time. However major questions remain about key minor species and how they vary throughout the major atmospheric regimes in the upper atmosphere, near the cloud tops where photolysis and condensation processes occur, near the surface where coupling and interchange with the atmosphere occurs, and in the middle atmosphere where they

  17. Non-Cooled Power System for Venus Lander

    Science.gov (United States)

    Salazar, Denise; Landis, Geoffrey A.; Colozza, Anthony J.

    2014-01-01

    The Planetary Science Decadal Survey of 2013-2022 stated that the exploration of Venus is of significant interest. Studying the seismic activity of the planet is of particular importance because the findings can be compared to the seismic activity of Earth. Further, the geological and atmospheric properties of Venus will shed light into the past and future of Earth. This paper presents a radioisotope power system (RPS) design for a small low-power Venus lander. The feasibility of the new power system is then compared to that of primary batteries. A requirement for the power source system is to avoid moving parts in order to not interfere with the primary objective of the mission - to collect data about the seismic activity of Venus using a seismometer. The target mission duration of the lander is 117 days, a significant leap from Venera 13, the longest-lived lander on the surface of Venus, which survived for 2 hours. One major assumption for this mission design is that the power source system will not provide cooling to the other components of the lander. This assumption is based on high-temperature electronics technology that will enable the electronics and components of the lander to operate at Venus surface temperature. For the proposed RPS, a customized General Purpose Heat Source Radioisotope Thermoelectric Generator (GPHSRTG) is designed and analyzed. The GPHS-RTG is chosen primarily because it has no moving parts and it is capable of operating for long duration missions on the order of years. This power system is modeled as a spherical structure for a fundamental thermal analysis. The total mass and electrical output of the system are calculated to be 24 kilograms and 26 Watts, respectively. An alternative design for a battery-based power system uses Sodium Sulfur batteries. To deliver a similar electrical output for 117 days, the battery mass is calculated to be 234 kilograms. Reducing mission duration or power required will reduce the required battery mass

  18. Atomic Energy Control Board

    International Nuclear Information System (INIS)

    Blackman, N.S.; Gummer, W.K.

    1982-02-01

    This paper has been prepared to provide an overview of the responsibilities and activities of the Atomic Energy Control Board. It is designed to address questions that are often asked concerning the establishment of the Atomic Energy Control Board, its enabling legislation, licensing and compliance activities, federal-provincial relationships, international obligations, and communications with the public

  19. Conjugate Shear Fractures at 'Ki Corona,' Southeast Parga Chasma, Venus

    Science.gov (United States)

    Willis, J. J.; Hansen, V. L.

    1996-03-01

    Brittle tensile failure of Venus' surface is evident in many tectonic regimes, including as extension fractures associated with caldera collapse, radial and concentric fractures of coronae, fractures normal to folds, and fracture belts. However, evidence of brittle shear failure has been described at only two localities_intersecting fractures oblique to wrinkle ridges in Lavinia Planitia were interpreted as conjugate shear fractures by Watters, and en echelon fractures in Guinevere Planitia record dominant extension. but with a component of shear. We confirm these earlier interpretations, and recognize the widespread nature of conjugate shear fractures across the Venus surface, identifying examples at over 100 locations in varied tectonic regimes, including coronae, wrinkle-ridged plains, and fracture belts. However, we focus here on fracture and fold relations at "Ki Corona" (46.8 degrees S, 302.5 degrees E), and their implications toward corona evolution.

  20. Venus. I - Carbon monoxide distribution and molecular-line searches

    Science.gov (United States)

    Wilson, W. J.; Klein, M. J.; Kahar, R. K.; Gulkis, S.; Olsen, E. T.; Ho, P. T. P.

    1981-01-01

    An observational program to study variations of the vertical distribution of CO in the Venus atmosphere is presented. Measurements of the J = 0 - 1 absorption line at 2.6 mm wavelength are reported for two phase angles in 1977, one near eastern elongation (February) and the other near inferior conjunction (April). The two spectra are significantly different, with the April absorption line being narrower and deeper. The results of numerical inversion calculations show that the CO mixing ratio increases by a factor of approximately 100 between 78 and 100 km and that the CO abundance above approximately 100 km is greatest on the night-side hemisphere. These conclusions are in qualitative agreement with theoretical models. In addition to the CO observations, a search for other molecules was made to provide further information on the composition of the Venus middle atmosphere. The J = 0 - 1 transition of (C-13)O was detected and upper limits were derived for nine other molecules.

  1. Basic theory and model calculations of the Venus ionosphere

    Science.gov (United States)

    Nagy, A. F.; Cravens, T. E.; Gombosi, T. I.

    1983-01-01

    An assessment is undertaken of current understanding of the physical and chemical processes that control Venus's ionospheric behavior, in view of the data that has been made available by the Venera and Pioneer Venus missions. Attention is given to the theoretical framework used in general planetary ionosphere studies, especially to the equations describing the controlling physical and chemical processes, and to the current status of the ion composition, density and thermal structure models developed to reproduce observed ionospheric behavior. No truly comprehensive and successful model of the nightside ionosphere has been published. Furthermore, although dayside energy balance calculations yield electron and ion temperature values that are in close agreement with measured values, the energetics of the night side eludes understanding.

  2. Data acquisition system for the VENUS detector at TRISTAN

    Energy Technology Data Exchange (ETDEWEB)

    Amako, K.; Arai, Y.; Sakamoto, H.; Teramoto, Y.; Uehara, S.; Yasu, Y.; Chiba, Y.; Endo, I.; Hayashibara, I.; Ohsugi, T.

    1988-11-01

    A data acquisition system for the VENUS detector at the TRISTAN electron-positron collider is presented. The whole system of the VENUS detector consists of nine different kinds of principal detectors, and the total number of electronics channels of the system reaches about 30 000. A FASTBUS system was introduced as the main data path and the TKO and the CAMAC standard have also been utilized for the frontened electronics. A FASTBUS interface to an on-line computer (VAX11/780), simplex segment interconnect and many data acquisition modules were developed. Most of the data are analyzed in a VAX cluster system in real time. Data logging is done in a main frame computer (FACOM M382) by using an automatic loading cartridge tape subsystem.

  3. Image processing and products for the Magellan mission to Venus

    Science.gov (United States)

    Clark, Jerry; Alexander, Doug; Andres, Paul; Lewicki, Scott; Mcauley, Myche

    1992-01-01

    The Magellan mission to Venus is providing planetary scientists with massive amounts of new data about the surface geology of Venus. Digital image processing is an integral part of the ground data system that provides data products to the investigators. The mosaicking of synthetic aperture radar (SAR) image data from the spacecraft is being performed at JPL's Multimission Image Processing Laboratory (MIPL). MIPL hosts and supports the Image Data Processing Subsystem (IDPS), which was developed in a VAXcluster environment of hardware and software that includes optical disk jukeboxes and the TAE-VICAR (Transportable Applications Executive-Video Image Communication and Retrieval) system. The IDPS is being used by processing analysts of the Image Data Processing Team to produce the Magellan image data products. Various aspects of the image processing procedure are discussed.

  4. Earthlike planets: Surfaces of Mercury, Venus, earth, moon, Mars

    Science.gov (United States)

    Murray, B.; Malin, M. C.; Greeley, R.

    1981-01-01

    The surfaces of the earth and the other terrestrial planets of the inner solar system are reviewed in light of the results of recent planetary explorations. Past and current views of the origin of the earth, moon, Mercury, Venus and Mars are discussed, and the surface features characteristic of the moon, Mercury, Mars and Venus are outlined. Mechanisms for the modification of planetary surfaces by external factors and from within the planet are examined, including surface cycles, meteoritic impact, gravity, wind, plate tectonics, volcanism and crustal deformation. The origin and evolution of the moon are discussed on the basis of the Apollo results, and current knowledge of Mercury and Mars is examined in detail. Finally, the middle periods in the history of the terrestrial planets are compared, and future prospects for the exploration of the inner planets as well as other rocky bodies in the solar system are discussed.

  5. Pioneer Venus Orbiter Radar Mapper - Design and operation

    Science.gov (United States)

    Pettengill, G. H.; Horwood, D. F.; Keller, C. H.

    1980-01-01

    The Radar Mapper Experiment, carried aboard the Pioneer Venus Orbiter spacecraft, is designed to obtain a near-global picture of the topography, meter-scale surface slopes and reflectivity of Venus. Constraints imposed by the choice of orbit limit radar coverage to a latitude band lying between 74 deg N and 61 deg S completely around the planet. In addition to the altimetry objectives, the experiment seeks an image of the radar scattering properties of the surface at oblique incidence. Sensitivity limits the imaged region to a band around the planet lying between 45 deg N and 10 deg S. Altimetric error is less than 200 m; altimetric surface 'footprint' size varies from about 10 km in diameter at a spacecraft altitude of 200 km, to 50 km at a maximum altitude of 4700 km. Imaging varies from 20 to 40 km, depending on spacecraft altitude.

  6. Mantle differentiation and thermal evolution of Mars, Mercury, and Venus

    International Nuclear Information System (INIS)

    Spohn, T.

    1991-01-01

    In the present models for the thermal evolution of Mercury, Venus, and Mars encompass core and mantle chemical differentiation, lithospheric growth, and volcanic heat-transfer processes. Calculation results indicate that crust and lithosphere thicknesses are primarily dependent on planet size as well as the bulk concentration of planetary radiogenic elements and the lithosphere's thermal conductivity. The evidence for Martian volcanism for at least 3.5 Gyr, and in Mercury for up to 1 Gyr, in conjunction with the presence of a magnetic field on Mercury and its absence on Mars, suggest the dominance of a lithospheric conduction heat-transfer mechanism in these planets for most of their thermal history; by contrast, volcanic heat piping may have been an important heat-transfer mechanism on Venus. 50 refs

  7. Disposal of radioactive waste in space towards Venus

    International Nuclear Information System (INIS)

    Anon.

    1980-01-01

    A review is given of an artical in Astronautics and Aeronautics by C. Priest, R. Nixon and E. Rice describing a NASA funded research project on the possible storage of highly radioactive waste in an orbit round the sun between earth and Venus. Minimum distance from earth is expected to be 22.5 million kilometers and it is suggested that storage should be secure for a million years. (G.M.E.)

  8. Parabolic features and the erosion rate on Venus

    Science.gov (United States)

    Strom, Robert G.

    1993-01-01

    The impact cratering record on Venus consists of 919 craters covering 98 percent of the surface. These craters are remarkably well preserved, and most show pristine structures including fresh ejecta blankets. Only 35 craters (3.8 percent) have had their ejecta blankets embayed by lava and most of these occur in the Atla-Beta Regio region; an area thought to be recently active. parabolic features are associated with 66 of the 919 craters. These craters range in size from 6 to 105 km diameter. The parabolic features are thought to be the result of the deposition of fine-grained ejecta by winds in the dense venusian atmosphere. The deposits cover about 9 percent of the surface and none appear to be embayed by younger volcanic materials. However, there appears to be a paucity of these deposits in the Atla-Beta Regio region, and this may be due to the more recent volcanism in this area of Venus. Since parabolic features are probably fine-grain, wind-deposited ejecta, then all impact craters on Venus probably had these deposits at some time in the past. The older deposits have probably been either eroded or buried by eolian processes. Therefore, the present population of these features is probably associated with the most recent impact craters on the planet. Furthermore, the size/frequency distribution of craters with parabolic features is virtually identical to that of the total crater population. This suggests that there has been little loss of small parabolic features compared to large ones, otherwise there should be a significant and systematic paucity of craters with parabolic features with decreasing size compared to the total crater population. Whatever is erasing the parabolic features apparently does so uniformly regardless of the areal extent of the deposit. The lifetime of parabolic features and the eolian erosion rate on Venus can be estimated from the average age of the surface and the present population of parabolic features.

  9. Decamp Clock Board Firmware

    International Nuclear Information System (INIS)

    Vicente, J. de; Castilla, J.; Martinez, G.

    2007-01-01

    Decamp (Dark Energy Survey Camera) is a new instrument designed to explore the universe aiming to reveal the nature of Dark Energy. The camera consists of 72 CCDs and 520 Mpixels. The readout electronics of DECam is based on the Monsoon system. Monsoon is a new image acquisition system developed by the NOAO (National Optical Astronomical Observatory) for the new generation of astronomical cameras. The Monsoon system uses three types of boards inserted in a Eurocard format based crate: master control board, acquisition board and clock board. The direct use of the Monsoon system for DECam readout electronics requires nine crates mainly due to the high number of clock boards needed. Unfortunately, the available space for DECam electronics is constrained to four crates at maximum. The major drawback to achieve such desired compaction degree resides in the clock board signal density. This document describes the changes performed at CIEMAT on the programmable logic of the Monsoon clock board aiming to meet such restricted space constraints. (Author) 5 refs

  10. Decamp Clock Board Firmware

    Energy Technology Data Exchange (ETDEWEB)

    Vicente, J. de; Castilla, J.; Martinez, G.

    2007-09-27

    Decamp (Dark Energy Survey Camera) is a new instrument designed to explore the universe aiming to reveal the nature of Dark Energy. The camera consists of 72 CCDs and 520 Mpixels. The readout electronics of DECam is based on the Monsoon system. Monsoon is a new image acquisition system developed by the NOAO (National Optical Astronomical Observatory) for the new generation of astronomical cameras. The Monsoon system uses three types of boards inserted in a Eurocard format based crate: master control board, acquisition board and clock board. The direct use of the Monsoon system for DECam readout electronics requires nine crates mainly due to the high number of clock boards needed. Unfortunately, the available space for DECam electronics is constrained to four crates at maximum. The major drawback to achieve such desired compaction degree resides in the clock board signal density. This document describes the changes performed at CIEMAT on the programmable logic of the Monsoon clock board aiming to meet such restricted space constraints. (Author) 5 refs.

  11. Analysis of Volcanic Deposits on Venus Using Radar Polarimetry

    Science.gov (United States)

    Douglas, M.; Carter, L. M.

    2015-12-01

    The atmosphere of Venus is relatively transparent at radio wavelengths, providing an opportunity to examine its volcanic planetary surface using radar. The highest resolution radar images come from the Magellan mission, which mapped 98% of Venus's surface by transmitting and receiving unidirectionally polarized radio waves. Upgrades to the ground-based Arecibo telescope in 1999 allowed further imaging of the surface of Venus at conjunction in 1999, 2001, and 2004 by the transmission of a circularly polarized beam at 12.6cm wavelength and then the reception of two orthogonal circular polarization components [Carter et al., 2006]. We apply the Stokes vector method to the Arecibo measurements to calculate the circular polarization ratio (CPR), an indication of surface roughness, and the degree of linear polarization (DLP), a measure of whether there is subsurface scattering of the radar wave. We combine both the CPR and DLP datasets to enable a more holistic geologic interpretation of Magellan images. This allows us to examine geographic variations in high-altitude, high-emissivity regions such Beta Regio, and to investigate regions that may contain young lava flows such as Themis Regio. Our approach permits a more precise geologic mapping of the textures of coronas and lava flow fields, including the identification of abnormally rugged lava flows. The data were also used to search for pyroclastics emanating from large and intermediate sized volcanoes within the region visible to Arecibo.

  12. Specular Reflections: John Brett and the Mirror of Venus

    Directory of Open Access Journals (Sweden)

    James Mussell

    2013-10-01

    Full Text Available Normal 0 false false false EN-GB X-NONE X-NONE MicrosoftInternetExplorer4 When John Brett, the Pre-Raphaelite painter and astronomer, presented his theory of specular reflection in Venus to the Royal Astronomical Society, he provoked a controversy over both the constitution of the planet and the learned society. Brett thought Venus was most likely a ball of molten metal enclosed in a glass envelope and this raised the tantalizing possibility that it might function as a mirror, reflecting back an image of the earth. A few months later another 'Mirror of Venus 'was displayed at the Grosvenor Gallery. The surface of Edward Burne-Jones's painting provides a different model of reflection but one that illuminates the space of the Royal Astronomical Society and the practice of astronomy more broadly. Using Burne-Jones’s painting as a point of comparison, I argue that Brett’s astronomy put into play a desiring, viewing subject that was disavowed in his landscape art.

  13. Magellan: A new view of Venus' geology and geophysics

    Science.gov (United States)

    Bindschadler, D. L.

    1995-07-01

    Within the past fifteen years, the surface of Venus has gone from being the least well understood of all the terrestrial planets to the most thoroughly mapped surface of any terrestrial planet, including the Earth. This is primarily due to the Magellan mission, which has collected a variety of data on the surface morphology, physical properties, and interior density structure of Venus amounting to more than 1 Terabit (1012 bits) of data. Synthetic aperture radar images have been obtained for over 95% of the surface; their high resolution reveals most surface features larger than 100-200 meters across. Using its radar altimeter, Magellan has collected data on surface elevations, sub-meter scale roughness, and radar reflectivity at a resolution of approximately 10 km. Further information on the physical properties of the surface was gathered by measuring the passive microwave emissivity of the surface [Pettengill et al, 1992]. Two-way Doppler tracking of the spacecraft has yielded line-of-sight (LOS) gravity data and a spherical harmonic model of gravity and geoid out to degree 75. Collection of high-resolution gravity data has been aided by an innovative aerobraking maneuver, which used Venus' atmosphere to brake the spacecraft and lower it from a highly elliptical orbit to a near-circular orbit.

  14. Near-infrared oxygen airglow from the Venus nightside

    Science.gov (United States)

    Crisp, D.; Meadows, V. S.; Allen, D. A.; Bezard, B.; Debergh, C.; Maillard, J.-P.

    1992-01-01

    Groundbased imaging and spectroscopic observations of Venus reveal intense near-infrared oxygen airglow emission from the upper atmosphere and provide new constraints on the oxygen photochemistry and dynamics near the mesopause (approximately 100 km). Atomic oxygen is produced by the Photolysis of CO2 on the dayside of Venus. These atoms are transported by the general circulation, and eventually recombine to form molecular oxygen. Because this recombination reaction is exothermic, many of these molecules are created in an excited state known as O2(delta-1). The airglow is produced as these molecules emit a photon and return to their ground state. New imaging and spectroscopic observations acquired during the summer and fall of 1991 show unexpected spatial and temporal variations in the O2(delta-1) airglow. The implications of these observations for the composition and general circulation of the upper venusian atmosphere are not yet understood but they provide important new constraints on comprehensive dynamical and chemical models of the upper mesosphere and lower thermosphere of Venus.

  15. Board Effectiveness in Small Firms

    OpenAIRE

    Söderqvist, Anette; Wägar, Karolina

    2010-01-01

    Purpose: This study investigates boards of directors in small firms and explores the link between board effectiveness and the composition, roles and working styles of the boards. Design/methodology/approach: The study analyses data from a telephone survey of boards in 45 small firms. The survey included both the CEO and the chairperson of the board. Findings: The study identifies three groups of small firms: ‘paperboards’, ‘professional boards’, and ‘management lead’ boards. Results show that...

  16. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2008-01-01

    The Joint Advisory Appeals Board has examined the internal appeal lodged by a member of the personnel against the decision to grant him only a periodic one-step advancement for the 2006 reference year. The person concerned has not objected to the report of the Board and the final decision of the Director-General being brought to the attention of the members of the personnel. In application of Article R VI 1.18 of the Staff Regulations, these documents will therefore be posted on the notice board of the Main building (bldg. 500) from 1 September to 14 September 2008. Human Resources Department (73911)

  17. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2008-01-01

    The Joint Advisory Appeals Board has examined the internal appeal lodged by a member of the personnel with regard to the decision not to grant him an indefinite contract. The person concerned has not objected to the report of the Board and the final decision of the Director-General being brought to the notice of the members of the personnel. In application of Article R VI 1.18 of the Staff Regulations, these documents will therefore be posted on the notice board of the Main Building (Bldg. 500) from 26 May to 6 June 2008. Human Resources Department (73911)

  18. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2006-01-01

    The Joint Advisory Appeals Board was convened to examine an appeal lodged by a member of the personnel with regard to advancement. The person concerned has requested that the report of the Board and the final decision of the Director-General be brought to the notice of the personnel in accordance with Article R VI 1.20 of the Staff Regulations. The relevant documents will therefore be posted on the notice boards of the Administration Building (No. 60) from 24 March to 10 April 2006. Human Resources Department Tel. 74128

  19. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2008-01-01

    The Joint Advisory Appeals Board has examined the internal appeal lodged by a member of the personnel against the decision to grant him only a periodic one-step advancement for the 2006 reference year. The person concerned has not objected to the report of the Board and the final decision of the Director-General being brought to the attention of the members of the personnel. In application of Article R VI 1.18 of the Staff Regulations, these documents will therefore be posted on the notice board of the Main Building (Bldg. 500) from 1 September to 14 September 2008. Human Resources Department (73911)

  20. Joint Advisory Appeals Board

    CERN Multimedia

    2003-01-01

    The Joint Advisory Appeals Board was convened to examine the appeal lodged by Mrs Judith Igo-Kemenes concerning the application of procedures foreseen by Administrative Circular N§ 26 (Rev. 3). As the appellant has not objected, the report of the Board and the final decision of the Director-General are brought to the notice of the personnel in accordance with Article R VI 1.20 of the Staff Regulations. The relevant documents will therefore be posted on the notice boards of the Administration Building (N° 60) from 6 to 20 June 2003. Human Resources Division Tel. 74128

  1. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2008-01-01

    The Joint Advisory Appeals Board was convened to examine an internal appeal lodged by a member of the personnel with regard to the decision not to grant him an indefinite contract. The person concerned has not objected to the report of the Board and the final decision of the Director-General being brought to the notice of the members of the personnel, in accordance with Article R VI 1.18 of the Staff Regulations. These documents will therefore be posted on the notice board of the Main Building (Bldg. 60) from 21 January to 3 February 2008. Human Resources Department (73911)

  2. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2008-01-01

    The Joint Advisory Appeals Board has examined the internal appeal lodged by a member of the personnel with regard to the decision not to award him a periodic one-step advancement for the 2006 reference year. The person concerned has not objected to the report of the Board and the final decision of the Director-General being brought to the notice of the members of the personnel. In application of Article R VI 1.18 of the Staff Regulations, these documents will therefore be posted on the notice board of the Main building (Bldg. 500) from 17 March to 30 March 2008. Human Resources Department Tel. 73911

  3. Joint Advisory Appeals Board

    CERN Multimedia

    HR Department

    2007-01-01

    The Joint Advisory Appeals Board was convened to examine an internal appeal lodged by a member of the personnel with regard to the decision not to grant him an indefinite contract. The person concerned has requested that the report of the Board and the final decision of the Director-General be brought to the notice of the members of the personnel, in accordance with Article R VI 1.18 of the Staff Regulations. The relevant documents will therefore be posted on the notice board of the Main building (Bldg. 60) from 24 September to 7 October 2007. Human Resources Department

  4. Primer printed circuit boards

    CERN Document Server

    Argyle, Andrew

    2009-01-01

    Step-by-step instructions for making your own PCBs at home. Making your own printed circuit board (PCB) might seem a daunting task, but once you master the steps, it's easy to attain professional-looking results. Printed circuit boards, which connect chips and other components, are what make almost all modern electronic devices possible. PCBs are made from sheets of fiberglass clad with copper, usually in multiplelayers. Cut a computer motherboard in two, for instance, and you'll often see five or more differently patterned layers. Making boards at home is relatively easy

  5. Joint Advisory Appeals Board

    CERN Multimedia

    2003-01-01

    The Joint Advisory Appeals Board was convened to examine the appeal lodged by Mr Aloïs Girardoz with regard to classification and advancement. As the appellant has not objected, the Board's report and the Director-General's decision will be brought to the notice of the personnel in accordance with Article R VI 1.20 of the Staff Regulations. The relevant documents will therefore be posted on the notice boards of the Administration Building (N° 60) from 15 to 29 August 2003. Human Resources Division Tel. 74128

  6. Venus Kinase Receptors: prospects in signalling and biological functions of these invertebrate receptors

    Directory of Open Access Journals (Sweden)

    Colette eDissous

    2014-05-01

    Full Text Available Venus Kinase Receptors (VKRs form a family of invertebrate receptor tyrosine kinases (RTKs initially discovered in the parasitic platyhelminth Schistosoma mansoni. VKRs are single transmembrane receptors which contain an extracellular Venus Flytrap (VFT structure similar to the ligand binding domain of G Protein Coupled Receptors of class C, and an intracellular Tyrosine Kinase domain close to that of Insulin Receptors. VKRs are found in a large variety of invertebrates from cnidarians to echinoderms, and are highly expressed in larval stages and in gonads, suggesting a role of these proteins in embryonic and larval development as well as in reproduction. Vkr gene silencing could demonstrate the function of these receptors in oogenesis as well as in spermatogenesis in Schistosoma .mansoni. VKRs are activated by amino-acids, and highly responsive to arginine. As many other RTKs, they form dimers when activated by ligands and induce intracellular pathways involved in protein synthesis and cellular growth, such as MAPK and PI3K/Akt/S6K pathways. VKRs are not present in vertebrates, nor in some invertebrate species. Questions remain open about the origin of this little-known RTK family in evolution and its role in emergence and specialization of Metazoa. What is the meaning of maintenance or loss of VKR in some phyla or species in terms of development and physiological functions? The presence of VKRs in invertebrates of economical and medical importance, such as pests, vectors of pathogens and platyhelminth parasites, and the implication of these RTKs in gametogenesis and reproduction processes are valuable reasons to consider VKRs as interesting targets in new programs for eradication/ control of pests and infectious diseases, with the main advantage in the case of parasite targeting that VKR counterparts are absent from the vertebrate host kinase panel.

  7. Novel Architecture for a Long-Life, Lightweight Venus Lander

    International Nuclear Information System (INIS)

    Bugby, D.; Seghi, S.; Kroliczek, E.; Pauken, M.

    2009-01-01

    This paper describes a novel concept for an extended lifetime, lightweight Venus lander. Historically, to operate in the 480 deg. C, 90 atm, corrosive, mostly CO 2 Venus surface environment, previous landers have relied on thick Ti spherical outer shells and thick layers of internal insulation. But even the most resilient of these landers operated for only about 2 hours before succumbing to the environment. The goal on this project is to develop an architecture that extends lander lifetime to 20-25 hours and also reduces mass compared to the Pioneer Venus mission architecture. The idea for reducing mass is to: (a) contain the science instruments within a spherical high strength lightweight polymer matrix composite (PMC) tank; (b) surround the PMC tank with an annular shell of high performance insulation pre-pressurized to a level that (after landing) will exceed the external Venus surface pressure; and (c) surround the insulation with a thin Ti outer shell that contains only a net internal pressure, eliminating buckling overdesign mass. The combination of the PMC inner tank and thin Ti outer shell is lighter than a single thick Ti outer shell. The idea for extending lifetime is to add the following three features: (i) an expendable water supply that is placed within the insulation or is contained in an additional vessel within the PMC tank; (ii) a thin spherical evaporator shell placed within the insulation a short radial distance from the outer shell; and (iii) a thin heat-intercepting liquid cooled shield placed inboard of the evaporator shell. These features lower the temperature of the insulation below what it would have been with the insulation alone, reducing the internal heat leak and lengthening lifetime. The use of phase change materials (PCMs) inside the PMC tank is also analyzed as a lifetime-extending design option. The paper describes: (1) analytical modeling to demonstrate reduced mass and extended life; (2) thermal conductivity testing of high

  8. CMS Collaboration Board Meeting

    CERN Multimedia

    Hoch, Michael

    2013-01-01

    The first CMS Collaboration Board meeting of the year (2013) provided an opportunity to thank Teresa Rodrigo, Matthias Kasemann and Randy Ruchti, the 2011-12 CB Chair, Deputy Chair and Secretary, respectively.

  9. Boat boarding ladder placement

    Science.gov (United States)

    1998-04-01

    Presented in three volumes; 'Boat Boarding Ladder Placement,' which explores safety considerations including potential for human contact with a rotating propeller; 'Boat Handhold Placement,' which explores essential principles and methods of fall con...

  10. Checking a printed board

    CERN Multimedia

    1977-01-01

    An 'Interactive Printed Circuit Board Design System' has been developed by a company in a Member-State. Printed circuits are now produced at the SB's surface treatment workshop using a digitized photo-plotter.

  11. Boarding school rules.

    Science.gov (United States)

    Griffiths, Matt

    2017-01-04

    Ofsted inspects and regulates services that care for children and young people, including boarding facilities. Medication management is an integral part of caring for children in boarding schools, and robust systems must be in place to pass inspection. These systems must cover how medicines are dispensed, administered and stored at the facility, risk assessments, identifying which pupils can manage their own medicines and the individual health needs of boarders, so that care plans can be put in place for children with specific needs.

  12. Equilibrium resurfacing of Venus: Results from new Monte Carlo modeling and implications for Venus surface histories

    Science.gov (United States)

    Bjonnes, E. E.; Hansen, V. L.; James, B.; Swenson, J. B.

    2012-02-01

    Venus' impact crater population imposes two observational constraints that must be met by possible model surface histories: (1) near random spatial distribution of ˜975 craters, and (2) few obviously modified impact craters. Catastrophic resurfacing obviously meets these constraints, but equilibrium resurfacing histories require a balance between crater distribution and modification to be viable. Equilibrium resurfacing scenarios with small incremental resurfacing areas meet constraint 1 but not 2, whereas those with large incremental resurfacing areas meet constraint 2 but not 1. Results of Monte Carlo modeling of equilibrium resurfacing ( Strom et al., 1994) is widely cited as support for catastrophic resurfacing hypotheses and as evidence against hypotheses of equilibrium resurfacing. However, the Monte Carlo models did not consider intermediate-size incremental resurfacing areas, nor did they consider histories in which the era of impact crater formation outlasts an era of equilibrium resurfacing. We construct three suites of Monte Carlo experiments that examine incremental resurfacing areas not previously considered (5%, 1%, 0.7%, and 0.1%), and that vary the duration of resurfacing relative to impact crater formation time (1:1 [suite A], 5:6 [suite B], and 2:3 [suite C]). We test the model results against the two impact crater constraints. Several experiments met both constraints. The shorter the time period of equilibrium resurfacing, or the longer the time of crater formation following the cessation of equilibrium resurfacing, the larger the possible areas of incremental resurfacing that satisfy both constraints. Equilibrium resurfacing is statistically viable for suite A at 0.1%, suite B at 0.1%, and suite C for 1%, 0.7%, and 0.1% areas of incremental resurfacing.

  13. COLLABORATION BOARD (CB55)

    CERN Multimedia

    B. Cousins

    Open Access Publication Policy ATLAS had recently issued a short statement in support of open access publishing. The mood of the discussions in the December CMS Collaboration Board had appeared to be in favour and so it was being proposed that CMS issue the same statement as that made by ATLAS (the statement is attached to the agenda of this meeting). The Collaboration Board agreed. Election of the Chair of the Collaboration Board Following the agreement to shorten the terms of both the Spokesperson and the Collaboration Board Chair, and to introduce a longer overlap period between the election and the start of the term, the election for the next Collaboration Board Chair was due in December 2007. If the old standard schedule specified in the Constitution were adapted to this date, then the Board should be informed at the present meeting that the election was being prepared. However, it was felt that the experience of the previous year's election of the Spokesperson had shown that it would be desirable to...

  14. Board certification in optometry.

    Science.gov (United States)

    Kirby, B S; Weaver, J L; Amos, J F; Hendrix, W G; Lewis, T L; Locke, J C; McCall, J A; Walls, L L

    2000-04-01

    In keeping with current expectations in the health care community, the purpose of the American Board of Optometric Practice (ABOP) is to enhance the quality of optometric care available to the public by fostering continued competence for practitioners through administering education and examinations for certification and re-certification. The formation of ABOP makes possible for the first time a board certification process for optometrists. The optometry model for board certification and recertification emphasizes the breadth of the profession. ABOP certification will be accomplished through a combination of examinations and high-quality, tested Board Certified Continuing Education (BCCE). Specific requirements for practitioners at various stages of their careers are presented. Board certification provides one important mechanism for an optometrist to demonstrate commitment to quality, professionalism, and ongoing clinical competence. The optometrist benefits from high-quality continuing education designed for timeliness, importance, and breadth. The public benefits by the enhancement of continued competence within the optometric profession. Health care agencies benefit by being able to recognize providers who have elected to demonstrate their qualifications through certification. Through board certification, optometrists will be able to demonstrate their commitment to maintaining clinical competence through a nationally uniform program, and they will be able to comply with standards that are generally recognized and required throughout the health care community.

  15. Summing Up the Unique Venus Transit 2004 (VT-2004) Programme

    Science.gov (United States)

    2004-11-01

    On June 8, 2004, Venus - the Earth's sister planet - passed in front of the Sun. This rare event - the last one occurred in 1882 - attracted the attention of millions of people all over the world. In a few days' time, on November 5-7, 2004, about 150 educators, media representatives, as well as amateur and professional astronomers will gather in Paris (France) at the international conference "The Venus Transit Experience" to discuss the outcome of the related Venus Transit 2004 (VT-2004) public education programme. This unique project was set up by the European Southern Observatory (ESO), together with the European Association for Astronomy Education (EAAE), the Institut de Mécanique Céleste et de Calcul des Éphémérides (IMCCE) and the Observatoire de Paris in France, as well as the Astronomical Institute of the Academy of Sciences of the Czech Republic. It was also supported by the European Commission in the framework of the European Science and Technology Week, cf. ESO PR 03/04. The VT-2004 programme successfully exposed the broad public to a number of fundamental issues at the crucial interface between society and basic science. It ensured the most comprehensive real-time coverage of the event via an extremely dynamic Central Display that was updated a short intervals. Thanks to the prior establishment of hundreds of mirror sites, the VT-2004 website was easily accessible all through the transit, even though it experienced about 55 million webhits during a period of 8 hours. The VT-2004 programme established a wide international network of individuals (including school teachers and their students, amateur astronomers, interested laypeople, etc.) and educational institutions (astronomical observatories, planetaria, science centres, etc.), as well as 25 National Nodes with their own websites about the Venus Transit in as many local languages. It collected a large number of photos and drawings. It also included an international Video Contest, inviting all

  16. Board diversity and sustainability performance

    African Journals Online (AJOL)

    kirstam

    of a trend analysis to compare the differences in board composition between a sample of ... 15Key words: sustainability, sustainability performance, boards of directors, board diversity, corporate governance, SRI index, director background, King Report, integrative model of board performance, corporate social responsibility.

  17. Board Certification in Counseling Psychology

    Science.gov (United States)

    Crowley, Susan L.; Lichtenberg, James W.; Pollard, Jeffrey W.

    2012-01-01

    Although specialty board certification by the American Board of Professional Psychology (ABPP) has been a valued standard for decades, the vast majority of counseling psychologists do not pursue board certification in the specialty. The present article provides a brief history of board certification in general and some historical information about…

  18. Venus' Spectral Signatures and the Potential for Life in the Clouds.

    Science.gov (United States)

    Limaye, Sanjay S; Mogul, Rakesh; Smith, David J; Ansari, Arif H; Słowik, Grzegorz P; Vaishampayan, Parag

    2018-03-30

    The lower cloud layer of Venus (47.5-50.5 km) is an exceptional target for exploration due to the favorable conditions for microbial life, including moderate temperatures and pressures (∼60°C and 1 atm), and the presence of micron-sized sulfuric acid aerosols. Nearly a century after the ultraviolet (UV) contrasts of Venus' cloud layer were discovered with Earth-based photographs, the substances and mechanisms responsible for the changes in Venus' contrasts and albedo are still unknown. While current models include sulfur dioxide and iron chloride as the UV absorbers, the temporal and spatial changes in contrasts, and albedo, between 330 and 500 nm, remain to be fully explained. Within this context, we present a discussion regarding the potential for microorganisms to survive in Venus' lower clouds and contribute to the observed bulk spectra. In this article, we provide an overview of relevant Venus observations, compare the spectral and physical properties of Venus' clouds to terrestrial biological materials, review the potential for an iron- and sulfur-centered metabolism in the clouds, discuss conceivable mechanisms of transport from the surface toward a more habitable zone in the clouds, and identify spectral and biological experiments that could measure the habitability of Venus' clouds and terrestrial analogues. Together, our lines of reasoning suggest that particles in Venus' lower clouds contain sufficient mass balance to harbor microorganisms, water, and solutes, and potentially sufficient biomass to be detected by optical methods. As such, the comparisons presented in this article warrant further investigations into the prospect of biosignatures in Venus' clouds. Key Words: Venus-Clouds-Life-Habitability-Microorganism-Albedo-Spectroscopy-Biosignatures-Aerosol-Sulfuric Acid. Astrobiology 18, xxx-xxx.

  19. Short-wavelength contractional structures in crustal plateau fold belts on Venus: constraints on early thermal state

    Science.gov (United States)

    Ghent, R. R.; Phillips, R. J.; Hansen, V. L.; Nunes, D. C.

    2002-05-01

    Marginal fold belts within Venusian crustal plateaus are characterized by contractional tectonic features showing a range of spatial wavelengths from 30 km. Previous studies have proposed that these features are folds formed by layer-normal compression during crustal plateau formation [e.g., 1] and that the characteristic deformation wavelength(s) expressed by these features reflect the thickness of a competent surface layer during deformation [1, 2]. We investigate the conditions under which the shortest wavelength features represented in these fold belts may have formed. Specifically, we report on finite element simulations of concurrent shortening and cooling in models with uniform composition and elasto-visco-plastic (EVP) rheology. The models are constrained by observations of crustal plateau marginal fold belts using Magellan SAR imagery and are motivated by the current plume tectonic hypothesis for crustal plateau formation [2, 3]. The models are unique because a) the EVP rheology more accurately represents the actual crust than viscous or viscoelastic models; and b) our models incorporate spatially uniform material properties but temperature-dependent rheology [4], so that the strength profile through the crust evolves with cooling. This allows local thermal and stress conditions to determine the instantaneous effective surface layer thickness and strength, which in turn determines surface topographic wavelengths. We find that short-wavelength contractional features can form under hot conditions consistent with the plume scenario but do not form under cooler conditions. The final model topography results from simultaneous brittle faulting and viscous folding. We conclude that the shortest-wavelength features preserved in marginal fold belts record an early stage of crustal plateau evolution and require an elevated thermal gradient and surface temperature. [1] Ghent, R.R., and V.L. Hansen 1999. Structural and kinematic analysis of eastern Ovda Regio,Venus

  20. Airborne Measurements of Venus Cloud-top H2O and HDO from NASA’s SOFIA in the Mid-Infrared

    Science.gov (United States)

    Tsang, Constantine; Encrenaz, Therese; DeWitt, Curtis N.; Richter, Matthew; Irwin, Patrick

    2017-10-01

    The determination of the D/H ratio in Venus’s atmosphere using water (H2O) and light water (HDO) has been used as evidence for the loss of a global sized ocean in the distant past on paleo-Venus. Measurements of atmospheric water vapour at and above the cloud level is also important as water is a key ingredient in the production of the hydrated H2SO4 clouds that prevail globally on Venus. While variations in latitude and local solar time of H2O at the cloud tops has been most recently measured by ESA’s Venus Express spacecraft, the data is sporadic due to the limb sounding geometry needed to make these measurements.Here we present H2O and HDO measurements from January 2017 from NASA’s Stratospheric Observatory for Infrared Astronomy (SOFIA) using the EXES mid-infrared spectrometer flying at 40,000 ft where the relatively low telluric absorption makes detection of Venusian H2O possible. Two observation sequences were obtained that yielded spatially resolved maps of H2O and HDO at R~89,000 centered at 7.21 µm (1380 cm-1). We will also discuss the preliminary retrieved values of D/H ratios at the 65 km altitude probed at this wavelength.

  1. Carl Sagan and the Exploration of Mars and Venus

    Science.gov (United States)

    Toon, Owen B.; Condon, Estelle P. (Technical Monitor)

    1997-01-01

    Inspired by childhood readings of books by Edgar Rice Burroughs, Carl Sagan's first interest in planetary science focused on Mars and Venus. Typical of much of his career he was skeptical of early views about these planets. Early in this century it was thought that the Martian wave of darkening, a seasonal albedo change on the planet, was biological in origin. He suggested instead that it was due to massive dust storms, as was later shown to be the case. He was the first to recognize that Mars has huge topography gradients across its surface. During the spacecraft era, as ancient river valleys were found on the planet, he directed studies of Mars' ancient climate. He suggested that changes in the planets orbit were involved in climate shifts on Mars, just as they are on Earth. Carl had an early interest in Venus. Contradictory observations led to a controversy about the surface temperature, and Carl was one of the first to recognize that Venus has a massive greenhouse effect at work warming its surface. His work on radiative transfer led to an algorithm that was extensively used by modelers of the Earth's climate and whose derivatives still dominate the calculation of radiative transfer in planetary atmospheres today. Carl inspired a vast number of young scientists through his enthusiasm for new ideas and discoveries, his skeptical approach, and his boundless energy. I had the privilege to work in Carl's laboratory during the peak of the era of Mars' initial exploration. It was an exciting time, and place. Carl made it a wonderful experience.

  2. On the Thermal Protection Systems of Landers for Venus Exploration

    Science.gov (United States)

    Ekonomov, A. P.; Ksanfomality, L. V.

    2018-01-01

    The landers of the Soviet Venera series—from Venera-9 to Venera-14—designed at the Lavochkin Association are a man-made monument to spectacular achievements of Soviet space research. For more than 40 years, they have remained the uneclipsed Soviet results in space studies of the Solar System. Within the last almost half a century, the experiments carried out by the Venera-9 to Venera-14 probes for studying the surface of the planet have not been repeated by any space agency in the world, mainly due to quite substantial technical problems. Since that time, no Russian missions with landers have been sent to Venus either. On Venus, there is an anoxic carbon dioxide atmosphere, where the pressure is 9.2 MPa and the temperature is 735 K near the surface. A long-lived lander should experience these conditions for an appreciable length of time. What technical solutions could provide a longer operation time for a new probe investigating the surface of Venus, if its thermal scheme is constructed similar to that of the Venera series? Onboard new landers, there should be a sealed module, where the physical conditions required for operating scientific instruments are maintained for a long period. At the same time, new high-temperature electronic equipment that remains functional under the above-mentioned conditions have appeared. In this paper, we consider and discuss different variants of the system for a long-lived sealed lander, in particular, the absorption of the penetrating heat due to water evaporation and the thermal protection construction for the instruments with intermediate characteristics.

  3. Structure and Properties of the Foreshock at Venus

    Science.gov (United States)

    Omidi, N.; Collinson, G.; Sibeck, D.

    2017-10-01

    The interaction of the solar wind with Venus is dominated by the planet's ionosphere that acts as an obstacle to the flow resulting in an induced magnetosphere and bow shock much smaller than their terrestrial counterparts. This study presents a 3-D electromagnetic hybrid (kinetic ions and fluid electrons) simulation of the solar wind interaction with an unmagnetized obstacle to examine the structure and properties of the Cytherean foreshock during periods of near radial IMF, that is, when it lies upstream of the ionosphere. The interaction between the backstreaming ions and the solar wind results in the generation of two classes of ULF waves: (1) parallel propagating sinusoidal waves with periods 20-30 s and (2) highly oblique fast magnetosonic waves. The joint nonlinear evolution of these waves results in the formation of structures called foreshock cavitons with dimensions comparable to the size of the planet. Foreshock cavitons are also present in the terrestrial foreshock. The excavation of plasma and magnetic field from their cores leads to lower average densities and magnetic field strengths in the foreshock. As in the case of Earth, this excavation results in the formation of a fast magnetosonic pulse/shock at the edge of the foreshock named the foreshock compressional boundary. Also similar to Earth is the formation of spontaneous hot flow anomalies (SHFAs) as foreshock cavitons approach the bow shock. The size and properties of SHFAs at Venus are comparable to those at Earth, and their existence has recently been established at Mars and Venus in a companion paper.

  4. Venus kinase receptors control reproduction in the platyhelminth parasite Schistosoma mansoni.

    Directory of Open Access Journals (Sweden)

    Mathieu Vanderstraete

    2014-05-01

    Full Text Available The Venus kinase receptor (VKR is a single transmembrane molecule composed of an intracellular tyrosine kinase domain close to that of insulin receptor and an extracellular Venus Flytrap (VFT structure similar to the ligand binding domain of many class C G protein coupled receptors. This receptor tyrosine kinase (RTK was first discovered in the platyhelminth parasite Schistosoma mansoni, then in a large variety of invertebrates. A single vkr gene is found in most genomes, except in S. mansoni in which two genes Smvkr1 and Smvkr2 exist. VKRs form a unique family of RTKs present only in invertebrates and their biological functions are still to be discovered. In this work, we show that SmVKRs are expressed in the reproductive organs of S. mansoni, particularly in the ovaries of female worms. By transcriptional analyses evidence was obtained that both SmVKRs fulfill different roles during oocyte maturation. Suppression of Smvkr expression by RNA interference induced spectacular morphological changes in female worms with a strong disorganization of the ovary, which was dominated by the presence of primary oocytes, and a defect of egg formation. Following expression in Xenopus oocytes, SmVKR1 and SmVKR2 receptors were shown to be activated by distinct ligands which are L-Arginine and calcium ions, respectively. Signalling analysis in Xenopus oocytes revealed the capacity of SmVKRs to activate the PI3K/Akt/p70S6K and Erk MAPK pathways involved in cellular growth and proliferation. Additionally, SmVKR1 induced phosphorylation of JNK (c-Jun N-terminal kinase. Activation of JNK by SmVKR1 was supported by the results of yeast two-hybrid experiments identifying several components of the JNK pathway as specific interacting partners of SmVKR1. In conclusion, these results demonstrate the functions of SmVKR in gametogenesis, and particularly in oogenesis and egg formation. By eliciting signalling pathways potentially involved in oocyte proliferation, growth

  5. WeaselBoard :

    Energy Technology Data Exchange (ETDEWEB)

    Mulder, John C.; Schwartz, Moses Daniel; Berg, Michael J.; Van Houten, Jonathan Roger; Urrea, Jorge Mario; King, Michael Aaron; Clements, Abraham Anthony; Jacob, Joshua A.

    2013-10-01

    Critical infrastructures, such as electrical power plants and oil refineries, rely on programmable logic controllers (PLCs) to control essential processes. State of the art security cannot detect attacks on PLCs at the hardware or firmware level. This renders critical infrastructure control systems vulnerable to costly and dangerous attacks. WeaselBoard is a PLC backplane analysis system that connects directly to the PLC backplane to capture backplane communications between modules. WeaselBoard forwards inter-module traffic to an external analysis system that detects changes to process control settings, sensor values, module configuration information, firmware updates, and process control program (logic) updates. WeaselBoard provides zero-day exploit detection for PLCs by detecting changes in the PLC and the process. This approach to PLC monitoring is protected under U.S. Patent Application 13/947,887.

  6. JOINT ADVISORY APPEALS BOARD

    CERN Multimedia

    Human Resources Division

    2001-01-01

    The Joint Advisory Appeals Board was convened to examine the appeal lodged by Mr Neil Calder, Mrs Sudeshna Datta Cockerill, Mrs Andrée Fontbonne, Mrs Moniek Laurent and Mr Ulrich Liptow with regard to membership in the Pension Fund under the period with a Paid Associate contract, appeals dealt with on a collective basis. As the appellants have not objected, the report of the Board and the final decision of the Director-General are brought to the notice of the personnel in accordance with Article R VI 1.20 of the Staff Regulations. The relevant documents will therefore be posted on the notice boards of the Administration Building (N° 60) from 10 to 31 August 2001.

  7. Pension Fund Governing Board

    CERN Multimedia

    HR Department

    2008-01-01

    Note The CERN pension scheme is based on the principle of defined benefits, so beneficiaries continue to receive the benefits to which they are entitled in accordance with the Rules of the Pension Fund. This means that pension entitlements under the Rules are not directly affected by the financial crisis and the current economic situation. However, the adjustment of pensions to the cost of living is not automatic and, under the method applied since 2006, must take into account the Fund’s financial position. Meeting of the Pension Fund Governing Board The Pension Fund Governing Board held its eighth meeting at ESO in Garching, Germany (near Munich) on 24 October 2008. Before starting its work, the Governing Board had the privilege of hearing an opening address by Professor Tim de Zeeuw, the Director General of ESO. Professor de Zeeuw described the mission of ESO and the ambitious projects of his organisation, which performs astronomy observations using telescopes located in...

  8. Importance of Including Topography in Numerical Simulations of Venus' Atmospheric Circulation

    Science.gov (United States)

    Parish, H. F.; Schubert, G.; Lebonnois, S.; Covey, C. C.; Walterscheid, R. L.; Grossman, A.

    2012-12-01

    Venus' atmosphere is characterized by strong superrotation, in which the wind velocities at cloud heights are around 60 times faster than the surface rotation rate. The reasons for this strong superrotation are still not well understood. Since the surface of the planet is both a source and sink of atmospheric angular momentum it is important to understand and properly account for the interactions at the surface-atmosphere boundary. A key aspect of the surface-atmosphere interaction is the topography. Topography has been introduced into different general circulation models (GCMs) of Venus' atmosphere, producing significant, but widely varying effects on the atmospheric circulation. The reasons for the inconsistencies among model results are not well known, but our studies suggest they might be related to the influences of different dynamical cores. In our recent study, we have analyzed the angular momentum budget for two Venus GCMs, the Venus Community Atmosphere model (Venus CAM) and the Laboratoire de Meteorologie Dynamique (LMD) Venus GCM. Because of Venus' low magnitude surface winds, surface friction alone supplies only a relatively weak angular momentum forcing to the atmosphere. We find that if surface friction is introduced without including surface topography, the angular momentum balance of the atmosphere may be dominated by effects such as numerical diffusion, a sponge layer, or other numerical residuals that are generally included in all GCMs, and can themselves be sources of angular momentum. However, we find the mountain torque associated with realistic Venus surface topography supplies a much larger source of angular momentum than the surface friction, and dominates nonphysical numerical terms. (A similar effect occurs for rapidly rotating planets like Earth, but in this case numerical errors in the angular momentum budget are relatively small even in the absence of mountain torque). Even if surface friction dominates numerical terms in the angular

  9. The Ancient Mariner and the transit of Venus.

    Science.gov (United States)

    Griffin-Short, Rita

    2003-12-01

    The achievements of William Wales FRS - astronomer, classical scholar, demographer, editor, mathematician, meteorologist and humane teacher - have been overshadowed by the fame of Cook's extraordinary voyages, and overlooked as a significant influence on Samuel Taylor Coleridge's early development. The Royal Society sent Wales to Hudson Bay, Canada, and James Cook to Tahiti, both to observe the 1769 transit of Venus as part of an international project to calculate solar parallax, and hence the distance to the Sun. Wales later taught mathematics and navigation science at Christ's Hospital School to a precocious Coleridge, whose creative mind translated tales of polar adventures into memorable poetry.

  10. Whistler Wave Propagation Through the Ionosphere of Venus

    Science.gov (United States)

    Pérez-Invernón, F. J.; Lehtinen, N. G.; Gordillo-Vázquez, F. J.; Luque, A.

    2017-11-01

    We investigate the attenuation of whistler waves generated by hypotetical Venusian lightning occurring at the altitude of the cloud layer under different ionospheric conditions. We use the Stanford full-wave method for stratified media of Lehtinen and Inan (2008) to model wave propagation through the ionosphere of Venus. This method calculates the electromagnetic field created by an arbitrary source in a plane-stratified medium (i.e., uniform in the horizontal direction). We see that the existence of holes in electronic densities and the magnetic field configuration caused by solar wind play an important role in the propagation of electromagnetic waves through the Venusian ionosphere.

  11. Sulfuric acid cloud interpretation of the infrared spectrum of Venus

    Science.gov (United States)

    Martonchik, J. V.

    1974-01-01

    Sulfuric acid single-cloud models are compared with the Venus spectrum in the 8-14 micron region. The results indicate that a cloud composed of a 75 percent H2SO4 solution and with a particle density of 100 per cu cm is in good agreement with observations. In addition to explaining the 11.2 micron absorption, this model also predicts an absorption feature at 16.7 microns which should be detectable if the observation is made from an aircraft.

  12. New Service Status Board

    CERN Multimedia

    2013-01-01

    On Monday 14 October, the Service Status Board for GS and IT will change. The new Status Board will be integrated with the CERN Service Portal and with the CERN Service Catalogue.   As of today, the SSB will display “Service Incidents”, “Planned Interventions” and “Service Changes”. References valid from 14 October: CERN SSB at https://cern.ch/ssb Computing SSB (previously IT SSB) at https://cern.ch/itssb   Nicole Cremel, IT and GS Service Management Support

  13. Joint Advisory Appeals Board

    CERN Multimedia

    2013-01-01

    The Joint Advisory Appeals Board has examined the internal appeal lodged by a former member of the personnel, a beneficiary of the CERN Pension Fund, against the calculation of his pension in the framework of the Progressive Retirement Programme.   The person concerned has not objected to the report of the Board and the final decision of the Director-General being brought to the attention of the members of the personnel. In application of Article R VI 1.18 of the Staff Regulations, these documents will therefore be available from 26 July to 11 August 2013 at the following link. HR Department Head Office

  14. Radiative energy balance of Venus based on improved models of the middle and lower atmosphere

    Science.gov (United States)

    Haus, R.; Kappel, D.; Tellmann, S.; Arnold, G.; Piccioni, G.; Drossart, P.; Häusler, B.

    2016-07-01

    The distribution of sources and sinks of radiative energy forces the atmospheric dynamics. The radiative transfer simulation model described by Haus et al. (2015b) is applied to calculate fluxes and temperature change rates in the middle and lower atmosphere of Venus (0-100 km) covering the energetic significant spectral range 0.125-1000 μm. The calculations rely on improved models of atmospheric parameters (temperature profiles, cloud parameters, trace gas abundances) retrieved from Venus Express (VEX) data (mainly VIRTIS-M-IR, but also VeRa and SPICAV/SOIR with respect to temperature results). The earlier observed pronounced sensitivity of the radiative energy balance of Venus to atmospheric parameter variations is confirmed, but present detailed comparative analyses of possible influence quantities ensure unprecedented insights into radiative forcing on Venus by contrast with former studies. Thermal radiation induced atmospheric cooling rates strongly depend on temperature structure and cloud composition, while heating rates are mainly sensitive to insolation conditions and UV absorber distribution. Cooling and heating rate responses to trace gas variations and cloud mode 1 abundance changes are small, but observed variations of cloud mode 2 abundances and altitude profiles reduce cooling at altitudes 65-80 km poleward of 50°S by up to 30% compared to the neglect of cloud parameter changes. Cooling rate variations with local time below 80 km are in the same order of magnitude. Radiative effects of the unknown UV absorber are modeled considering a proxy that is based on a suitable parameterization of optical properties, not on a specific chemical composition, and that is independent of the used cloud model. The UV absorber doubles equatorial heating near 68 km. Global average radiative equilibrium at the top of atmosphere (TOA) is characterized by the net flux balance of 156 W/m2, the Bond albedo of 0.76, and the effective planetary emission temperature of 228

  15. Venus-Earth-Mars: Comparative Climatology and the Search for Life in the Solar System

    Science.gov (United States)

    Launius, Roger D.

    2012-01-01

    Both Venus and Mars have captured the human imagination during the twentieth century as possible abodes of life. Venus had long enchanted humans—all the more so after astronomers realized it was shrouded in a mysterious cloak of clouds permanently hiding the surface from view. It was also the closest planet to Earth, with nearly the same size and surface gravity. These attributes brought myriad speculations about the nature of Venus, its climate, and the possibility of life existing there in some form. Mars also harbored interest as a place where life had or might still exist. Seasonal changes on Mars were interpreted as due to the possible spread and retreat of ice caps and lichen-like vegetation. A core element of this belief rested with the climatology of these two planets, as observed by astronomers, but these ideas were significantly altered, if not dashed during the space age. Missions to Venus and Mars revealed strikingly different worlds. The high temperatures and pressures found on Venus supported a “runaway greenhouse theory,” and Mars harbored an apparently lifeless landscape similar to the surface of the Moon. While hopes for Venus as an abode of life ended, the search for evidence of past life on Mars, possibly microbial, remains a central theme in space exploration. This survey explores the evolution of thinking about the climates of Venus and Mars as life-support systems, in comparison to Earth. PMID:25371106

  16. Venus-Earth-Mars: Comparative Climatology and the Search for Life in the Solar System

    Directory of Open Access Journals (Sweden)

    Roger D. Launius

    2012-09-01

    Full Text Available Both Venus and Mars have captured the human imagination during the twentieth century as possible abodes of life. Venus had long enchanted humans—all the more so after astronomers realized it was shrouded in a mysterious cloak of clouds permanently hiding the surface from view. It was also the closest planet to Earth, with nearly the same size and surface gravity. These attributes brought myriad speculations about the nature of Venus, its climate, and the possibility of life existing there in some form. Mars also harbored interest as a place where life had or might still exist. Seasonal changes on Mars were interpreted as due to the possible spread and retreat of ice caps and lichen-like vegetation. A core element of this belief rested with the climatology of these two planets, as observed by astronomers, but these ideas were significantly altered, if not dashed during the space age. Missions to Venus and Mars revealed strikingly different worlds. The high temperatures and pressures found on Venus supported a “runaway greenhouse theory,” and Mars harbored an apparently lifeless landscape similar to the surface of the Moon. While hopes for Venus as an abode of life ended, the search for evidence of past life on Mars, possibly microbial, remains a central theme in space exploration. This survey explores the evolution of thinking about the climates of Venus and Mars as life-support systems, in comparison to Earth.

  17. Venus-Earth-Mars: comparative climatology and the search for life in the solar system.

    Science.gov (United States)

    Launius, Roger D

    2012-09-19

    Both Venus and Mars have captured the human imagination during the twentieth century as possible abodes of life. Venus had long enchanted humans-all the more so after astronomers realized it was shrouded in a mysterious cloak of clouds permanently hiding the surface from view. It was also the closest planet to Earth, with nearly the same size and surface gravity. These attributes brought myriad speculations about the nature of Venus, its climate, and the possibility of life existing there in some form. Mars also harbored interest as a place where life had or might still exist. Seasonal changes on Mars were interpreted as due to the possible spread and retreat of ice caps and lichen-like vegetation. A core element of this belief rested with the climatology of these two planets, as observed by astronomers, but these ideas were significantly altered, if not dashed during the space age. Missions to Venus and Mars revealed strikingly different worlds. The high temperatures and pressures found on Venus supported a "runaway greenhouse theory," and Mars harbored an apparently lifeless landscape similar to the surface of the Moon. While hopes for Venus as an abode of life ended, the search for evidence of past life on Mars, possibly microbial, remains a central theme in space exploration. This survey explores the evolution of thinking about the climates of Venus and Mars as life-support systems, in comparison to Earth.

  18. Mission Architecture and Technology Options for a Flagship Class Venus In Situ Mission

    Science.gov (United States)

    Balint, Tibor S.; Kwok, Johnny H.; Kolawa, Elizabeth A.; Cutts, James A.; Senske, David A.

    2008-01-01

    Venus, as part of the inner triad with Earth and Mars, represents an important exploration target if we want to learn more about solar system formation and evolution. Comparative planetology could also elucidate the differences between the past, present, and future of these three planets, and can help with the characterization of potential habitable zones in our solar system and, by extension, extrasolar systems. A long lived in situ Venus mission concept, called the Venus Mobile Explorer, was prominently featured in NASA's 2006 SSE Roadmap and supported in the community White Paper by the Venus Exploration Analysis Group (VEXAG). Long-lived in situ missions are expected to belong to the largest (Flagship) mission class, which would require both enabling and enhancing technologies beside mission architecture options. Furthermore, extreme environment mitigation technologies for Venus are considered long lead development items and are expected to require technology development through a dedicated program. To better understand programmatic and technology needs and the motivating science behind them, in this fiscal year (FY08) NASA is funding a Venus Flaghip class mission study, based on key science and technology drivers identified by a NASA appointed Venus Science and Technology Definition Team (STDT). These mission drivers are then assembled around a suitable mission architecture to further refine technology and cost elements. In this paper we will discuss the connection between the final mission architecture and the connected technology drivers from this NASA funded study, which - if funded - could enable a future Flagship class Venus mission and potentially drive a proposed Venus technology development program.

  19. Theoretical study of the luminance distribution on the Venus disk

    International Nuclear Information System (INIS)

    Bigourd, C.; Deuze, J.L.; Devaux, C.; Herman, M.; Lenoble, J.

    1974-01-01

    The analysis of the sunlight scattered by Venus gives some insight upon its clouds. The measurements of polarized light are probably more sensitive to the nature of their constituents, and some recent studies seem to be able to give a satisfactory interpretation of this part of the scattered light. But the polarized light concerns the upper part of the clouds, and it is interesting to compare these with intensity measurements. The phase curves, for the integrated light, leave some indetermination, so we have studied if the intensity distribution on the Venus disk could give more accurate informations. This work based on some plates kindly communicated by A. Dolfus, and analysed at Meudon Observatory, is more a preliminary investigation of the sensitivity of the method than an interpretation of the partial results presented. A simple model, of homogeneous plane parallel cloud, has been used, and the influence of various parameters has been tested (single scattering albedo, refractive index of particles and size distribution, optical depth of the cloud). (Auth.)

  20. A POTENTIAL SUPER-VENUS IN THE KEPLER-69 SYSTEM

    International Nuclear Information System (INIS)

    Kane, Stephen R.; Gelino, Dawn M.; Barclay, Thomas

    2013-01-01

    Transiting planets have greatly expanded and diversified the exoplanet field. These planets provide greater access to characterization of exoplanet atmospheres and structure. The Kepler mission has been particularly successful in expanding the exoplanet inventory, even to planets smaller than the Earth. The orbital period sensitivity of the Kepler data is now extending into the habitable zones of their host stars, and several planets larger than the Earth have been found to lie therein. Here we examine one such proposed planet, Kepler-69c. We provide new orbital parameters for this planet and an in-depth analysis of the habitable zone. We find that, even under optimistic conditions, this 1.7 R ⊕ planet is unlikely to be within the habitable zone of Kepler-69. Furthermore, the planet receives an incident flux of 1.91 times the solar constant, which is similar to that received by Venus. We thus suggest that this planet is likely a super-Venus rather than a super-Earth in terms of atmospheric properties and habitability, and we propose follow-up observations to disentangle the ambiguity.

  1. Fluid outflows from Venus impact craters - Analysis from Magellan data

    Science.gov (United States)

    Asimow, Paul D.; Wood, John A.

    1992-01-01

    Many impact craters on Venus have unusual outflow features originating in or under the continuous ejecta blankets and continuing downhill into the surrounding terrain. These features clearly resulted from flow of low-viscosity fluids, but the identity of those fluids is not clear. In particular, it should not be assumed a priori that the fluid is an impact melt. A number of candidate processes by which impact events might generate the observed features are considered, and predictions are made concerning the rheological character of flows produce by each mechanism. A sample of outflows was analyzed using Magellan images and a model of unconstrained Bingham plastic flow on inclined planes, leading to estimates of viscosity and yield strength for the flow materials. It is argued that at least two different mechanisms have produced outflows on Venus: an erosive, channel-forming process and a depositional process. The erosive fluid is probably an impact melt, but the depositional fluid may consist of fluidized solid debris, vaporized material, and/or melt.

  2. Extreme Temperature Pulse Injection Position Sensor for Venus Environment

    Science.gov (United States)

    Ji, Jerri; Kumar, Nishant; Singh, Sase; Narine, Roop

    After developed two types of extreme temperature motors (Switched Reluctance Motor and Blushless DC Motor), Honeybee Robotics has successfully developed an Extreme Temperature Pulse Injection Position Sensor that can be used to commutate motors and provide positional information. This paper presents an insight into the challenges of designing extreme tempera-ture electro-mechanical system and provides results of the experiment performed in the Venus environment. The operational temperature range for existing commutation devices, include Hall Sensors, Resolvers and Encoders is limited to temperatures less than 180C. The Extreme Temperature Pulse Injection Position Sensor is capable of working continuously at 460C and at 92 atm. The design of this device involves a unique rotor design and an innovative phase pulsing algorithm implemented through a high speed DSP. The shape of the rotor provides a unique flow-path to the lines-of-flux through the poles of the stator. The pulsing algorithm makes it possible to nullify the effects of parametric changes (wire resistance, permeability, air gap, etc.) due to increase in temperature. The algorithm relies on the relative flux density between two stator poles rather than the absolute measurement of the flux density in each pole. Extreme temperature position sensor, along with scalable extreme temperature motor and gearhead allow for creation of robot arms and even mobility systems for future Venus missions to achieve their goals and objectives.

  3. Corona Formation and Heat Loss on Venus by Coupled Upwelling and Delamination

    Science.gov (United States)

    Smrekar, Suzanne E.; Stofan, Ellen R.

    1997-01-01

    Coronae are volcanotectonic features that are unique to Venus and are interpreted to be small-scale upwellings. A model in which upwelling causes delamination at the edge of the plume head, along with deformation of a pre-existing depleted mantel Layer, can produce the full range of topographic forms of coronae. If half of the coronae are active, delamination of the lower lithosphere could account for about 10% of venus's heat loss, with another 15% due to upwelling. Delamination may occur in other geologic enviroment and could help account for 'Venus' heat loss 'deficit'.

  4. Can a time-stratigraphic classification system be developed for Venus?

    Science.gov (United States)

    Tanaka, K. L.; Schaber, G. G.

    1992-01-01

    Magellan radar images reveal that Venus' exposed geologic record covers a relatively short and recent time span, as indicated by the low density of impact craters across the planet. Therefore, because impact cratering in itself will not be a useful tool to define geologic ages on Venus, it was questioned whether a useful stratigraphic scheme can be developed for the planet. We believe that a venusian stratigraphy is possible and that it can be based on the following: (1) an examination of the rationale and methods that have been used to develop such schemes for the other planets; and (2) what can be gleaned from Magellan and other datasets of Venus.

  5. Terrestrial spreading centers under Venus conditions - Evaluation of a crustal spreading model for Western Aphrodite Terra

    Science.gov (United States)

    Sotin, C.; Senske, D. A.; Head, J. W.; Parmentier, E. M.

    1989-01-01

    The model of Reid and Jackson (1981) for terrestrial spreading centers is applied to Venus conditions. On the basis of spreading rate, mantle temperature, and surface temperature, the model predicts both isostatic topography and crustal thickness. The model and Pioneer Venus altimetry and gravity data are used to test the hypothesis of Head and Crumpler (1987) that Western Aphrodite Terra is the location of crustal spreading on Venus. It is concluded that a spreading center model for Ovda Regio in Western Aphrodite Terra could account for the observed topography and line-of-sight gravity anomalies found in the Pioneer data.

  6. Oxygen ionization rates at Mars and Venus - Relative contributions of impact ionization and charge exchange

    Science.gov (United States)

    Zhang, M. H. G.; Luhmann, J. G.; Nagy, A. F.; Spreiter, J. R.; Stahara, S. S.

    1993-01-01

    Oxygen ion production rates above the ionopauses of Venus and Mars are calculated for photoionization, charge exchange, and solar wind electron impact ionization processes. The latter two require the use of the Spreiter and Stahara (1980) gas dynamic model to estimate magnetosheath velocities, densities, and temperatures. The results indicate that impact ionization is the dominant mechanism for the production of O(+) ions at both Venus and Mars. This finding might explain both the high ion escape rates measured by Phobos 2 and the greater mass loading rate inferred for Venus from the bow shock positions.

  7. DAVINCI: Deep Atmosphere Venus Investigation of Noble gases, Chemistry, and Imaging

    Science.gov (United States)

    Glaze, Lori S.; Garvin, James B.; Robertson, Brent; Johnson, Natasha M.; Amato, Michael J.; Thompson, Jessica; Goodloe, Colby; Everette, Dave

    2017-01-01

    DAVINCI is one of five Discovery-class missions selected by NASA in October 2015 for Phase A studies. Launching in November 2021 and arriving at Venus in June of 2023, DAVINCI would be the first U.S. entry probe to target Venus atmosphere in 45 years. DAVINCI is designed to study the chemical and isotopic composition of a complete cross-section of Venus atmosphere at a level of detail that has not been possible on earlier missions and to image the surface at optical wavelengths and process-relevant scales.

  8. Geologic map of the Rusalka Planitia Quadrangle (V-25), Venus

    Science.gov (United States)

    Young, Duncan A.; Hansen, Vicki L.

    2003-01-01

    The Rusalka Planitia quadrangle (herein referred to as V-25) occupies an 8.1 million square kilometer swath of lowlands nestled within the eastern highlands of Aphrodite Terra on Venus. The region (25?-0? N., 150?-180? E.) is framed by the crustal plateau Thetis Regio to the southwest, the coronae of the Diana-Dali chasmata complex to the south, and volcanic rise Atla Regio to the west. Regions to the north, and the quadrangle itself, are part of the vast lowlands, which cover four-fifths of the surface of Venus. The often-unspectacular lowlands of Venus are typically lumped together as ridged or regional plains. However, detailed mapping reveals the mode of resurfacing in V-25's lowlands: a mix of corona-related flow fields and local edifice clusters within planitia superimposed on a background of less clearly interpretable extended flow fields, large volcanoes, probable corona fragments, and edifice-flow complexes. The history detailed within the Rusalka Planitia quadrangle is that of the extended evolution of long-wavelength topographic basins in the presence of episodes of extensive corona-related volcanism, pervasive low-intensity small-scale eruptions, and an early phase of regional circumferential shortening centered on central Aphrodite Terra. Structural reactivation both obscures and illuminates the tectonic development of the region. The data are consistent with progressive lithospheric thickening, although the critical lack of an independent temporal marker on Venus severely hampers our ability to test this claim and correlate between localities. Two broad circular basins dominate V-25 geology: northern Rusalka Planitia lies in the southern half of the quadrangle, whereas the smaller Llorona Planitia sits along the northwestern corner of V-25. Similar large topographic basins occur throughout the lowlands of Venus, and gravity data suggest that some basins may represent dynamic topography over mantle downwellings. Both planitiae include coronae and

  9. Long term evolution of temperature in the venus upper atmosphere at the evening and morning terminators

    Science.gov (United States)

    Krause, P.; Sornig, M.; Wischnewski, C.; Kostiuk, T.; Livengood, T. A.; Herrmann, M.; Sonnabend, G.; Stangier, T.; Wiegand, M.; Pätzold, M.; Mahieux, A.; Vandaele, A. C.; Piccialli, A.; Montmessin, F.

    2018-01-01

    This paper contains a comprehensive dataset of long-term observations between 2009 and 2015 at the upper mesosphere/lower thermosphere providing temperature values at different locations of the morning and evening side of the terminator of Venus. Temperature information is obtained by line-resolved spectroscopy of Doppler broadened CO2 transitions features. Results are restricted to a pressure level of 1 μbar, ∼110 km altitude due the nature of the addressed non-LTE CO2 emission line at 10 μm. The required high spectral resolution of the instrumentation is provided by the ground-based spectrometers THIS (University of Cologne) and HIPWAC (NASA GSFC). For the first time upper mesosphere/lower thermosphere temperatures at the Venusian terminator derived from IR-het spectroscopy between 2009 and 2015 are investigated in order to clarify the local-time dependences, latitudinal dependences and the long-term trend. Measured temperatures were distributed in the range between 140 K and 240 K, with mean values equal to 199 K ± 17 K for the morning side of the terminator and 195 K ± 19 K for the evening side of the terminator. Within the uncertainty no difference between the averaged morning and evening terminator side temperature is found. In addition, no strong latitudinal dependency is observed at these near terminator local times. In contrast IR-het data from 2009 show a strong latitudinal dependency at noon, with a temperature difference of around 60 K between the equatorial and polar region (Sonnabend et al., 2012). Accord with the instruments of the Venus Express mission a northern-southern hemispherical symmetry is observed (Mahieux et al., 2012; Piccialli et al., 2015). The data shows no consistent long-term temperature trend throughout the six years of observation, but a variability in the order of tens of Kelvin for the different observing runs representing a time step of few month to two years. This is about the same order of magnitude as the variability

  10. Geologic Mapping of the Helen Planitia Quadrangle (V52), Venus: The First Results

    Science.gov (United States)

    López, I.; Hansen, V. L.

    2003-03-01

    Preliminary geologic mapping of the Helen Planitia Quadrangle (V52), Venus is in progress. This area allows the investigation of the transition between the mesolands of Eastern Parga Chasmata and the lowlands of Helen Planitia.

  11. Constraints A-Z for the Surface Evolution of Venus, and Proposed History

    Science.gov (United States)

    Hansen, V. L.

    2012-03-01

    This contribution summarizes constraints A through Z for surface evolution of Venus, as derived from geologic mapping and analysis from a wide range of studies. All viable resurfacing models must be able to accommodate each of these constraints.

  12. PVO VENUS ONMS BROWSE NEUTRAL DENSITY 12 SECOND V1.0

    Data.gov (United States)

    National Aeronautics and Space Administration — This data set was designed to determine the composition of the neutral thermosphere/exosphere of Venus. The term composition includes both the type of neutral gases...

  13. Harsh Environment Gas Sensor Array for Venus Atmospheric Measurements, Phase II

    Data.gov (United States)

    National Aeronautics and Space Administration — Makel Engineering and the Ohio State University propose to develop a harsh environment tolerant gas sensor array for atmospheric analysis in future Venus missions....

  14. Thermal Management System for Long-Lived Venus Landers, Phase I

    Data.gov (United States)

    National Aeronautics and Space Administration — Long-lived Venus landers require power and cooling. Heat from the roughly 64 General Purpose Heat Source (GPHS) modules must be delivered to the convertor with...

  15. Nonthermal escape of hydrogen and deuterium from Venus and implications for loss of water

    Science.gov (United States)

    Kumar, S.; Hunten, D. M.; Pollack, J. B.

    1983-01-01

    As the dominant nonthermal mechanism for the escape of hydrogen in past Venus atmospheres, the charge exchange of H(+) with H would have provided an escape flux close to the diffusion-limiting value for H-mixing ratios up to 0.002 at the homopause, which also marks the onset of hydrodynamic flow. Charge exchange therefore represents a viable mechanism through which Venus could have lost up to an earth-equivalent ocean of water from its atmosphere over geologic time. Present Venus atmosphere estimates are based on in situ Pioneer Venus mission measurements, and assumptions in the course of extrapolation to past atmospheres have been with respect to the nature of the bulge, circulation pattern, and ion temperature.

  16. Venus Interior Probe Using In-situ Power and Propulsion (VIP-INSPR), Phase II

    Data.gov (United States)

    National Aeronautics and Space Administration — Venus, despite being our closest neighboring planet, is under-explored due to its hostile environment. The atmosphere is composed primarily of CO2, with a 92 bar...

  17. Titan is to Earth's Hydrological Cycle what Venus is to its Greenhouse Effect

    Science.gov (United States)

    Lorenz, R. D.

    2012-06-01

    Titan serves as an extreme extrapolation of Earth's possible present trend toward more violent rainstorms interspersed by long droughts, much as Venus has acted as a bogeyman to illustrate the perils of enhanced greenhouse warming.

  18. Pension Fund Governing Board

    CERN Multimedia

    HR Department

    2008-01-01

    Note The CERN pension scheme is based on the principle of defined benefits, so beneficiaries continue to receive the benefits to which they are entitled in accordance with the Rules of the Pension Fund. This means that pension entitlements under the Rules are not directly affected by the financial crisis and the current economic situation. However, the adjustment of pensions to the cost of living is not automatic and, under the method applied since 2006, must take into account the Fund’s financial position. Meeting of the Pension Fund Governing Board The Pension Fund Governing Board held its eighth meeting at ESO in Garching (near Munich), Germany on 24 October 2008. Before starting its work, the Governing Board had the privilege of hearing an opening address by Professor Tim de Zeeuw, the Director General of ESO. Professor de Zeeuw described the mission of ESO and the ambitious projects of his organisation, which performs astronomy observations using telescopes located in Chile. The Director-General receiv...

  19. The result of Venus Orbit Insertion of Akatsuki on December 7th, 2015

    Science.gov (United States)

    Sugiyama, K. I.; Nakamura, M.; Imamura, T.; Ishii, N.; Abe, T.; Kawakatsu, Y.; Hirose, C.; Satoh, T.; Suzuki, M.; Ueno, M.; Yamazaki, A.; Iwagami, N.; Watanabe, S.; Taguchi, M.; Fukuhara, T.; Takahashi, Y.; Yamada, M.; Imai, M.; Ohtsuki, S.; Uemizu, K.; Hashimoto, G. L.; Takagi, M.; Matsuda, Y.; Ogohara, K.; Sato, N.; Kasaba, Y.; Kouyama, T.; Hirata, N.; Nakamura, R.; Yamamoto, Y.; Horinouchi, T.; Yamamoto, M.; Hayashi, Y. Y.; Nakatsuka, J.; Kashimura, H.; Sakanoi, T.; Ando, H.; Murakami, S. Y.; Sato, T.; Takagi, S.; Nakajima, K.; Peralta, J.; Lee, Y. J.

    2015-12-01

    Japan launched Venus Climate Orbiter 'Akatsuki' (JAXA's mission code name: PLANET-C) to observe the dynamics of the Venus atmosphere globally and clarify the mechanism of the atmospheric circulation. The launch was on May 21st , 2010 from the Tanegashima Space Center. The cruise to Venus was smooth, however, the first Venus Orbit Insertion (VOI) trial on December 7th, 2010 tuned out to be a failure. Later Akatsuki has been orbiting the sun. Fortunately we keep the spacecraft in a healthy condition and surprisingly we have found another chance to let this spacecraft to meet Venus in 2015. Next VOI trial will be done on December 7th, 2015 and we report the result of this operation at this AGU meeting. This mission is planed to answer the question described below. The radius of the Earth and Venus are almost the same. In addition the radiation from the sun is also almost the same. The climates of these planets, however, are much different. For example, the strong zonal wind is observed on Venus with the period of 4 days, where Venus rotates westward with the period of 243 days. The wind speed is about 100 m s-1. This is called super rotation. We will investigate from data from Akatsuki what attributes to the difference of the climates between Earth and Venus. AKATSUKI was designed for remote sensing from an equatorial, elliptical orbit to tract the atmospheric motion at different altitudes using 5 cameras (3xIR, UV, Visible) and by the radio occultation technique. The first VOI has failed due to a malfunction of the propulsion system. The check valve between the helium tank and the fuel tank was blocked by an unexpected salt formation during the cruising from the Earth to Venus. As a result the main engine (orbital maneuvering engine, OME) became oxidizer-rich and fuel-poor condition, which led to an abnormal combustion in the engine with high temperature, and finally the engine was broken. We decide to use RCS thrusters for Trajectory Control Maneuvers' (TCMs) and

  20. VERITAS: a Discovery-Class Venus Surface Geology and Geophysics Mission

    Science.gov (United States)

    Freeman, Anthony; Smrekar, Suzanne E.; Hensley, Scott; Wallace, Mark; Sotin, Christophe; Darrach, Murray; Xaypraseuth, Peter; Helbert, Joern; Mazarico, Erwan

    2016-01-01

    Our understanding of solar system evolution is limited by a great unanswered question: How Earthlike is Venus? We know that these "twin" planets formed with similar bulk composition and size. Yet the evolutionary path Venus followed has diverged from Earth's, in losing its surface water and becoming hotter than Mercury. What led to this? The answer has profound implications for how terrestrial planets become habitable and the potential for life in the universe.

  1. Long-Lived Venus Lander Conceptual Design: How To Keep It Cool

    Science.gov (United States)

    Dyson, Ridger W.; Schmitz, Paul C.; Penswick, L. Barry; Bruder, Geoffrey A.

    2009-01-01

    Surprisingly little is known about Venus, our neighboring sister planet in the solar system, due to the challenges of operating in its extremely hot, corrosive, and dense environment. For example, after over two dozen missions to the planet, the longest-lived lander was the Soviet Venera 13, and it only survived two hours on the surface. Several conceptual Venus mission studies have been formulated in the past two decades proposing lander architectures that potentially extend lander lifetime. Most recently, the Venus Science and Technology Definition Team (STDT) was commissioned by NASA to study a Venus Flagship Mission potentially launching in the 2020- 2025 time-frame; the reference lander of this study is designed to survive for only a few hours more than Venera 13 launched back in 1981! Since Cytherean mission planners lack a viable approach to a long-lived surface architecture, specific scientific objectives outlined in the National Science Foundation Decadal Survey and Venus Exploration Advisory Group final report cannot be completed. These include: mapping the mineralogy and composition of the surface on a planetary scale determining the age of various rock samples on Venus, searching for evidence of changes in interior dynamics (seismometry) and its impact on climate and many other key observations that benefit with time scales of at least a full Venus day (Le. daylight/night cycle). This report reviews those studies and recommends a hybrid lander architecture that can survive for at least one Venus day (243 Earth days) by incorporating selective Stirling multi-stage active cooling and hybrid thermoacoustic power.

  2. Venusians: the Planet Venus in the 18th-Century Extraterrestrial Life Debate

    Science.gov (United States)

    Duner, David

    2013-05-01

    In the seventeenth and eighteenth centuries it became possible to believe in the existence of life on other planets on scientific grounds. Once the Earth was no longer the center of the universe according to Copernicus, once Galileo had aimed his telescope at the Moon and found it a rough globe with mountains and seas, the assumption of life on other planets became much less far-fetched. In general there were no actual differences between Earth and Venus, since both planets orbited the Sun, were of similar size, and possessed mountains and an atmosphere. If there is life on Earth, one may ponder why it could not also exist on Venus. In the extraterrestrial life debate of the seventeenth and eighteenth centuries, the Moon, our closest celestial body, was the prime candidate for life on other worlds, although a number of scientists and scholars also speculated about life on Venus and on other planets, both within our solar system and beyond its frontiers. This chapter discusses the arguments for life on Venus and those scientific findings that were used to support them, which were based in particular on assumptions and claims that both mountains and an atmosphere had been found on Venus. The transits of Venus in the 1760s became especially important for the notion that life could thrive on Venus. Here, I detect two significant cognitive processes that were at work in the search for life on Venus, i.e., analogical reasoning and epistemic perception, while analogies and interpretations of sensory impressions based on prior knowledge played an important role in astrobiological theories.

  3. Aerosol properties in the upper haze of Venus from SPICAV IR data

    Science.gov (United States)

    Luginin, M.; Fedorova, A.; Belyaev, D.; Montmessin, F.; Wilquet, V.; Korablev, O.; Bertaux, J.-L.; Vandaele, A. C.

    2016-10-01

    SPICAV IR, a channel of the SPICAV/SOIR suite of instruments onboard Venus Express spacecraft measured spectra in nadir and solar occultation modes in the range of 0.65-1.7 μm. We report results from 222 solar occultations observed from May 2006 to November 2014. The vertical resolution of measurements varies from 1 to 25 km depending on the distance of the spacecraft to the limb of Venus. The vertical profiles of atmospheric extinction were obtained at 10 near-IR wavelengths in the altitude range from 70 to 95 km. This allowed us to derive microphysical properties of the mesospheric haze. The aerosol haze top is higher near the equator than near the pole. In the upper haze, the aerosol scale height is found to be 3.3 ± 0.7 km. Detached haze layers were detected at altitudes from 70 to 90 km. Particle size and number density profiles are retrieved from extinction coefficients using Mie scattering theory adopting H2SO4 refractive indices. Bimodal distribution of particles is consistent with data for some orbits with mean radius for mode 1 reff1 = 0.12 ± 0.03 μm and reff2 = 0.84 ± 0.16 μm for mode 2. Particle radii tend to cluster within occultation campaign and vary on the time scale of several months. The radius for the single mode case equals Reff = 0.54 ± 0.25 μm, and they are also 1.5-2 times smaller in the polar region (60°N-90°N) than in nonpolar regions (60°S-60°N). In bimodal case the number density profiles decrease smoothly for both modes, from ∼500 cm-3 at 75 km to ∼50 cm-3 at 90 km for mode 1, and from ∼1 cm-3 at 75 km to ∼0.1 cm-3 at 90 km for mode 2.

  4. Structural analysis of central and eastern Ovda Regio, Venus

    Science.gov (United States)

    Ghent, R. R.; Hansen, V. L.

    1997-03-01

    Ovda Regio is the largest of the Venusian crustal plateaus and lies in Western Aphrodite Terra, Venus. An understanding of the strain history of this region will provide a key to understanding the processes involved in the formation of Ovda Regio and of crustal plateaus in general. This paper reports on a detailed structural mapping and analysis of Ovda and implications for the tectonic evolution of Ovda and other crustal plateaus. The tectonic features of Ovda Regio were mapped using Magellan SAR images. The three major structures seen in Ovda Regio are folds, ribbons, and graben. The folds are interpreted to be contractional, and the graben and ribbons extensional. The strain history recorded in Ovda Regio involves early extension, followed by contraction, then later extension. This strain history is consistent with the formation of Ovda Regio by mantle upwelling.

  5. Venus' spectroscopic phase variation - Implications of the Mariner 10 photographs

    Science.gov (United States)

    Chamberlain, J. W.

    1975-01-01

    The recent ultraviolet photographs of Venus by Mariner 10 have shown an irregular cloud structure. There is an apparent tendency for clearing along a wide equatorial band more or less centered on the subsolar point. This synoptic picture is in marked contrast to the uniform cloud cover conventionally used in model calculations of the variation with phase of CO2 absorption bands. To illustrate the consequences of subsolar weakening of CO2 absorption, a mathematically simple (but realistically naive) model is used. Two conclusions are reached: (1) efforts to distinguish between single- and double-layer models for the clouds from spectroscopic data alone are not merely ambiguous (as argued earlier by Chamberlain and Smith); with present data they are hopeless; (2) the decrease in the CO2 absorption close to full phase, as reported by Young et al., could result entirely from an equatorial darkening that is relatively inconsequential at the crescent phase and increasingly predominant for fuller phases.

  6. "Chiriguano" Astronomy - Venus and a Guarani New Year

    Science.gov (United States)

    Pereira, Gonzalo

    A Supreme Decree emitted by the government of Bolivia instituted the celebration of the June solstices in view of the fact that the indigenous people, both the Andean highlands and the Amazon and Chaco, "have commemorated this event for thousands of years" (Gobierno del Estado Plurinacional de Bolivia, Decreto Supremo N° 0173, June16, 2009, La Paz). In the case of the lowlands' indigenous, particularly the Guarani people, the decree mentions the planet Venus as the argument for this celebration. In this case of study and in light of astronomical and ethnographic evidence, we analyze the relevance of this decree in the case of the Guarani people of the Bolivian Chaco region, known as "Chiriguanos".

  7. Venus atmosphere profile from a maximum entropy principle

    Directory of Open Access Journals (Sweden)

    L. N. Epele

    2007-10-01

    Full Text Available The variational method with constraints recently developed by Verkley and Gerkema to describe maximum-entropy atmospheric profiles is generalized to ideal gases but with temperature-dependent specific heats. In so doing, an extended and non standard potential temperature is introduced that is well suited for tackling the problem under consideration. This new formalism is successfully applied to the atmosphere of Venus. Three well defined regions emerge in this atmosphere up to a height of 100 km from the surface: the lowest one up to about 35 km is adiabatic, a transition layer located at the height of the cloud deck and finally a third region which is practically isothermal.

  8. Clementine Observes the Moon, Solar Corona, and Venus

    Science.gov (United States)

    1997-01-01

    In 1994, during its flight, the Clementine spacecraft returned images of the Moon. In addition to the geologic mapping cameras, the Clementine spacecraft also carried two Star Tracker cameras for navigation. These lightweight (0.3 kg) cameras kept the spacecraft on track by constantly observing the positions of stars, reminiscent of the age-old seafaring tradition of sextant/star navigation. These navigation cameras were also to take some spectacular wide angle images of the Moon.In this picture the Moon is seen illuminated solely by light reflected from the Earth--Earthshine! The bright glow on the lunar horizon is caused by light from the solar corona; the sun is just behind the lunar limb. Caught in this image is the planet Venus at the top of the frame.

  9. Comparative kinematical analyses of Venus flytrap (Dionaea muscipula snap traps

    Directory of Open Access Journals (Sweden)

    Simon Poppinga

    2016-05-01

    Full Text Available Although the Venus flytrap (Dionaea muscipula can be considered as one of the most extensively investigated carnivorous plants, knowledge is still scarce about diversity of the snap-trap motion, the functionality of snap traps under varying environmental conditions, and their opening motion. By conducting simple snap-trap closure experiments in air and under water, we present striking evidence that adult Dionaea snaps similarly fast in aerial and submersed states and, hence, is potentially able to gain nutrients from fast aquatic prey during seasonal inundation. We reveal three snapping modes of adult traps, all incorporating snap buckling, and show that millimeter-sized, much slower seedling traps do not yet incorporate such elastic instabilities. Moreover, opening kinematics of young and adult Dionaea snap traps reveal that reverse snap buckling is not performed, corroborating the assumption that growth takes place on certain trap lobe regions. Our findings are discussed in an evolutionary, biomechanical, functional–morphological and biomimetic context.

  10. Patients overwhelmingly prefer inpatient boarding to emergency department boarding.

    Science.gov (United States)

    Viccellio, Peter; Zito, Joseph A; Sayage, Valerie; Chohan, Jasmine; Garra, Gregory; Santora, Carolyn; Singer, Adam J

    2013-12-01

    Boarding of admitted patients in the emergency department (ED) is a major cause of crowding. One alternative to boarding in the ED, a full-capacity protocol where boarded patients are redeployed to inpatient units, can reduce crowding and improve overall flow. Our aim was to compare patient satisfaction with boarding in the ED vs. inpatient hallways. We performed a structured telephone survey regarding patient experiences and preferences for boarding among admitted ED patients who experienced boarding in the ED hallway and then were subsequently transferred to inpatient hallways. Demographic and clinical characteristics, as well as patient preferences, including items related to patient comfort and safety using a 5-point scale, were recorded and descriptive statistics were used to summarize the data. Of 110 patients contacted, 105 consented to participate. Mean age was 57 ± 16 years and 52% were female. All patients were initially boarded in the ED in a hallway before their transfer to an inpatient hallway bed. The overall preferred location after admission was the inpatient hallway in 85% (95% confidence interval 75-90) of respondents. In comparing ED vs. inpatient hallway boarding, the following percentages of respondents preferred inpatient boarding with regard to the following 8 items: rest, 85%; safety, 83%; confidentiality, 82%; treatment, 78%; comfort, 79%; quiet, 84%; staff availability, 84%; and privacy, 84%. For no item was there a preference for boarding in the ED. Patients overwhelmingly preferred the inpatient hallway rather than the ED hallway when admitted to the hospital. Copyright © 2013 Elsevier Inc. All rights reserved.

  11. The Governing Board of the Pension Fund

    CERN Multimedia

    2007-01-01

    The Governing Board of the Pension Fund held its 151st meeting on 7 March at which the Legal Service reported on the ILOAT's judgment concerning an appeal lodged by a beneficiary against the CERN Council's decision to index his pension by 0% for 2005. The Governing Board noted with satisfaction that the appeal had been rejected. The ILOAT recognised that the CERN Council, which had followed the Governing Board's recommendation, had been entitled to take this decision as an 'urgent protective measure' in respect of the Fund's financial position. At the same meeting, the members of the Governing Board expressed their opinions on the report by the consultancy firm Mercer which had been entrusted with the task of comparing the CERN Pension Fund with a sample of similar European funds. It endorsed the CERN Management's opinion that Mercer had not been in a position to make a pertinent comparison between the CERN Pension Fund and other pension funds, and concurred with the conclusions presented by the Management....

  12. Magellan radio occultation measurements of atmospheric waves on Venus

    Science.gov (United States)

    Hinson, David P.; Jenkins, J. M.

    1995-01-01

    Radio occultation experiments were conducted at Venus on three consecutive orbits of the Magellan spacecraft in October 1991. Each occultation occurred over the same topography (67 deg N, 127 deg E) and at the same local time (22 hr 5 min), but the data are sensitive to zonal variations because the atmosphere rotates significantly during one orbit. Through comparisons between observations and predictions of standard wave theory, we have demonstrated that small-scale oscillations in retrieved temperature profiles as well as scintillations in received signal intensity are caused by a spectrum of vertically propagating internal gravity waves. There is a strong similarity between the intensity scintillations observed here and previous measurements, which pertain to a wide range of locations and experiment dates. This implies that the same basic phenomenon underlies all the observations and hence that gravity waves are a persistent, global feature of Venus' atmosphere. We obtained a fairly complete characterization of a gravity wave that appears above the middle cloud in temperature measurements on all three orbits. The amplitude and vertical wavelength are about 4 K and 2.5 km respectively, at 65 km. A model for radiative damping implies that the wave intrinsic frequency is approximately 2 x 10(exp 4) rad/sec, the corresponding ratio between horizontal and vertical wavelengths is approximately 100. The wave is nearly stationary relative to the surface or the Sun. Radiative attenuation limits the wave amplitude at altitudes above approximately 65 km, leading to wave drag on the mean zonal winds of about +0.4 m/sec per day (eastward). The sign, magnitude, and location of this forcing suggest a possible role in explaining the decrease with height in the zonal wind speed that is believed to occur above the cloud tops. Temperature oscillations with larger vertical wavelengths (5-10 km) were also observed on all three orbits, but we are able unable to interpret these

  13. An Atmospheric Variability Model for Venus Aerobraking Missions

    Science.gov (United States)

    Tolson, Robert T.; Prince, Jill L. H.; Konopliv, Alexander A.

    2013-01-01

    Aerobraking has proven to be an enabling technology for planetary missions to Mars and has been proposed to enable low cost missions to Venus. Aerobraking saves a significant amount of propulsion fuel mass by exploiting atmospheric drag to reduce the eccentricity of the initial orbit. The solar arrays have been used as the primary drag surface and only minor modifications have been made in the vehicle design to accommodate the relatively modest aerothermal loads. However, if atmospheric density is highly variable from orbit to orbit, the mission must either accept higher aerothermal risk, a slower pace for aerobraking, or a tighter corridor likely with increased propulsive cost. Hence, knowledge of atmospheric variability is of great interest for the design of aerobraking missions. The first planetary aerobraking was at Venus during the Magellan mission. After the primary Magellan science mission was completed, aerobraking was used to provide a more circular orbit to enhance gravity field recovery. Magellan aerobraking took place between local solar times of 1100 and 1800 hrs, and it was found that the Venusian atmospheric density during the aerobraking phase had less than 10% 1 sigma orbit to orbit variability. On the other hand, at some latitudes and seasons, Martian variability can be as high as 40% 1 sigmaFrom both the MGN and PVO mission it was known that the atmosphere, above aerobraking altitudes, showed greater variability at night, but this variability was never quantified in a systematic manner. This paper proposes a model for atmospheric variability that can be used for aerobraking mission design until more complete data sets become available.

  14. The photochemical stability of the Venus atmosphere against UV radiation

    International Nuclear Information System (INIS)

    Mills, F.P.; Slanger, T.G.; Allen, M.

    2004-01-01

    Full text: One unresolved question regarding the Venus atmosphere is what chemical mechanism(s) stabilize its primary constituent (CO 2 ) against UV radiation. CO 2 photolyzes on the day side into CO and O after absorbing photons at 2 rather than recombining with CO to form CO 2 , and the intense night side O 2 airglow observed quantitatively supports this. CO and O 2 are photochemically stable in an otherwise pure CO 2 atmosphere so significant abundances of CO and O 2 could accumulate on Venus if no catalytic mechanism existed to speed the reformation of CO 2 . However, the observational upper limit on ground state O 2 is equivalent to 2 from CO and O 2 . Recent laboratory work verified the existence of the ClC(O)OO catalytic mechanism that has been used in photochemical models since the early 1980s. However, there are significant uncertainties in the rates for the component steps of this catalytic mechanism. An alternative mechanism for production of CO 2 that has not previously been modeled but which could be competitive with the ClCO(O)O mechanism is the reaction CO + O 2 (c 1 Σ - u ) → CO 2 + O( 1 D) or O( 1 S), Reaction (1). A range of values for Reaction (1) will be examined in model calculations to compare with observational (UV to IR) constraints and to assess under what conditions this mechanism is competitive with the ClC(O)OO catalytic mechanism. The sensitivity of the results to uncertainties in the CO 2 UV absorption cross section also will be examined

  15. Reliability of the Wii Balance Board in kayak.

    Science.gov (United States)

    Vando, Stefano; Laffaye, Guillaume; Masala, Daniele; Falese, Lavinia; Padulo, Johnny

    2015-01-01

    the seat of the kayaker represent the principal contact point to express mechanical Energy. therefore we investigated the reliability of the Wii Balance Board measures in the kayak vs. on the ground. Bland-Altman test showed a low systematic bias on the ground (2.85%) and in kayak (-2.13%) respectively; while 0.996 for Intra-class correlation coefficient. the Wii Balance Board is useful to assess postural sway in kayak.

  16. Withdrawal Strength of Dowels in Plywood and Oriented Strand Board

    OpenAIRE

    ERDİL, Yusuf Z.; ECKELMAN, Carl A.

    2001-01-01

    Plywood and oriented strand board (OSB) are being used increasingly in the construction of upholstered furniture frames. Yet there is little information available concerning the holding strength of various fasteners, and, in particular, dowels in these materials. A study was conducted accordingly, to obtain basic information about the holding strength of dowels in both plywood and oriented strand board. Results of the tests were incorporated into predictive expressions that allow designers to...

  17. Aplikasi Dua Segitiga Sebangun pada Studi Venus Transit di Matahari Tanggal 8 Juni 2004 dari BPD LAPAN Watukosek

    Directory of Open Access Journals (Sweden)

    Nanang Widodo

    2013-11-01

    Full Text Available Transit planet Venus di cakram matahari (jari-jari = 696000 km merupakan peristiwa alam yang dapat dilihat secara berkala. Planet Venus merupakan planet kedua dalam sistem tata surya yang mempunyai orbit lebih dekat ke matahari (= 0,723 Astronomical Unit dibanding jarak bumi-matahari (= 149.600.000 km = 1 AU. Sehingga pada suatu waktu tertentu ada peluang berada tepat di depan Bumi, saat menghadap matahari atau dikenal dengan transit Venus. Proses pengamatan fenomena transit Venus di cakram matahari tersebut dapat diimplimentasikan sebagai aplikasi dua segitiga sebangun, Dimana jari-jari planet Venus (jari-jari = 6051,8 km dinyatakan sebagai tinggi benda dan jari-jari tinggi bayangan Venus sebesar 20880 km (= 3,65 mm pada cakram matahari. Dimana diameter matahari 1.392.000 km (= 240 mm pada lembar sket. Dengan pengukuran jarak tempuh Venus transit 72,4 mm (419 920 km di cakram matahari terhadap waktu kontak pertama bayangan Venus pada jam 05.28 UT (12.28 WIB di tepi timur hingga akhir transit pada 17.50 UT (14.50 WIB diperoleh kecepatan bayangan Venus sebesar 49,286 km/detik

  18. What makes great boards great.

    Science.gov (United States)

    Sonnenfeld, Jeffrey A

    2002-09-01

    In the wake of meltdowns at WorldCom, Tyco, and Enron, enormous attention has been focused on the companies' boards. It seems inconceivable that business disasters of such magnitude could happen without gross or even criminal negligence on the part of board members. And yet a close examination of those boards reveals no broad pattern of incompetence or corruption. In fact, they followed most of the accepted standards for board operations: Members showed up for meetings; they had money invested in the company; audit committees, compensation committees, and codes of ethics were in place; the boards weren't too small or too big, nor were they dominated by insiders. In other words, they passed the tests that would normally be applied to determine whether a board of directors was likely to do a good job. And that's precisely what's so scary, according to corporate governance expert Jeffrey Sonnenfeld, who suggests that it's time for some new thinking about how corporate boards operate and are evaluated. He proposes thinking not only about how to structure the board's work but also about how to manage it as a social system. Good boards are, very simply, high-functioning work groups. They're distinguished by a climate of respect, trust, and candor among board members and between the board and management. Information is shared openly and on time; emergent political factions are quickly eliminated. Members feel free to challenge one another's assumptions and conclusions, and management encourages lively discussion of strategic issues. Directors feel a responsibility to contribute meaningfully to the board's performance. In addition, good boards assess their own performance, both collectively and individually.

  19. Mean winds at the cloud top of Venus obtained from two-wavelength UV imaging by Akatsuki

    Science.gov (United States)

    Horinouchi, Takeshi; Kouyama, Toru; Lee, Yeon Joo; Murakami, Shin-ya; Ogohara, Kazunori; Takagi, Masahiro; Imamura, Takeshi; Nakajima, Kensuke; Peralta, Javier; Yamazaki, Atsushi; Yamada, Manabu; Watanabe, Shigeto

    2018-01-01

    Venus is covered with thick clouds. Ultraviolet (UV) images at 0.3-0.4 microns show detailed cloud features at the cloud-top level at about 70 km, which are created by an unknown UV-absorbing substance. Images acquired in this wavelength range have traditionally been used to measure winds at the cloud top. In this study, we report low-latitude winds obtained from the images taken by the UV imager, UVI, onboard the Akatsuki orbiter from December 2015 to March 2017. UVI provides images with two filters centered at 365 and 283 nm. While the 365-nm images enable continuation of traditional Venus observations, the 283-nm images visualize cloud features at an SO2 absorption band, which is novel. We used a sophisticated automated cloud-tracking method and thorough quality control to estimate winds with high precision. Horizontal winds obtained from the 283-nm images are generally similar to those from the 365-nm images, but in many cases, westward winds from the former are faster than the latter by a few m/s. From previous studies, one can argue that the 283-nm images likely reflect cloud features at higher altitude than the 365-nm images. If this is the case, the superrotation of the Venusian atmosphere generally increases with height at the cloud-top level, where it has been thought to roughly peak. The mean winds obtained from the 365-nm images exhibit local time dependence consistent with known tidal features. Mean zonal winds exhibit asymmetry with respect to the equator in the latter half of the analysis period, significantly at 365 nm and weakly at 283 nm. This contrast indicates that the relative altitude may vary with time and latitude, and so are the observed altitudes. In contrast, mean meridional winds do not exhibit much long-term variability. A previous study suggested that the geographic distribution of temporal mean zonal winds obtained from UV images from the Venus Express orbiter during 2006-2012 can be interpreted as forced by topographically induced

  20. First AGU Board of Directors

    Science.gov (United States)

    McPhaden, Michael J.

    2010-08-01

    On 1 July 2010, the first AGU Board of Directors took office. The board is composed of the president, president-elect, immediate past president, general secretary, international secretary, development board chair, six members elected by the Union membership, vice chair of the AGU Council, and the executive director. Two additional members may be nominated by the AGU president and approved by the board. The creation of the board is a result of the new governance structure approved by the AGU membership in November 2009. The board is responsible for the business aspects of the Union, while an expanded AGU Council will focus on science issues. Council members will be introduced in a future issue of Eos.

  1. Currency Boards; The Ultimate Fix?

    OpenAIRE

    Atish R. Ghosh

    1998-01-01

    The growing integration of world capital markets has made it fashionable to argue that only extreme exchange rate regimes are sustainable. Short of adopting a common currency, currency board arrangements represent the most extreme form of exchange rate peg. This paper compares the macroeconomic performance of countries with currency boards to those with other forms of pegged exchange rate regime. Currency boards are indeed associated with better inflation performance, even allowing for potent...

  2. Static Board evaluation on Go

    OpenAIRE

    STRIHAGEN,, KARL; HEDENCRONA, DANIEL

    2014-01-01

    Computers are still not outperforming professional go-players because of several complex aspects of the game. A common feature of computerised board-game players is that they needs a estimated value of how good or bad a given board is for one of the players. In this report we evaluate some trivial board-evaluation algorithms for the go board in how accurate they are to the outcome of the whole go-match.To our disappointment but also not unexpected very simple heuristic methods don't show any ...

  3. German versus Nordic Board Models

    DEFF Research Database (Denmark)

    Ringe, Georg

    2016-01-01

    changes and developments in business practice, the article argues that board practices in the two systems effectively blur the structural distinction, and that board organization is converging in practice. It thereby contributes to the broader debates on functionality and comparative corporate law......Board structure is an important component of the individual governance of firms, and the appropriateness of the various models is one of the most debated issues in corporate governance today. A comparison of the Nordic and German approaches to the structure of corporate boards reveals stark...

  4. Pension Fund governing board

    CERN Multimedia

    HR Department

    2008-01-01

    On 16 March and 7 May, the Pension Fund Governing Board (PFGB) held its fourth and fifth meetings The first of these meetings was primarily dedicated to the examination of the strategic asset allocation. The PFGB reaffirmed the main goal of the new strategic asset allocation: to improve the Pension Fund’s position with regard to risk by lowering overall portfolio volatility through suitable investments in less volatile asset classes such as real estate and absolute return strategies, where the return does not depend on market trends and negative growth is extremely unlikely. The finalised document will be presented to the Finance Committee and the Council at their June meetings for approval, in accordance with the provisions of the Levaux report. The PFGB also took note of the Internal Audit’s report on Pension Fund operations and decided to refer it to Working Group I as a working document for establishing a control and internal monitoring system for Pension Fund oper...

  5. Life in the Clouds of Venus? An Experimental Synthetic Biology Approach

    Science.gov (United States)

    Rothschild, L. J.; Paulino-Lima, I. G.; Amatya, D.; Bajar, B.; Geilich, B.; Hu, J.; Jackson, C. J.

    2015-01-01

    The surface of Venus constitutes the most hellish and biologically inhospitable planetary surface in our solar system, boasting a pH of 0, blistering winds that can melt lead, and pressures of 60 atm. However, during the earlier years of the solar system, without the runaway greenhouse effect that has plagued the planet, Venus potentially housed oceans and perhaps even life. There is a possibility that microbes could have retreated into hospitable niches in the atmosphere, as suggested by Carl Sagan as early as 1967 [1]. For example, 50 km above the raging hell of the Venusian surface, exists a relatively temperate environment that might serve as reservoir for life. This astrobiology project seeks to explore life at the extremes and to theorize whether microbial communities could not only survive but also reproduce in the Venusian atmosphere. Specifically, we ask: are aerosols viable microbial environments? But before we can test for life in the clouds, we have to develop a proper reporter to visualize cell growth in situ. For this purpose, we aimed to develop cell-growth dependent reporters to serve as remote biosensors for cell growth. We developed two using the polA promoter, a DNA-replication dependent promoter, and nrd operon promoter, a cell-cycle dependent promoter. Using these cell-growth reporters, the next step is to aerosolize microbes expressing these reporters in a suspension chamber adapted from a Millikan Drop Apparatus to assay reproduction in an aerosolized environment. Better yet is to test the reproduction of microbes in a microgravity regime such as on ISS.Approach: We engineered two cell-cycle dependent genetic reporters. One was the polA promoter which codes for DNA Polymerase I, a gene active in DNA replication [2]. The other was the nrdP. The activation of ribonucleotide reductase reduces ribonucleotides into deoxyribonucleotides and is involved in the bacterial cell cycle [3]. This promoter began activation during the initiation of DNA

  6. Thermal and magmatic processes on Venus, Earth, and Mars

    Science.gov (United States)

    Hauck, Steven Arthur, II

    Venus, Mars, and Earth present unique opportunities and laboratories for studying the thermal and magmatic evolution of terrestrial planets. Key observations from the Magellan mission to Venus were that the surface hosts a mere ˜1000 impact craters and that more than 65% of the surface is covered by volcanic plains. A popular hypothesis suggested the plains were emplaced in 10--100 Myr. However, analysis of the population of impact craters with respect to plains geology suggests that magmatism associated with plains emplacement lasted approximately half the average surface age of the planet, almost 500 Myr. Martian thermo-magmatic evolution is constrained by estimates that the crust was predominantly emplaced within the first 500 Myr, has an average crustal thickness of 50--100 km, and observations that imply that the planet had an internally generated magnetic field early, but is lacking one today. Coupling of a simple, parameterized model of mantle convection to a batch-melting model for peridotite allows reconstruction of reasonable estimates of the conditions and evolutionary path of the crust and mantle. Key elements of the nominal model are inclusion of the energetics of melting, a wet (weak) mantle rheology, self-consistent fractionation of heat producing elements to the crust, a near chondritic abundance of those same elements, and a core with 15 wt% sulfur. Inclusion of the latent heat of melting mantle material is crucial for constraining thermal and magmatic history of Mars. The nominal model results in an average crustal thickness of 67 km that was 75% emplaced by 4 Ga. The subduction of terrestrial oceanic lithosphere is an important heat transfer process related to plate tectonics. The source of deep focus earthquakes may be tied to the thermal structure of downgoing slabs and the potential for catastrophic transformation of metastable olivine below the 410 km discontinuity. The first models of subducting slabs that include thermal conductivity that

  7. Hot climate inhibits volcanism on Venus: Constraints from rock deformation experiments and argon isotope geochemistry

    Science.gov (United States)

    Mikhail, Sami; Heap, Michael J.

    2017-07-01

    The disparate evolution of sibling planets Earth and Venus has left them markedly different. Venus' hot (460 °C) surface is dry and has a hypsometry with a very low standard deviation, whereas Earth's average temperature is 4 °C and the surface is wet and has a pronounced bimodal hypsometry. Counterintuitively, despite the hot Venusian climate, the rate of intraplate volcano formation is an order of magnitude lower than that of Earth. Here we compile and analyse rock deformation and atmospheric argon isotope data to offer an explanation for the relative contrast in volcanic flux between Earth and Venus. By collating high-temperature, high-pressure rock deformation data for basalt, we provide a failure mechanism map to assess the depth of the brittle-ductile transition (BDT). These data suggest that the Venusian BDT likely exists between 2 and 12 km depth (for a range of thermal gradients), in stark contrast to the BDT for Earth, which we find to be at a depth of ∼25-27 km using the same method. The implications for planetary evolution are twofold. First, downflexing and sagging will result in the sinking of high-relief structures, due to the low flexural rigidity of the predominantly ductile Venusian crust, offering an explanation for the curious coronae features on the Venusian surface. Second, magma delivery to the surface-the most efficient mechanism for which is flow along fractures (dykes; i.e., brittle deformation)-will be inhibited on Venus. Instead, we infer that magmas must stall and pond in the ductile Venusian crust. If true, a greater proportion of magmatism on Venus should result in intrusion rather than extrusion, relative to Earth. This predicted lower volcanic flux on Venus, relative to Earth, is supported by atmospheric argon isotope data: we argue here that the anomalously unradiogenic present-day atmospheric 40Ar/36Ar ratio for Venus (compared with Earth) must reflect major differences in 40Ar degassing, primarily driven by volcanism. Indeed

  8. Divergent Evolution Among Earth-like Planets: The Case for Venus Exploration

    Science.gov (United States)

    Crisp, D.; Allen, M. A.; Anicich, V. G.; Arvidson, R. E.; Atreya, S. K.; Baines, K. H.; Banerdt, W. B.; Bjoraker, G. L.; Bougher, S. W.; Campbell, B. A.; Carlson, R. W.; Chin, G.; Chutjian, A.; Clancy, R. T.; Clark, B. C.; Cravens, T. E.; del Genio, A. D.; Esposito, L. W.; Fegley, B.; Flasar, M.; Fox, J. L.; Gierasch, P. J.; Goody, R. M.; Grinspoon, D. H.; Gulkis, S.; Hansen, V. L.; Herrick, R. R.; Huestis, D. L.; Hunten, D. M.; Janssen, M. A.; Jenkins, J.; Johnson, C. L.; Keating, G. M.; Kliore, A. J.; Limaye, S. S.; Luhmann, J. G.; Lunine, J. I.; Mahaffy, P.; McGovern, P. J.; Meadows, V. S.; Mills, F. P.; Niemann, H. B.; Owen, T. C.; Oyama, K. I.; Pepin, R. O.; Plaut, J. J.; Reuter, D. C.; Richardson, M. I.; Russell, C. T.; Saunders, R. S.; Schofield, J. T.; Schubert, G.; Senske, D. A.; Shepard, M. K.; Slanger, T. G.; Smrekar, S. E.; Stevenson, D. J.; Titov, D. V.; Ustinov, E. A.; Young, R. E.; Yung, Y. L.

    2002-08-01

    The planet Venus is our most Earth-like neighbor in size, mass, and distance from the sun. In spite of these similarities, and the intense scrutiny that it received early in the space age, the Venus surface and atmosphere are characterized by some of the most enigmatic features seen anywhere in the solar system. A reinvigorated Venus exploration program is essential to the development of a comprehensive understanding of the origin and evolution of Earth-like terrestrial planets. The present NASA inner planets strategy, which focuses exclusively on Mars, will provide an incomplete, and possibly misleading description of processes that produce these objects. If Venus-like terrestrial planets are common, this approach will also impede efforts to interpret observations of extrasolar terrestrial planets, which are expected to become available by the end of the decade. Here, we propose a Venus exploration program that has been designed to explain the origin and divergent evolution of the interiors, surfaces, and atmospheres of the terrestrial planets in our solar system, and provide greater insight into the conditions that may affect the habitability of terrestrial planets in other solar systems.

  9. Prolonged silicon carbide integrated circuit operation in Venus surface atmospheric conditions

    Directory of Open Access Journals (Sweden)

    Philip G. Neudeck

    2016-12-01

    Full Text Available The prolonged operation of semiconductor integrated circuits (ICs needed for long-duration exploration of the surface of Venus has proven insurmountably challenging to date due to the ∼ 460 °C, ∼ 9.4 MPa caustic environment. Past and planned Venus landers have been limited to a few hours of surface operation, even when IC electronics needed for basic lander operation are protected with heavily cumbersome pressure vessels and cooling measures. Here we demonstrate vastly longer (weeks electrical operation of two silicon carbide (4H-SiC junction field effect transistor (JFET ring oscillator ICs tested with chips directly exposed (no cooling and no protective chip packaging to a high-fidelity physical and chemical reproduction of Venus’ surface atmosphere. This represents more than 100-fold extension of demonstrated Venus environment electronics durability. With further technology maturation, such SiC IC electronics could drastically improve Venus lander designs and mission concepts, fundamentally enabling long-duration enhanced missions to the surface of Venus.

  10. Overview of the conceptual design of the future VENUS beamline at the Spallation Neutron Source

    Energy Technology Data Exchange (ETDEWEB)

    Bilheux, Hassina Z [ORNL; Herwig, Kenneth W [ORNL; Keener, Wylie S [ORNL; Davis, Larry E [ORNL

    2015-01-01

    VENUS will be a world-class neutron-imaging instrument that will uniquely utilize the Spallation Neutron Source (SNS) time-of-flight (TOF) capabilities to measure and characterize objects across several length scales (mm to m). When completed, VENUS will provide academia, industry and government laboratories with the opportunity to advance scientific research in areas such as energy, materials, additive manufacturing, geosciences, transportation, engineering, plant physiology, biology, etc. It is anticipated that a good portion of the VENUS user community will have a strong engineering/industrial research focus. Installed at Beamline 10 (BL10), VENUS will be a 25-m neutron imaging facility with the capability to fully illuminate (i.e., umbra illumination) a 20 cm x 20 cm detector area. The design allows for a 28 cm x 28 cm field of view when using the penumbra to 80% of the full illumination flux. A sample position at 20 m will be implemented for magnification measurements. The optical components are comprised of a series of selected apertures, T0 and bandwidth choppers, beam scrapers, a fast shutter to limit sample activation, and flight tubes filled with Helium. Techniques such as energy selective, Bragg edge and epithermal imaging will be available at VENUS

  11. Automated cloud tracking system for the Akatsuki Venus Climate Orbiter data

    Science.gov (United States)

    Ogohara, Kazunori; Kouyama, Toru; Yamamoto, Hiroki; Sato, Naoki; Takagi, Masahiro; Imamura, Takeshi

    2012-02-01

    Japanese Venus Climate Orbiter, Akatsuki, is cruising to approach to Venus again although its first Venus orbital insertion (VOI) has been failed. At present, we focus on the next opportunity of VOI and the following scientific observations.We have constructed an automated cloud tracking system for processing data obtained by Akatsuki in the present study. In this system, correction of the pointing of the satellite is essentially important for improving accuracy of the cloud motion vectors derived using the cloud tracking. Attitude errors of the satellite are reduced by fitting an ellipse to limb of an imaged Venus disk. Next, longitude-latitude distributions of brightness (cloud patterns) are calculated to make it easy to derive the cloud motion vectors. The grid points are distributed at regular intervals in the longitude-latitude coordinate. After applying the solar zenith correction and a highpass filter to the derived longitude-latitude distributions of brightness, the cloud features are tracked using pairs of images. As a result, we obtain cloud motion vectors on longitude-latitude grid points equally spaced. These entire processes are pipelined and automated, and are applied to all data obtained by combinations of cameras and filters onboard Akatsuki. It is shown by several tests that the cloud motion vectors are determined with a sufficient accuracy. We expect that longitude-latitude data sets created by the automated cloud tracking system will contribute to the Venus meteorology.

  12. Global Reference Atmospheric Models, Including Thermospheres, for Mars, Venus and Earth

    Science.gov (United States)

    Justh, Hilary L.; Justus, C. G.; Keller, Vernon W.

    2006-01-01

    This document is the viewgraph slides of the presentation. Marshall Space Flight Center's Natural Environments Branch has developed Global Reference Atmospheric Models (GRAMs) for Mars, Venus, Earth, and other solar system destinations. Mars-GRAM has been widely used for engineering applications including systems design, performance analysis, and operations planning for aerobraking, entry descent and landing, and aerocapture. Preliminary results are presented, comparing Mars-GRAM with measurements from Mars Reconnaissance Orbiter (MRO) during its aerobraking in Mars thermosphere. Venus-GRAM is based on the Committee on Space Research (COSPAR) Venus International Reference Atmosphere (VIRA), and is suitable for similar engineering applications in the thermosphere or other altitude regions of the atmosphere of Venus. Until recently, the thermosphere in Earth-GRAM has been represented by the Marshall Engineering Thermosphere (MET) model. Earth-GRAM has recently been revised. In addition to including an updated version of MET, it now includes an option to use the Naval Research Laboratory Mass Spectrometer Incoherent Scatter Radar Extended Model (NRLMSISE-00) as an alternate thermospheric model. Some characteristics and results from Venus-GRAM and Earth-GRAM thermospheres are also presented.

  13. Investigating the Origin and Evolution of Venus with in Situ Mass Spectrometry

    Science.gov (United States)

    Trainer, M. G.; Mahaffy, P. R.; Brinckerhoff, W. B.; Johnson, N. M.; Glaze, L. S.

    2016-01-01

    The exploration of Venus continues to be a top priority of planetary science. The Planetary Decadal Survey goals for inner-planet exploration seek to discern the origin and diversity of terrestrial planets, understand how the evolution of terrestrial planets relates to the evolution of life, and explore the processes that control climate on Earth-like planets. These goals can only be realized through continued and extensive exploration of Venus, the most mysterious of the terrestrial planets, remarkably different from the Earth despite the gross similarities between these "twin planets". It is unknown if this apparent divergence was intrinsic, programmed during accretion from distinct nebular reservoirs, or a consequence of either measured or catastrophic processes during planetary evolution. Even if the atmosphere of Venus is a more "recent" development, its relationship to the resurfacing of the planet's enigmatic surface is not well understood. Resolving such uncertainties directly addresses the hypothesis of a more clement, possibly water-rich era in Venus' past as well as whether Earth could become more Venus-like in the future.

  14. Governance, sustainability and contemporary boards

    OpenAIRE

    Coulson-Thomas, Colin

    2016-01-01

    In relation to governance, sustainability and contemporary boards explores the changing business context, stakeholder relationships, the role of independent directors, remuneration and other committees, corporate purpose, and widening board perspectives in order to reconcile different perspectives and address sustainability concerns. Raises questions in these areas and in relation to determining what to sustain, reviewing contemporary approaches and understanding their consequences, relevance...

  15. Does Board Diversity Really Matter?

    DEFF Research Database (Denmark)

    Rose, Caspar; Munch-Madsen, Peter; Funch, Maja

    2013-01-01

    We study the impact of female board representation as well as citizenship on corporate performance based on a sample of the largest listed firms in the Nordic countries as well as Germany. We also seek to determine the variation of board structures using factor analysis. We find no support for an...

  16. General purpose programmable accelerator board

    Science.gov (United States)

    Robertson, Perry J.; Witzke, Edward L.

    2001-01-01

    A general purpose accelerator board and acceleration method comprising use of: one or more programmable logic devices; a plurality of memory blocks; bus interface for communicating data between the memory blocks and devices external to the board; and dynamic programming capabilities for providing logic to the programmable logic device to be executed on data in the memory blocks.

  17. The Dutch Female Board Index 2010

    NARCIS (Netherlands)

    Lückerath – Rovers, M.

    2010-01-01

    The Dutch Female Board Index 2010 shows for the fourth year a survey of female representation on the Executive Boards and Supervisory Boards of 99 Dutch NVs listed on Euronext Amsterdam. The companies were classified by the percentage of women in their joint Executive Board and Supervisory Board.

  18. Venus 2004: east and west elongations and solar transit

    Science.gov (United States)

    McKim, R. J.; Blaxall, K.; Heath, A.

    2007-04-01

    The year 2004 was exceptional in producing the first solar transit of Venus since the late Victorian era. The bright aureole and atmospheric ring were re-observed, and the entire phenomenon was witnessed for the first time ever in hydrogen alpha light. Although routine observations throughout 2004 were unexceptional, patterns of visibility of bright and dark markings, cusp extensions and cusp-caps were recorded. No correlation was found between the latitude of the sub-Earth point and the visibility of either cusp-cap, with the S. cap predominating for most of the year. It was possible to accurately follow individual ultraviolet dark markings over many consecutive rotations, extending from the E. to W. elongations, and thereby to make a current measurement of the synodic atmospheric rotation period for the near-equatorial features: 3.996 ± 0.001 days. The true Ashen Light was reported visually on only a few occasions, but these correspond closely to times when infrared emission from the surface of the dark side was recorded in 1-micron waveband images. Some of the stable dark side albedo features were also visible upon the 1-micron images, and have been tentatively identified with known surface features. Infrared imaging at the same waveband showed little detail on the sunlit disk, but a few bright spots were sufficiently well observed to suggest a synodic rotation period close to 5.0 days, not atypical for the lower cloud decks.

  19. Structural Analysis and Geodynamic Implications of Tessera Terrain, Venus

    Science.gov (United States)

    Hansen, V. L.; Willis, J. J.

    1996-03-01

    Understanding processes of tessera formation is fundamental to Venus tectonic and geodynamic models. We examined tessera terrain in Ishtar Terra, crustal plateaus, and as inliers within the plains using high-resolution Magellan SAR imagery. We describe several major types of tesseraeeach found in specific geologic or geomorphic regions. Fold and S-C tessera terrain are found only in Ishtar Terra; lava flow and basin-and-dome terrains reside within the interior of crustal plateaus, whereas folded ribbon terrain and extended folded terrain comprise margins of crustal plateaus; and star terrain lies within central Phoebe. Inliers are divisible into fracture-dominated and graben-dominated tesserae, which may represent ancient flooded coronae-chasmata and crustal plateaus, respectively. Thus tesserae might form in several tectonic environments, including as a result of (1) subsurface flow in Ishtar Terra, (2) as sequences of surface-layer extension and contraction in crustal plateaus, (3) as highly-extended, previously-deformed crustal plateaus which have deflated or sunken, and become flooded and thus preserved as large plains inliers, and (4) as densely-fractured surface layersfractured as a result of corona and chasma formationwhich have since sunken and become flooded, and thus preserved as isolated, scattered, highly-fractured inliers. If these models of formation are correct, tesserae would not form a global onion skin; they would not represent a globally synchronous unit; they would not record a single period of deformation; and it would not infer a single mechanism for tesserae formation.

  20. Bilateral topographic symmetry patterns across Aphrodite Terra, Venus

    International Nuclear Information System (INIS)

    Crumpler, L.S.; Head, J.W.

    1988-01-01

    Western Aphrodite Terra, Venus, is characterized by a series of parallel linear structural discontinuities 2000--4000 km in length and 100--200 km wide, which strike at high angles to the general topographic trend of the Aphrodite Terra highlands. The broad chracteristics of the cross-strike discontinuities (CSDs) are similar to both strike-slip fault zones and terrestrial oceanic fracture zones. In an effort to distinguish between these two hypotheses, topographic profiles were taken across Aphrodite Terra to test for bilateral symmetry of the type associated with thermal boundary layer topography at divergent plate boundaries on Earth. In addition to a broad bilateral symmetry at a range of angles across Aphrodite Terra, detailed bilateral symmetry is observed within domains between linear discontinuities in directions generally parallel to the strike of the discontinuities. In addition, within a domain the centers of symmetry of several profiles define a linear rise crest that is oriented normal to the bounding CSDs and terminates against them

  1. Geologic map of the Themis Regio quadrangle (V-53), Venus

    Science.gov (United States)

    Stofan, Ellen R.; Brian, Antony W.

    2012-01-01

    The Themis Regio quadrangle (V-53), Venus, has been geologically mapped at 1:5,000,000 scale as part of the NASA Planetary Geologic Mapping Program. The quadrangle extends from lat 25° to 50° S. and from long 270° to 300° E. and encompasses the Themis Regio highland, the surrounding plains, and the southernmost extension of Parga Chasmata. Themis Regio is a broad regional topographic high with a diameter of about 2,000 km and a height of about 0.5 km that has been interpreted previously as a hotspot underlain by a mantle plume. The Themis rise is dominated by coronae and lies at the terminus of the Parga Chasmata corona chain. Themis Regio is the only one of the three corona-dominated rises that contains significant extensional deformation. Fractures and grabens are much less common than along the rest of Parga Chasmata and are embayed by corona-related flows in places. Rift and corona formation has overlapped in time at Themis Regio.

  2. The Transit of Venus: an Opportunity to Promote Astronomy

    Science.gov (United States)

    Ros, R. M.

    The transit of Venus was an excellent opportunity to promote Astronomy to everybody. In particular this occasion was used to encourage interest in Astronomy in schools. In our society, which has a good quality of life, interest in science has decreased. Every year the number of students interested in studying science degrees at university is smaller than in previous years. Our new generations do not seem to be motivated to study in the field of science. Probably this situation is a consequence of the lack of understanding of the true meaning of science. Of course, it is not possible that a student would decide to study a topic that they do not know about. In the media science appears less than sports, cinema, or business! In consequence, the general public is more concerned about items other than science. On June 8th we took advantage of an opportunity to introduce science and Astronomy into the lives of everybody, but especially in schools. This paper will show two projects related to the transit in schools: ”Pilla el Tránsito de Venus” and ”VT-2004” and a short appendix to another project for schools ”ALMA-ITP”

  3. Outcrops of plastic material on the surface of Venus

    Science.gov (United States)

    Ksanfomality, L. V.

    2015-05-01

    The archive data of the television experiment performed by the Venera-14 spacecraft on the surface of the planet Venus in March, 1982, were reprocessed, which significantly improved the image definition quality. An unusual geologic object located relatively near the camera was found, which allowed its details to be analyzed. The object is a low long bank in shape; it is formed by a relatively thin, jagged, almost vertical stratum. The bank contours the oval formation 1.5-2 m across that stands out against the layered surface. The location of the bank suggests that its material is extruded from under the layered plates surrounding the oval formation. A segment of the bank resembling a falling wave is inclined and partly covers the surface by forming the beddings. The object is likely formed by the rocks that remain semisoftened (plastic), when they appear on the surface at the temperature characteristic for the Venusian surface (about 740 K). It is suggested that, from the data on the physical and chemical conditions and the composition of the Venusian surface, the nature of the observed plastic medium can be hypothesized, and it can be even modeled under laboratory conditions.

  4. Chinese records of the 1874 transit of Venus

    Science.gov (United States)

    Lu, Lingfeng; Li, Huifang

    2013-03-01

    Before the advent of radar, transits of Venus were very important for measuring the distance between the Earth and the Sun. A transit occurred in 1874, and was visible from China, other parts of east and southeast Asia and from India, Australia and New Zealand and certain islands in the Indian and Pacific Oceans. As a result, many astronomers from Western countries came to China to observe it. According to traditional Chinese astrology, the Sun represented the Emperor, and if the Sun was invaded by other astronomical bodies it meant that the Emperor and the country faced some ominous disaster. In the late nineteenth century, Western astronomical knowledge was widely translated into Chinese and spread among Chinese intellectuals, so the 1874 transit supposedly was easily understood by Chinese intellectuals. Before the transit took place, various Chinese publications introduced this kind of celestial event as science news, but at the same time other influential newspapers and journals discussed the astrological connection between the transit and the fortunes of the nation. In this paper we review these interesting Chinese records and discuss the different attitudes towards the transit exhibited by Chinese intellectuals and officials, during a period when Western learning was being widely disseminated throughout China.

  5. The support of long wavelength loads on Venus

    Science.gov (United States)

    Benerdt, W. B.; Saunders, R. S.

    1985-04-01

    One of the great surprises of the Pioneer Venus mission was the high degree of correlation between topography and gravity found at all wavelengths. This implies a close relationship between topography and lateral subsurface density anomalies, such as those due to passive or dynamic compensation. Sleep-Phillips type compensation model with a variable crustal thickness and a variable upper mantle density was developed. The thin shell theory was used to investigate three end member cases: (1) loading by topographic construction, resulting in a downward deflection of the surface (no mantle support); (2) completely compensated support of a constructional load (no surface deflection); and (3) topography due entirely to upward deflection of the surface supported by a low density upper mantle (no surface load). In general, the models imply relatively thick crust and dense upper mantle for Ishtar Terra and Ovda Regio (western Aphrodite), thinned crust and buoyant upper mantle for Tethus Regio and regions near Sappho and Alpha Regio, and a nearly uniform crust with a buoyant upper mantle for Beta Regio and Atla Regio (eastern Aphrodite).

  6. Geologic map of the Lada Terra quadrangle (V-56), Venus

    Science.gov (United States)

    Kumar, P. Senthil; Head, James W.

    2013-01-01

    This publication provides a geological map of Lada Terra quadrangle (V–56), a portion of the southern hemisphere of Venus that extends from lat 50° S. to 70° S. and from long 0° E. to 60° E. V–56 is bordered by Kaiwan Fluctus (V–44) and Agnesi (V–45) quadrangles in the north and by Mylitta Fluctus (V–61), Fredegonde (V–57), and Hurston (V–62) quadrangles in the west, east, and south, respectively. The geological map of V–56 quadrangle reveals evidence for tectonic, volcanic, and impact processes in Lada Terra in the form of tesserae, regional extensional belts, coronae, and volcanic plains. In addition, the map also shows relative age relations such as overlapping or cross-cutting relations between the mapped geologic units. The geology observed within this quadrangle addresses (1) how coronae evolved in association with regional extensional belts and (2) how tesserae, regional plains, and impact craters, which are also significant geological units observed in Lada Terra quadrangle, were formed.

  7. Cloud motions on Venus - Global structure and organization

    Science.gov (United States)

    Limaye, S. S.; Suomi, V. E.

    1981-01-01

    Results on cloud motions on Venus obtained over a period of 3.5 days from Mariner 10 television images are presented. The implied atmosphere flow is almost zonal everywhere on the visible disk, and is in the same retrograde sense as the solid planet. Objective analysis of motions suggests the presence of jet cores (-130 m/s) and organized atmospheric waves. The longitudinal mean meridional profile of the zonal component of motion of the ultraviolet features shows presence of a midlatitude jet stream (-110 m/s). The mean zonal component is -97 m/s at the equator. The mean meridional motion at most latitudes is directed toward the pole in either hemisphere and is at least an order of magnitude smaller so that the flow is nearly zonal. A tentative conclusion from the limited coverage available from Mariner 10 is that at the level of ultraviolet features mean meridional circulation is the dominant mode of poleward angular momentum transfer as opposed to the eddy circulation.

  8. Governing Board of the Pension Fund

    CERN Document Server

    HR Department

    2007-01-01

    The Governing Board of the Pension Fund held its one-hundred-and-fifty-second and one-hundred-and-fifty-third meetings on 18 April and 15 May 2007 respectively. The latter was a full-day joint meeting with the Investment Committee. At the first of the two meetings on 18 April, the Chairman of the Governing Board, Professor F. Ferrini, reported on the outcome of the Finance Committee meeting and the Council Session of March 2007. The Council had taken note of a progress report by the Chairman of the Study Group on CERN Pension Fund Governance, Mr P. Levaux, had expressed satisfaction at the Study Group's progress and was now looking forward to the proposal, largely bearing on the Pension Fund's bodies and their composition, which is due to be submitted to the Council for approval at its June 2007 Session. At the same meeting, the Governing Board approved the Annual Report and Accounts of the Fund for 2006 and thanked the Fund's Administration for the substantial work entailed in providing the reader with a...

  9. Governing Board of the Pension Fund

    CERN Multimedia

    2007-01-01

    The Governing Board of the Pension Fund held its one-hundred-and-fifty-second and one-hundred-and-fifty-third meetings on 18 April and 15 May 2007 respectively. The latter was a full-day joint meeting with the Investment Committee. At the first of the two meetings, on 18 April, the Chairman of the Governing Board, Professor F. Ferrini, reported on the outcome of the Finance Committee meeting and the Council Session of March 2007. The Council had taken note of a progress report by the Chairman of the Study Group on CERN Pension Fund Governance, Mr P. Levaux, had expressed satisfaction at the Study Group’s progress and was now looking forward to the proposal, largely bearing on the Pension Fund’s bodies and their composition, which is due to be submitted to the Council for approval at its June 2007 Session. At the same meeting, the Governing Board approved the Annual Report and Accounts of the Fund for 2006 and thanked the Fund’s Administration for the substantial work entailed in providing the reader ...

  10. GOVERNING BOARD OF THE PENSION FUND

    CERN Multimedia

    2003-01-01

    The Governing Board held its 116th meeting on 6 May 2003, which was mainly devoted to two presentations, the first by J.-P. Matheys, Chairman of the Working Group set up to examine a request from ESO, who reported on the group's first meeting, and the second by Guy Maurin, Chairman of the Investment Committee, on the latter's meeting of 9 April. Concerning ESO's request to the Governing Board of the Pension Fund relating to changes that ESO wishes to make to the conditions of membership of its staff members, J.-P. Matheys reported that at the first meeting of the Working Group specially set up to examine this request the members had agreed that the Group should give priority to ensuring that ESO's request had no financial or legal repercussions for the Fund. The Group had also expressed its agreement with the Governing Board's opinion that any amendment to the Pension Fund Rules and Regulations should be avoided. Furthermore, the Group had reached the conclusion that it would be impossible to submit recommend...

  11. Applicability of ultralow-frequency global resonances for investigating lightning activity on Venus

    International Nuclear Information System (INIS)

    Nikolaenko, A.P.; Rabinovich, L.M.

    1987-01-01

    The application to experiments on Venus of methods of investigating global lightning activity that are used on earth in the ultralow-frequency range is discussed. Calculations of the electromagnetic fields in the range from a few Hertz to tens of Hertz are carried out in the framework of the model of the lower ionosphere of Venus, which generalizes the information about the planet's atmosphere which is presently available. The calculations showed that observations of global resonances on Venus must, as on the earth, allow one to obtain data about the global distribution of lightning in space and time, and to make the values of the parameters of the lower ionosphere model more precise

  12. The effect of recent Venus transit on Earth’s atmosphere

    Directory of Open Access Journals (Sweden)

    H. P. Sardar

    2006-06-01

    Full Text Available Some experiments on June 8, 2004, the day of transit of Venus across the Sun, were undertaken at Kolkata (latitude: 22°34lN to observe the effect, if any, of transit of Venus on FWF, ELF and VLF amplitudes. The result shows a good correlation between their temporal variations during the transit. The observation was unbelievable as the Venus subtends only 1/32th of the cone subtended by Sun on Earth. This anomaly may be explained on the assumption that the height of Venusian atmosphere with high content of CO2, and nitrogen which absorbs electromagnetic and corpuscular radiations from Sun, depleting the solar radiation reaching the Earth to a considerable extent. As a result, relevant parameters of Earth’s atmosphere are modulated and here we show how these changes are reflected in identical behaviour of fair weather field and ELF and VLF spectra.

  13. Digital amateur observations of Venus at 0.9μm

    Science.gov (United States)

    Kardasis, E.

    2017-09-01

    Venus atmosphere is extremely dynamic, though it is very difficult to observe any features on it in the visible and even in the near-IR range. Digital observations with planetary cameras in recent years routinely produce high-quality images, especially in the near-infrared (0.7-1μm), since IR wavelengths are less influenced by Earth's atmosphere and Venus's atmosphere is partially transparent in this spectral region. Continuous observations over a few hours may track dark atmospheric features in the dayside and determine their motion. In this work we will present such observations and some dark-feature motion measurements at 0.9μm. Ground-based observations at this wavelength are rare and are complementary to in situ observations by JAXA's Akatsuki orbiter, that studies the atmospheric dynamics of Venus also in this band with the IR1 camera.

  14. Estimation of the rate of volcanism on Venus from reaction rate measurements

    Science.gov (United States)

    Fegley, Bruce, Jr.; Prinn, Ronald G.

    1989-01-01

    Laboratory rate data for the reaction between SO2 and calcite to form anhydrite are presented. If this reaction rate represents the SO2 reaction rate on Venus, then all SO2 in the Venusian atmosphere will disappear in 1.9 Myr unless volcanism replenishes the lost SO2. The required volcanism rate, which depends on the sulfur content of the erupted material, is in the range 0.4-11 cu km of magma erupted per year. The Venus surface composition at the Venera 13, 14, and Vega 2 landing sites implies a volcanism rate of about 1 cu km/yr. This geochemically estimated rate can be used to determine if either (or neither) of two discordant geophysically estimated rates is correct. It also suggests that Venus may be less volcanically active than the earth.

  15. Mitigating Extreme Environments for In-Situ Jupiter and Venus Missions

    Science.gov (United States)

    Balint, Tibor S.; Kolawa, Elizabeth A.; Cutts, James A.

    2006-01-01

    In response to the recommendations by the National Research Council (NRC), NASA's Solar System Exploration (SSE) Roadmap identified the in situ exploration of Venus and Jupiter as high priority science objectives. For Jupiter, deep entry probes are recommended, which would descend to approx.250 km - measured from the 1 bar pressure depth. At this level the pressure would correspond to approx.100 bar and the temperature would reach approx.500(deg)C. Similarly, at the surface of Venus the temperature and pressure conditions are approx.460(deg)C and approx.90 bar. Lifetime of the Jupiter probes during descent can be measured in hours, while in{situ operations at and near the surface of Venus are envisioned over weeks or months. In this paper we discuss technologies, which share commonalities in mitigating these extreme conditions over proposed mission lifetimes, specially focusing on pressure and temperature environments.

  16. Geologic Mapping of the Beta-Atla-Themis (BAT) Region of Venus: A Progress Report

    Science.gov (United States)

    Bleamaster, Leslie F., III

    2009-01-01

    The BAT province is of particular interest with respect to evaluating Venus geologic, tectonic, and volcanic history and provides tests of global paradigms regarding her thermal evolution. The BAT is "ringed" by volcano-tectonic troughs (Parga, Hecate, and Devana Chasmata), has an anomalously high-density of volcanic features with concentrations 2-4 times the global average [1], and is spatially coincident with "young terrain" as illustrated by Average Surface Model Ages [2, 3]. The BAT province is key to understanding Venus current volcanic and tectonic modes, which may provide insight for evaluating Venus historical record. Several quadrangles, two 1:5,000,000 scale - Isabella (V-50) Quadrangle and Devana Chasma (V-29) Quadrangle and two 1:10,000,000 scale - Helen Planitia (I-2477) and Guinevere Planitia (I-2457), are in various stages of production (Figure 1). This abstract will report on their levels of completion as well as highlight some current results and outstanding issues.

  17. Sequencing and characterization of striped venus transcriptome expand resources for clam fishery genetics.

    Directory of Open Access Journals (Sweden)

    Alessandro Coppe

    Full Text Available BACKGROUND: The striped venus Chamelea gallina clam fishery is among the oldest and the largest in the Mediterranean Sea, particularly in the inshore waters of northern Adriatic Sea. The high fishing pressure has lead to a strong stock abundance decline, enhanced by several irregular mortality events. The nearly complete lack of molecular characterization limits the available genetic resources for C. gallina. We achieved the first transcriptome of this species with the aim of identifying an informative set of expressed genes, potential markers to assess genetic structure of natural populations and molecular resources for pathogenic contamination detection. METHODOLOGY/PRINCIPAL FINDINGS: The 454-pyrosequencing of a normalized cDNA library of a pool C. gallina adult individuals yielded 298,494 raw reads. Different steps of reads assembly and filtering produced 36,422 contigs of high quality, one half of which (18,196 were annotated by similarity. A total of 111 microsatellites and 20,377 putative SNPs were identified. A panel of 13 polymorphic transcript-linked microsatellites was developed and their variability assessed in 12 individuals. Remarkably, a scan to search for contamination sequences of infectious origin indicated the presence of several Vibrionales species reported to be among the most frequent clam pathogen's species. Results reported in this study were included in a dedicated database available at http://compgen.bio.unipd.it/chameleabase. CONCLUSIONS/SIGNIFICANCE: This study represents the first attempt to sequence and de novo annotate the transcriptome of the clam C. gallina. The availability of this transcriptome opens new perspectives in the study of biochemical and physiological role of gene products and their responses to large and small-scale environmental stress in C. gallina, with high throughput experiments such as custom microarray or targeted re-sequencing. Molecular markers, such as the already optimized EST

  18. VenSAR on EnVision: Taking earth observation radar to Venus

    Science.gov (United States)

    Ghail, Richard C.; Hall, David; Mason, Philippa J.; Herrick, Robert R.; Carter, Lynn M.; Williams, Ed

    2018-02-01

    Venus should be the most Earth-like of all our planetary neighbours: its size, bulk composition and distance from the Sun are very similar to those of Earth. How and why did it all go wrong for Venus? What lessons can be learned about the life story of terrestrial planets in general, in this era of discovery of Earth-like exoplanets? Were the radically different evolutionary paths of Earth and Venus driven solely by distance from the Sun, or do internal dynamics, geological activity, volcanic outgassing and weathering also play an important part? EnVision is a proposed ESA Medium class mission designed to take Earth Observation technology to Venus to measure its current rate of geological activity, determine its geological history, and the origin and maintenance of its hostile atmosphere, to understand how Venus and Earth could have evolved so differently. EnVision will carry three instruments: the Venus Emission Mapper (VEM); the Subsurface Radar Sounder (SRS); and VenSAR, a world-leading European phased array synthetic aperture radar that is the subject of this article. VenSAR will obtain images at a range of spatial resolutions from 30 m regional coverage to 1 m images of selected areas; an improvement of two orders of magnitude on Magellan images; measure topography at 15 m resolution vertical and 60 m spatially from stereo and InSAR data; detect cm-scale change through differential InSAR, to characterise volcanic and tectonic activity, and estimate rates of weathering and surface alteration; and characterise of surface mechanical properties and weathering through multi-polar radar data. These data will be directly comparable with Earth Observation radar data, giving geoscientists unique access to an Earth-sized planet that has evolved on a radically different path to our own, offering new insights on the Earth-sized exoplanets across the galaxy.

  19. New Frontiers Science at Venus from Orbit plus Atmospheric Gas Sampling

    Science.gov (United States)

    Smrekar, Suzanne; Dyar, Melinda; Hensley, Scott; Helbert, Joern; VOX Science and Engineering Teams

    2017-10-01

    Venus remains the most Earth-like body in terms of size, composition, surface age, and insulation. Venus Origins Explorer (VOX) determines how Earth’s twin diverged, and enables breakthroughs in our understanding of rocky planet evolution and habitability. At the time of the Decadal Survey the ability to map mineralogy from orbit (Helbert et al.) and present-day radar techniques to detect active deformation were not fully appreciated. VOX leverages these methods and in-situ noble gases to answer New Frontiers science objectives:1. Atmospheric physics/chemistry: noble gases and isotopes to constrain atmospheric sources, escape processes, and integrated volcanic outgassing; global search for current volcanically outgassed water.2. Past hydrological cycles: global tessera composition to determine the role of volatiles in crustal formation.3. Crustal physics/chemistry: global crustal mineralogy/chemistry, tectonic processes, heat flow, resolve the catastrophic vs. equilibrium resurfacing debate, active geologic processes and possible crustal recycling.4. Crustal weathering: surface-atmosphere weathering reactions from redox state and the chemical equilibrium of the near-surface atmosphere.5. Atmospheric properties/winds: map cloud particle modes and their temporal variations, and track cloud-level winds in the polar vortices.6. Surface-atmosphere interactions: chemical reactions from mineralogy; weathering state between new, recent and older flows; possible volcanically outgassed water.VOX’s Atmosphere Sampling Vehicle (ASV) dips into and samples the well-mixed atmosphere, using Venus Original Constituents Experiment (VOCE) to measure noble gases. VOX’s orbiter carries the Venus Emissivity Mapper (VEM) and the Venus Interferometric Synthetic Aperture Radar (VISAR), and maps the gravity field using Ka-band tracking.VOX is the logical next mission to Venus because it delivers: 1) top priority atmosphere, surface, and interior science; 2) key global data for

  20. The Effect of Bond Albedo on Venus' Atmospheric and Surface Temperatures

    Science.gov (United States)

    Bullock, M. A.; Limaye, S. S.; Grinspoon, D. H.; Way, M.

    2017-12-01

    In spite of Venus' high planetary albedo, sufficient solar energy reaches the surface to drive a powerful greenhouse effect. The surface temperature is three times higher than it would be without an atmosphere. However, the details of the energy balance within Venus' atmosphere are poorly understood. Half of the solar energy absorbed within the clouds, where most of the solar energy is absorbed, is due to an unknown agent. One of the challenges of modeling Venus' atmosphere has been to account for all the sources of opacity sufficient to generate a globally averaged surface temperature of 735 K, when only 2% of the incoming solar energy is deposited at the surface. The wavelength and spherically integrated albedo, or Bond albedo, has typically been cited as between 0.7 and 0.82 (Colin 1983). Yet, recent photometry of Venus at extended phase angles between 2 and 179° indicate a Bond albedo of 0.90 (Mallama et al., 2006). The authors note an increase in cloud top brightness at phase angles right). Venus surface temperature as Bond Albedo changes. Radiative-convective equilibrium models predict the correct globally averaged surface temperature at a=0.81. Calculations here show that a Bond albedo of a=0.9 would yield a surface temperature of 666.4 K, about 70 K too low, unless there is additional thermal absorption within the atmosphere that is not understood. Colin, L.,, Venus, University of Arizona Press, Tucson, 1983, pp 10-26. Mallama, A., et al., 2006. Icarus. 182, 10-22.

  1. The Devil in the Dark: A Fully Self-Consistent Seismic Model for Venus

    Science.gov (United States)

    Unterborn, C. T.; Schmerr, N. C.; Irving, J. C. E.

    2017-12-01

    The bulk composition and structure of Venus is unknown despite accounting for 40% of the mass of all the terrestrial planets in our Solar System. As we expand the scope of planetary science to include those planets around other stars, the lack of measurements of basic planetary properties such as moment of inertia, core-size and thermal profile for Venus hinders our ability to compare the potential uniqueness of the Earth and our Solar System to other planetary systems. Here we present fully self-consistent, whole-planet density and seismic velocity profiles calculated using the ExoPlex and BurnMan software packages for various potential Venusian compositions. Using these models, we explore the seismological implications of the different thermal and compositional initial conditions, taking into account phase transitions due to changes in pressure, temperature as well as composition. Using mass-radius constraints, we examine both the centre frequencies of normal mode oscillations and the waveforms and travel times of body waves. Seismic phases which interact with the core, phase transitions in the mantle, and shallower parts of Venus are considered. We also consider the detectability and transmission of these seismic waves from within the dense atmosphere of Venus. Our work provides coupled compositional-seismological reference models for the terrestrial planet in our Solar System of which we know the least. Furthermore, these results point to the potential wealth of fundamental scientific insights into Venus and Earth, as well as exoplanets, which could be gained by including a seismometer on future planetary exploration missions to Venus, the devil in the dark.

  2. 7 CFR 1221.2 - Board.

    Science.gov (United States)

    2010-01-01

    ... ORDERS; MISCELLANEOUS COMMODITIES), DEPARTMENT OF AGRICULTURE SORGHUM PROMOTION, RESEARCH, AND INFORMATION ORDER Sorghum Promotion, Research, and Information Order Definitions § 1221.2 Board. Board or Sorghum Promotion, Research, and Information Board means the administrative body established pursuant to...

  3. 78 FR 54629 - Consumer Advisory Board meeting

    Science.gov (United States)

    2013-09-05

    ... From the Federal Register Online via the Government Publishing Office CONSUMER FINANCIAL PROTECTION BUREAU Consumer Advisory Board meeting AGENCY: Bureau of Consumer Financial Protection. ACTION... Consumer Advisory Board (``CAB'' or ``Board'') of the Consumer Financial Protection Bureau (Bureau). The...

  4. 78 FR 66384 - Membership of the Merit Systems Protection Board's Performance Review Board

    Science.gov (United States)

    2013-11-05

    ... MERIT SYSTEMS PROTECTION BOARD Membership of the Merit Systems Protection Board's Performance Review Board AGENCY: Merit Systems Protection Board. ACTION: Notice. SUMMARY: Notice is hereby given of the members of the Merit Systems Protection Board's Performance Review Board. DATES: November 5, 2013...

  5. Modeling Venus-like Worlds Through Time and Implications for the Habitable Zone

    Science.gov (United States)

    Way, M.; Del Genio, A. D.; Amundsen, D. S.; Sohl, L. E.; Kiang, N. Y.; Aleinov, I. D.; Kelley, M.

    2017-12-01

    In recent work [1] we demonstrated that the climatic history of Venus may have allowed for surface liquid water to exist for several billion years using a 3D GCM [2]. Model resolution was 4x5 latitude x longitude, 20 atmospheric layers and a 13 layer fully coupled ocean. Several assumptions were made based on what data we have for early Venus: a.) Used a solar spectrum from 2.9 billion years ago, and 715 million years ago for the incident radiation. b.) Assumed Venus had the same slow modern retrograde rotation throughout the 2.9 to 0.715 Gya history explored, although one simulation at faster rotation rate was shown not to be in the HZ. c.) Used atmospheric constituents similar to modern Earth: 1 bar N2, 400ppmv CO2, 1ppmv CH4. d.) Gave the planet a shallow 310m deep ocean constrained by published D/H ratio observations. e.) Used present day Venus topography and one run with Earth topography.In all cases except the faster rotating one the planet was able to maintain surface liquid water. We have now inserted the SOCRATES [3] radiation scheme into our 3D GCM to more accurately calculate heating fluxes for different atmospheric constituents. Using SOCRATES we have explored a number of other possible early histories for Venus including: f.) An aquaplanet configuration at 2.9Gya with present day rotation period.g.) A Land planet configuration at 2.9Gya with the equivalent of 10m of water in soil and lakes. h.) A synchronously rotating version of a, f, and g (supported by recent work of [4] and older work of [5]) i.) A Venus topography with a 310m ocean, but using present day insolation (1.9 x Earth). j.) Versions of most of the worlds above but with solar insolations >1.9 to explore more Venus-like exoplanetary worlds around G-type stars. In these additional cases the planet still resides in the liquid water habitable zone. Studies such as these should help Astronomers better understand whether exoplanets found in the Venus zone [6] are capable of hosting liquid water

  6. Fractionation of hydrogen and deuterium on Venus due to collisional ejection

    Science.gov (United States)

    Gurwell, Mark A.; Yung, Yuk L.

    1993-01-01

    The collisional ejection process for hydrogen on Venus is reanalyzed. Improved values for the efficiency of H and D escape as a function of the ionospheric temperature are reported. It is proposed that the reduction of the hydrogen flux for collisional ejection be reduced from 8 to 3.5 x 10 exp 6/sq cm/s, and a revised D/H fractional factor of 0.47 due to collisional ejection is suggested. The resulting deuterium flux is 3.1 x 10 exp 4/sq cm/s, roughly six times the flux due to charge exchange, making collisional ejection the dominant escape mechanism for deuterium on Venus.

  7. Radioisotope Power Systems for In-situ Exploration of Titan and Venus

    Science.gov (United States)

    Balint, Tibor S.

    2006-01-01

    This viewgraph presentation reviews the timeline for the robotic in situ investigation of Titan and Venus, and the use of radioisotope power systems in this exploration. The atmospheric and surface conditions of both sites are reviewed. The presentation also examines the conceptual design of the Venus Mobile Explorer and the Titan orbiter and in situ explorer. After this the presentation reviews the radioisotope power systems for each of the vehicles, with some explanation of the different requirements based on the vastly different environments that they would be investigating

  8. Ownership Structure, Board Composition and Investment Performance

    OpenAIRE

    Eklund, Johan; Palmberg, Johanna; Wiberg, Daniel

    2009-01-01

    In this paper the relation between ownership structure, board composition and firm performance is explored. A panel of Swedish listed firms is used to investigate how board composition affects firm performance. Board heterogeneity is measured as board size, age and gender diversity. The results show that Swedish board of directors have become more diversified in terms of gender. Also, fewer firms have the CEO on the board which can be interpreted as a sign of increased independency. The regre...

  9. Board-to-board consistency in initial dental licensure examinations.

    Science.gov (United States)

    Chambers, David W

    2011-10-01

    The consistency between student clinical performance in dental school and performance on initial licensure examinations is known to be weak. A review of the literature failed to identify any reports of the consistency between performance on initial licensure examinations and quality of technical work in practice. This research examines the consistency of performance among candidates who took two initial licensure examinations given by different testing agencies but for the same jurisdiction within a few weeks of each other. Twenty-seven candidates from one dental school took both the California Dental Board examination and the Western Regional Examining Board initial licensure examinations in 2005 and 2006. Their performance on the patient-based amalgam and composite restorations and the root planing tests were compared in these two board settings and with various dental school measures of competence. Consistent with previous findings, school-to-board performance was barely above chance levels. Board-to-board association was also insignificant and accounted for 12 percent of the common variance in the best case. Patient-based initial licensure examinations have yet to demonstrate validity in terms of consistency of performance for candidates from one performance to the next.

  10. Geological Map of the Fredegonde (V-57) Quadrangle, Venus

    Science.gov (United States)

    Ivanov, M. A.; Head, J. W.

    2009-01-01

    The area of V-57, the Fredegonde quadrangle (50-75degS, 60-120degE, Fig.1), is located within the eastern portion of Lada Terra within the topographic province of midlands (0-2 km above MPR [1,2]). Midlands form the most abundant portion of the surface of Venus and are characterized by diverse sets of units and structures [3-11]. The area of the Fredegonde quadrangle is in contact with the elevated portion of Lada Terra to the W and with the lowland of Aino Planitia to the NE. The transitions of the mid-lands to the lowlands and highlands are, thus, one of the main themes of the geology within the V-57 quadrangle. The character of the transitions and distribution and sequence of units/structures in the midlands are crucially important in understanding the time and modes of formation of this topographic province. The most prominent features in the map area are linear deformational zones consisting of swarms of grooves and graben and large coronae. The zones characterize the central and NW portions of the map area and represent regionally important, broad (up to 100s km wide) ridges that are 100s m high. Relatively small (100s km across, 100s m deep) equidimensional basins occur between the corona-groove-chains in the west and border the central chain from the east. Here we describe units that make up the surface within the V-57 quadrangle and present a summary of our geological map that shows the areal distribution of the major groups of units.

  11. Tidal Venuses: triggering a climate catastrophe via tidal heating.

    Science.gov (United States)

    Barnes, Rory; Mullins, Kristina; Goldblatt, Colin; Meadows, Victoria S; Kasting, James F; Heller, René

    2013-03-01

    Traditionally, stellar radiation has been the only heat source considered capable of determining global climate on long timescales. Here, we show that terrestrial exoplanets orbiting low-mass stars may be tidally heated at high-enough levels to induce a runaway greenhouse for a long-enough duration for all the hydrogen to escape. Without hydrogen, the planet no longer has water and cannot support life. We call these planets "Tidal Venuses" and the phenomenon a "tidal greenhouse." Tidal effects also circularize the orbit, which decreases tidal heating. Hence, some planets may form with large eccentricity, with its accompanying large tidal heating, and lose their water, but eventually settle into nearly circular orbits (i.e., with negligible tidal heating) in the habitable zone (HZ). However, these planets are not habitable, as past tidal heating desiccated them, and hence should not be ranked highly for detailed follow-up observations aimed at detecting biosignatures. We simulated the evolution of hypothetical planetary systems in a quasi-continuous parameter distribution and found that we could constrain the history of the system by statistical arguments. Planets orbiting stars with massesplanet orbiting a 0.3 MSun star at 0.12 AU. We found that it probably did not lose its water via tidal heating, as orbital stability is unlikely for the high eccentricities required for the tidal greenhouse. As the inner edge of the HZ is defined by the onset of a runaway or moist greenhouse powered by radiation, our results represent a fundamental revision to the HZ for noncircular orbits. In the appendices we review (a) the moist and runaway greenhouses, (b) hydrogen escape, (c) stellar mass-radius and mass-luminosity relations, (d) terrestrial planet mass-radius relations, and (e) linear tidal theories.

  12. Investor Perceptions of Board Performance

    DEFF Research Database (Denmark)

    Fischer, Paul E.; Gramlich, Jeffrey D.; Miller, Brian P.

    2009-01-01

    This paper provides evidence that uncontested director elections provide informative polls of investor perceptions regarding board performance. We find that higher (lower) vote approval is associated with lower (higher) stock price reactions to subsequent announcements of management turnovers...

  13. Specialty Board on Fluency Disorders

    Science.gov (United States)

    ... or large groups of speech-language pathologists. Speech-language pathologists who are Board Certified Specialists in Fluency may be found on this website by searching name, city(location) or zip code. ...

  14. Institutional Evolution and Corporate Boards

    DEFF Research Database (Denmark)

    Chen, Victor Zitian; Hobdari, Bersant; Sun, Pei

    2014-01-01

    We argue that corporate boards are a dynamic repository of human- and social capital in response to external institutional evolution. Theoretically, integrating institutional economics, agency theory and resource dependence theory, we explain that evolution of market-, legal- and political....... Such particular contexts entail the external competitive environment and the principal-agency relationship in corporate governance, amplify (or weaken) the need for certain type of board roles, and ultimately require corporations to reconfigure the human- and social capital embedded within the board. Additionally......, since the board changes are typically proposed by the block shareholders, whose motivation for doing so is closely associated with a corporation’s financial performance, we further argue that financial performance is a key moderator of the relationships between institutional evolution and changes...

  15. Employee on Boarding Process Automation

    OpenAIRE

    Khushboo Nalband; Priyanka Jadhav; Geetanjali Salunke

    2017-01-01

    On boarding, also known as organizational socialization, plays a vital role in building the initial relationship between an organization and an employee. It also contributes to an employees’ satisfaction, better performance and greater organizational commitment thus increasing an employees’ effectiveness and productivity in his/her role. Therefore, it is essential that on boarding process of an organization is efficient and effective to improve new employees’ retention. Generally this on boar...

  16. Purification and Characterization of Hemagglutinating Proteins from Poker-Chip Venus (Meretrix lusoria and Corbicula Clam (Corbicula fluminea

    Directory of Open Access Journals (Sweden)

    Chin-Fu Cheng

    2012-01-01

    Full Text Available Hemagglutinating proteins (HAPs were purified from Poker-chip Venus (Meretrix lusoria and Corbicula clam (Corbicula fluminea using gel-filtration chromatography on a Sephacryl S-300 column. The molecular weights of the HAPs obtained from Poker-chip Venus and Corbicula clam were 358 kDa and 380 kDa, respectively. Purified HAP from Poker-chip Venus yielded two subunits with molecular weights of 26 kDa and 29 kDa. However, only one HAP subunit was purified from Corbicula clam, and its molecular weight was 32 kDa. The two Poker-chip Venus HAPs possessed hemagglutinating ability (HAA for erythrocytes of some vertebrate animal species, especially tilapia. Moreover, HAA of the HAP purified from Poker-chip Venus was higher than that of the HAP of Corbicula clam. Furthermore, Poker-chip Venus HAPs possessed better HAA at a pH higher than 7.0. When the temperature was at 4°C–10°C or the salinity was less than 0.5‰, the two Poker-chip Venus HAPs possessed better HAA compared with that of Corbicula clam.

  17. Purification and characterization of hemagglutinating proteins from Poker-chip Venus (Meretrix lusoria) and Corbicula clam (Corbicula fluminea).

    Science.gov (United States)

    Cheng, Chin-Fu; Hung, Shao-Wen; Chang, Yung-Chung; Chen, Ming-Hui; Chang, Chen-Hsuan; Tsou, Li-Tse; Tu, Ching-Yu; Lin, Yu-Hsing; Liu, Pan-Chen; Lin, Shiun-Long; Wang, Way-Shyan

    2012-01-01

    Hemagglutinating proteins (HAPs) were purified from Poker-chip Venus (Meretrix lusoria) and Corbicula clam (Corbicula fluminea) using gel-filtration chromatography on a Sephacryl S-300 column. The molecular weights of the HAPs obtained from Poker-chip Venus and Corbicula clam were 358 kDa and 380 kDa, respectively. Purified HAP from Poker-chip Venus yielded two subunits with molecular weights of 26 kDa and 29 kDa. However, only one HAP subunit was purified from Corbicula clam, and its molecular weight was 32 kDa. The two Poker-chip Venus HAPs possessed hemagglutinating ability (HAA) for erythrocytes of some vertebrate animal species, especially tilapia. Moreover, HAA of the HAP purified from Poker-chip Venus was higher than that of the HAP of Corbicula clam. Furthermore, Poker-chip Venus HAPs possessed better HAA at a pH higher than 7.0. When the temperature was at 4°C-10°C or the salinity was less than 0.5‰, the two Poker-chip Venus HAPs possessed better HAA compared with that of Corbicula clam.

  18. Seismic qualification of nuclear control board by using base isolation technique

    International Nuclear Information System (INIS)

    Koizumi, T.; Tsujiuchi, N.; Fujita, T.

    1987-01-01

    The purpose is to adopt base isolation technique as a new approach for seismic qualification of nuclear control board. Basic concept of base isolation technique is expressed. Two dimensional linear motion mechanism with pre-tensioned coil springs and some dampers are included in the isolation device. Control board is regarded as a lamped mass system with inertia moment. Fundamental movement of this device and control board is calculated as a non-linear response problems. Fundamental analysis and numerical estimation, experimental investigation has been undertaken using an actual size control board. Sufficient agreement was recognized between experimental results and numerical estimation. (orig./HP)

  19. Purification and Characterization of Hemagglutinating Proteins from Poker-Chip Venus (Meretrix lusoria) and Corbicula Clam (Corbicula fluminea)

    OpenAIRE

    Cheng, Chin-Fu; Hung, Shao-Wen; Chang, Yung-Chung; Chen, Ming-Hui; Chang, Chen-Hsuan; Tsou, Li-Tse; Tu, Ching-Yu; Lin, Yu-Hsing; Liu, Pan-Chen; Lin, Shiun-Long; Wang, Way-Shyan

    2012-01-01

    Hemagglutinating proteins (HAPs) were purified from Poker-chip Venus (Meretrix lusoria) and Corbicula clam (Corbicula fluminea) using gel-filtration chromatography on a Sephacryl S-300 column. The molecular weights of the HAPs obtained from Poker-chip Venus and Corbicula clam were 358 kDa and 380 kDa, respectively. Purified HAP from Poker-chip Venus yielded two subunits with molecular weights of 26 kDa and 29 kDa. However, only one HAP subunit was purified from Corbicula clam, and its molecul...

  20. Phyto-oestrogen levels in foods : The design and construction of the VENUS database

    NARCIS (Netherlands)

    Kiely, M.; Faughnan, M.; Wähälä, K.; Brants, H.; Mulligan, A.

    2003-01-01

    The objective of the Vegetal Estrogens in Nutrition and the Skeleton (VENUS) project was to evaluate existing data on dietary exposure to compounds with oestrogenic and anti-oestrogenic effects present in plant foods as constituents or contaminants, and to identify and disseminate in vitro and in

  1. Upstream waves at Mercury, Venus and earth - Comparison of the properties of one Hertz waves

    Science.gov (United States)

    Orlowski, D. S.; Crawford, G. K.; Russell, C. T.

    1990-01-01

    Previous studies have shown that the Venus foreshock region contains low-frequency upstream waves similar to those in the terrestrial foreshock, but perhaps with different amplitudes than at earth. This paper compares the properties of a second class of upstream waves, analogous to the so-called 1 Hz waves at earth. The waves observed at Mercury, Venus, and earth have very similar properties, i.e., propagation angles less than 55 degrees to the magnetic field and less than 35 degrees to the solar wind flow direction. The waves occur exclusively on the field lines connected to the bow shock. They are most commonly left-hand elliptically polarized with similar fractional amplitudes, approximately 0.1 of the background field strength. Their amplitudes decrease with increasing distance from the shock. The observed frequencies are similar for Mercury, Venus, and earth when scaled by the interplanetary magnetic field. If, as generally assumed at earth, these waves arise in regions of backstreaming electrons, these results imply that similar electron foreshocks occur at earth, Venus and Mercury despite differences in bow shock size and the nature of the obstacle to the solar wind.

  2. Radioisotope Stirling Engine Powered Airship for Low Altitude Operation on Venus

    Science.gov (United States)

    Colozza, Anthony J.

    2012-01-01

    The feasibility of a Stirling engine powered airship for the near surface exploration of Venus was evaluated. The heat source for the Stirling engine was limited to 10 general purpose heat source (GPHS) blocks. The baseline airship utilized hydrogen as the lifting gas and the electronics and payload were enclosed in a cooled insulated pressure vessel to maintain the internal temperature at 320 K and 1 Bar pressure. The propulsion system consisted of an electric motor driving a propeller. An analysis was set up to size the airship that could operate near the Venus surface based on the available thermal power. The atmospheric conditions on Venus were modeled and used in the analysis. The analysis was an iterative process between sizing the airship to carry a specified payload and the power required to operate the electronics, payload and cooling system as well as provide power to the propulsion system to overcome the drag on the airship. A baseline configuration was determined that could meet the power requirements and operate near the Venus surface. From this baseline design additional trades were made to see how other factors affected the design such as the internal temperature of the payload chamber and the flight altitude. In addition other lifting methods were evaluated such as an evacuated chamber, heated atmospheric gas and augmented heated lifting gas. However none of these methods proved viable.

  3. Kepler-1649b: An Exo-Venus in the Solar Neighborhood

    Energy Technology Data Exchange (ETDEWEB)

    Angelo, Isabel; Rowe, Jason F.; Huber, Daniel [SETI Institute, Mountain View, CA 94043 (United States); Howell, Steve B.; Quintana, Elisa V.; Burningham, Ben; Barclay, Thomas [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Still, Martin [Bay Area Environmental Research Institute, 625 2nd Street, Suite 209, Petaluma, CA 94952 (United States); Mann, Andrew W. [Department of Astronomy, The University of Texas at Austin, Austin, TX 78712 (United States); Ciardi, David R. [NASA Exoplanet Science Institute/Caltech, Pasadena, CA (United States); Kane, Stephen R., E-mail: isabelangelo@berkeley.edu [Department of Physics and Astronomy, San Francisco State University, 1600 Holloway Avenue, San Francisco, CA 94132 (United States)

    2017-04-01

    The Kepler mission has revealed that Earth-sized planets are common, and dozens have been discovered to orbit in or near their host star’s habitable zone. A major focus in astronomy is to determine which of these exoplanets are likely to have Earth-like properties that are amenable to follow-up with both ground- and future space-based surveys, with an ultimate goal of probing their atmospheres to look for signs of life. Venus-like atmospheres will be of particular interest in these surveys. While Earth and Venus evolved to have similar sizes and densities, it remains unclear what factors led to the dramatic divergence of their atmospheres. Studying analogs to both Earth and Venus can thus shed light on the limits of habitability and the potential for life on known exoplanets. Here, we present the discovery and confirmation of Kepler-1649b, an Earth-sized planet orbiting a nearby M5V star that receives incident flux at a level similar to that of Venus. We present our methods for characterizing the star, using a combination of point-spread function photometry, ground-based spectroscopy, and imaging, to confirm the planetary nature of Kepler-1649b. Planets like Kepler-1649b will be prime candidates for atmospheric and habitability studies in the next generation of space missions.

  4. CUVE - Cubesat UV Experiment: Unveil Venus' UV Absorber with Cubesat UV Mapping Spectrometer

    Science.gov (United States)

    Cottini, V.; Aslam, S.; D'Aversa, E.; Glaze, L.; Gorius, N.; Hewagama, T.; Ignatiev, N.; Piccioni, G.

    2017-09-01

    Our Venus mission concept Cubesat UV Experiment (CUVE) is one of ten proposals selected for funding by the NASA PSDS3 Program - Planetary Science Deep Space SmallSat Studies. CUVE concept is to insert a CubeSat spacecraft into a Venusian orbit and perform remote sensing of the UV spectral region using a high spectral resolution point spectrometer to resolve UV molecular bands, observe nightglow, and characterize the unidentified main UV absorber. The UV spectrometer is complemented by an imaging UV camera with multiple bands in the UV absorber main band range for contextual imaging. CUVE Science Objectives are: the nature of the "Unknown" UV-absorber; the abundances and distributions of SO2 and SO at and above Venus's cloud tops and their correlation with the UV absorber; the atmospheric dynamics at the cloud tops, structure of upper clouds and wind measurements from cloud-tracking; the nightglow emissions: NO, CO, O2. This mission will therefore be an excellent platform to study Venus' cloud top atmospheric properties where the UV absorption drives the planet's energy balance. CUVE would complement past, current and future Venus missions with conventional spacecraft, and address critical science questions cost effectively.

  5. Did Ibn Sina Observe the Transit of Venus of 1032 CE?

    Science.gov (United States)

    Kapoor, R. C.

    2012-09-01

    The Persian polymath Abu Ali ibn Sina (980--1037 CE), known to early Western sources as Avicenna, records that ``I say that I saw Venus as a spot on the surface of the sun''. This statement has been quoted, for example, by Nasir al Din al Tusi (1201--1274 CE). A Transit of Venus indeed took place during ibn Sina's life time, that is on 24 May 1032 CE. Did ibn Sina see this Transit or did he merely see a sunspot? The question was addressed by Bernard R. Goldstein in 1969 who concluded that ``this Transit may not have been visible where he lived''. Goldstein based his conclusion on the input provided by Brian G Marsden who in turn used mathematical tables prepared by J. Meeus in 1958. I have begun re-examination of the question by employing Fred Espenak's Transit predictions. Preliminary work shows that ibn Sina could indeed have obtained a glimpse of the Transit of Venus just before sunset from places like Isfahan or Hamadan. In other words, when ibn Sina said he saw Venus on the surface of the Sun, he probably meant it.

  6. Understanding divergent evolution of Earth-like planets: the case for a Venus exploration program

    Science.gov (United States)

    Crisp, D.

    2002-01-01

    Here, we propose a Venus exploration program designed to explain the origin and divergent evolution of the interiors, surfaces, and atmospheres of the terrestrial planets in our solar system, and provide greater insight into the conditions that may affect the habitability of terrestrial planets in other solar systems.

  7. Investigating the Origin and Evolution of Venus with In Situ Mass Spectrometry

    Science.gov (United States)

    Trainer, M. G.; Mahaffy, P. R.; Brinckerhoff, W. B.; Johnson, N. M.; Glaze, L. S.

    2015-01-01

    Measurement of noble gas abundances on Venus remain a high priority for planetary science. These studies are only possible through in situ measurement, and can be accomplished by a modern neutral mass spectrometer (NMS) such as that developed at NASA Goddard, based on flight-proven technology. Here we show how the measurement of noble gases can be secured using demonstrated enrichment techniques.

  8. Getting boards on board: engaging governing boards in quality and safety.

    Science.gov (United States)

    Conway, James

    2008-04-01

    As hospitals seek to drive rapid quality improvement, boards have an opportunity-and a significant responsibility--to make better quality of care the organization's top priority. "Six things all boards should do to improve quality and reduce harm" are recommended: (1) setting aims--set a specific aim to reduce harm this year; make an explicit, public commitment to measurable quality improvement; (2) getting data and hearing stories--select and review progress toward safer care as the first agenda item at every board meeting, grounded in transparency--and putting a "human face" on harm data; (3) establishing and monitoring system-level measures--identify a small group of organizationwide "roll-up" measures of patient safety that are continually updated and are made transparent to the entire organization and its customers; (4) changing the environment, policies, and culture--commit to establish and maintain an environment that is respectful, fair, and just for all who experience the pain and loss as a result of avoidable harm and adverse outcomes: the patients, their families, and the staff at the sharp end of error; (5) learning, starting with the board--develop the board's capability and learn about how "best-in-the-world" boards work with executive and medical staff leaders to reduce harm; (6) establishing executive accountability--oversee the effective execution of a plan to achieve aims to reduce harm, including executive team accountability for clear quality improvement targets.

  9. The Dutch 'Female Board Index' 2009

    NARCIS (Netherlands)

    Lückerath – Rovers, M.

    2009-01-01

    This report gives an overview of the presence of women in the Executive Board and Supervisory Board (together: 'the Board') of Dutch listed companies per September 2009. The companies have been ranked by the percentage women in the Board. A difference analysis has been made at personal level

  10. Better Board Meetings in Less Time.

    Science.gov (United States)

    Botch, Ray; Cartwright, Janet

    Based upon the experiences of Black Hawk College (BHC), this two-part report presents guidelines for the effective administration of the meetings of a college's board of trustees. The report first discusses board composition and argues that large boards only complicate and slow down the decision-making process. Specific board responsibilities are…

  11. 7 CFR 930.2 - Board.

    Science.gov (United States)

    2010-01-01

    ... 7 Agriculture 8 2010-01-01 2010-01-01 false Board. 930.2 Section 930.2 Agriculture Regulations of the Department of Agriculture (Continued) AGRICULTURAL MARKETING SERVICE (Marketing Agreements and... Definitions § 930.2 Board. Board means the Cherry Industry Administrative Board established pursuant to § 930...

  12. 7 CFR 982.18 - Board.

    Science.gov (United States)

    2010-01-01

    ... Order Regulating Handling Definitions § 982.18 Board. Board means the Hazelnut Marketing Board... 7 Agriculture 8 2010-01-01 2010-01-01 false Board. 982.18 Section 982.18 Agriculture Regulations of the Department of Agriculture (Continued) AGRICULTURAL MARKETING SERVICE (Marketing Agreements and...

  13. Presidential Search: An Overview for Board Members

    Science.gov (United States)

    Association of Governing Boards of Universities and Colleges, 2012

    2012-01-01

    The selection of a president is a governing board's most important responsibility, and the search process is the board's best opportunity to help guide its institution into a successful new era. This guide outlines the leadership roles during a search (those of the board, the board chair, the search committee, and others), briefs board…

  14. 22 CFR 902.3 - Board staff.

    Science.gov (United States)

    2010-04-01

    ... 22 Foreign Relations 2 2010-04-01 2010-04-01 true Board staff. 902.3 Section 902.3 Foreign Relations FOREIGN SERVICE GRIEVANCE BOARD ORGANIZATION § 902.3 Board staff. The chairperson shall select the Board's executive secretary and other staff provided for in the Act. The executive secretary and staff...

  15. Advisory Boards: Gateway to Business Engagement

    Science.gov (United States)

    Meeder, Hans; Pawlowski, Brett

    2012-01-01

    Interest has been growing in how to build or manage an effective business advisory board. Developing an advisory board is crucial to keeping CTE programs relevant and viable by engaging the support of business and industry. This article delves into how to build and manage a board, and how to re-energize boards that already exist but may be lacking.

  16. 22 CFR 401.28 - Advisory boards.

    Science.gov (United States)

    2010-04-01

    ... 22 Foreign Relations 2 2010-04-01 2010-04-01 true Advisory boards. 401.28 Section 401.28 Foreign Relations INTERNATIONAL JOINT COMMISSION, UNITED STATES AND CANADA RULES OF PROCEDURE References § 401.28 Advisory boards. (a) The Commission may appoint a board or boards, composed of qualified persons, to...

  17. Plume-induced subduction and accretion on present-day Venus and Archean Earth

    Science.gov (United States)

    Davaille, A.; Smrekar, S. E.; Sibrant, A.; Mittelstaedt, E. L.

    2017-12-01

    Plate tectonics is responsible for the majority of Earth's heat loss, cycling of volatiles between the atmosphere and interior, recycling in the mantle of most of the surface plates, and possibly even for maintaining habitability. Despite its similarity in size and bulk density to Earth, Venus lacks plate tectonics today, and its mode of operation remains debated. Using laboratory experiments in colloidal dispersion which brittle viscosity-elasto-plastic rheology, we recently showed that plume-induced subduction could be operating nowadays on Venus. The experimental fluids were heated from below to produce upwelling plumes, which in turn produced tensile fractures in the lithosphere-like skin that formed on the upper surface. Plume material upwelling through the fractures then spread above the skin, analogous to volcanic flooding, and lead to bending and eventual subduction of the skin along arcuate segments. These segments are analogous to the semi-circular trenches seen on large coronae. Scaling analysis suggests that this regime with limited, plume-induced subduction is favored by a hot lithosphere, such as that found on early Earth or present-day Venus. Moreover, in this regime, subduction proceeds primarily by roll-back and the coronae expands through time at velocity that could reach 10 cm/yr. A second set of experiments focusing on accretion processes suggests that accretion dynamics depends on the strength of the lithosphere, as well as the spreading velocity. Venus hot surface temperature would act to decrease the lithosphere strength, and therefore weaken the ridge axis, that would become highly unstable, showing large sinuosity and producing a number of micro-plates. These plume, subduction, and accretion characteristics explain well the features seen in Artemis coronae, the largest coronae on Venus.

  18. Venus O2 visible and IR nightglow: Implications for lower thermosphere dynamics and chemistry

    Science.gov (United States)

    Bougher, S. W.; Borucki, W. J.

    1994-01-01

    The National Center for Atmospheric Research thermospheric general circulation model for the Venus thermosphere is modified to examine two observed night airglow features, both of which serve as sensitive tracers of the thermospheric circulation. New O2 nightglow data from the Pioneer Venus Orbiter (PVO) star tracker (O2 Herzberg II at 400-800 nm) and ground-based telescopes (O2 IR at 1.27 microns) yield additional model constraints for estimating Venus winds over 100-130 km. Atomic oxygen, produced by dayside CO2 photolysis peaking near 110 km, and transported to the nightside by the global wind system, is partially destroyed through three-body recombination, yielding the O2 Herzberg II visible nightglow. This emission is very sensitive to horizontal winds at altitudes between 100 and 130 km. Other trace species catalytic reactions also contribute to the production of the very strong nightside infrared (1.27 microns) emission. This paper examines the dynamical and chemical implications of these new data using the Venus thermospheric general circulation model (VTGCM) as an analysis tool. Three-dimensional calculations are presented for both solar maximum and solar medium conditions, corresponding to early PVO (1979-1981) and PVO entry (mid-1992) time periods. Very distinct periods are identified in which zonal winds are alternately weak and strong in the Venus lower thermosphere. VTGCM sensitivity studies are conducted to assess the impacts of potential changes in thermospheric zonal and day-to-night winds, and eddy diffusion on the corresponding nightglow intensities. It appears that cyclostrophic balance extends above 80 km periodically, owing to a reversal of the upper mesosphere latitudinal temperature gradient, and thereby producing strong zonal winds and correspondingly modified O2 nightglow distributions that are observed.

  19. Feasibility Study of Venus Surfuce Cooling Using Chemical Reactions with the Atmosphere

    Science.gov (United States)

    Evans, Christopher

    2013-01-01

    A literature search and theoretical analysis were conducted to investigate the feasibility of cooling a craft on Venus through chemical reformation of materials from the atmosphere. The core concept was to take carbon dioxide (CO2) from the Venus atmosphere and chemically reform it into simpler compounds such as carbon, oxygen, and carbon monoxide. This process is endothermic, taking energy from the surroundings to produce a cooling effect. A literature search was performed to document possible routes for achieving the desired reactions. Analyses indicated that on Venus, this concept could theoretically be used to produce cooling, but would not perform as well as a conventional heat pump. For environments other than Venus, the low theoretical performance limits general applicability of this concept, however this approach to cooling may be useful in niche applications. Analysis indicated that environments with particular atmospheric compositions and temperatures could allow a similar cooling system to operate with very good performance. This approach to cooling may also be useful where the products of reaction are also desirable, or for missions where design simplicity is valued. Conceptual designs for Venus cooling systems were developed using a modified concept, in which an expendable reactant supply would be used to promote more energetically favorable reactions with the ambient CO2, providing cooling for a more limited duration. This approach does not have the same performance issues, but the use of expendable supplies increases the mass requirements and limits the operating lifetime. This paper summarizes the findings of the literature search and corresponding analyses of the various cooling options

  20. Feasibility Study of Venus Surface Cooling Using Chemical Reactions with the Atmosphere

    Science.gov (United States)

    Evans, Christopher

    2013-01-01

    A literature search and theoretical analysis were conducted to investigate the feasibility of cooling a craft on Venus through chemical reformation of materials from the atmosphere. The core concept was to take carbon dioxide (CO2) from the Venus atmosphere and chemically reform it into simpler compounds such as carbon, oxygen, and carbon monoxide. This process is endothermic, taking energy from the surroundings to produce a cooling effect. A literature search was performed to document possible routes for achieving the desired reactions. Analyses indicated that on Venus, this concept could theoretically be used to produce cooling, but would not perform as well as a conventional heat pump. For environments other than Venus, the low theoretical performance limits general applicability of this concept, however this approach to cooling may be useful in niche applications. Analysis indicated that environments with particular atmospheric compositions and temperatures could allow a similar cooling system to operate with very good performance. This approach to cooling may also be useful where the products of reaction are also desirable, or for missions where design simplicity is valued. Conceptual designs for Venus cooling systems were developed using a modified concept, in which an expendable reactant supply would be used to promote more energetically favorable reactions with the ambient CO2, providing cooling for a more limited duration. This approach does not have the same performance issues, but the use of expendable supplies increases the mass requirements and limits the operating lifetime. This paper summarizes the findings of the literature search and corresponding analyses of the various cooling options.

  1. Exploring the Venus global super-rotation using a comprehensive general circulation model

    Science.gov (United States)

    Mendonça, J. M.; Read, P. L.

    2016-12-01

    The atmospheric circulation in Venus is well known to exhibit strong super-rotation. However, the atmospheric mechanisms responsible for the formation of this super-rotation are still not fully understood. In this work, we developed a new Venus general circulation model to study the most likely mechanisms driving the atmosphere to the current observed circulation. Our model includes a new radiative transfer, convection and suitably adapted boundary layer schemes and a dynamical core that takes into account the dependence of the heat capacity at constant pressure with temperature. The new Venus model is able to simulate a super-rotation phenomenon in the cloud region quantitatively similar to the one observed. The mechanisms maintaining the strong winds in the cloud region were found in the model results to be a combination of zonal mean circulation, thermal tides and transient waves. In this process, the semi-diurnal tide excited in the upper clouds has a key contribution in transporting axial angular momentum mainly from the upper atmosphere towards the cloud region. The magnitude of the super-rotation in the cloud region is sensitive to various radiative parameters such as the amount of solar radiative energy absorbed by the surface, which controls the static stability near the surface. In this work, we also discuss the main difficulties in representing the flow below the cloud base in Venus atmospheric models. Our new radiative scheme is more suitable for 3D Venus climate models than those used in previous work due to its easy adaptability to different atmospheric conditions. This flexibility of the model was crucial to explore the uncertainties in the lower atmospheric conditions and may also be used in the future to explore, for example, dynamical-radiative-microphysical feedbacks.

  2. The new Board of Governors

    International Nuclear Information System (INIS)

    1964-01-01

    Full text: Miss Blanche Margaret Meagher was elected chairman of the IAEA Board of Governors for 1964-65, after the new Board had been constituted at the Eighth Session of the General Conference in September. Since 1962 Miss Meagher has been Canadian Ambassador to Austria, and Canadian Governor of the Agency. Miss Meagher joined the Canadian Department of External Affairs in 1942, and has held a number of foreign diplomatic appointments; she has also served on Canadian delegations to the UN Educational, Scientific and Cultural Organization, the International Telecommunication Union, the Economic and Social Council of UN and the UN Disarmament Sub-Committee. The Vice-Chairmen of the Board are Mr. Wilhelm Billig (Poland) and Mr. Hassan M. Tohamy (UAR). Mr. Billig is Chairman of the State Council for Atomic Energy, and High Commissioner for Peaceful Uses of Atomic Energy. Mr. Tohamy is Ambassador to Austria, and Resident Representative to the Agency. Of the twelve elected members of the Board, five were chosen by the General Conference in 1964 for two years, viz. Argentina, Chile, Netherlands, Thailand and the United Arab Republic. Seven were elected in 1963: Afghanistan, China, Congo (Leopoldville), Morocco, Romania, Switzerland and Uruguay. The remaining thirteen members have been designated by the Board: Australia, Belgium, Brazil, Canada, Finland, France, India, Japan, Poland, South Africa, USSR, United Kingdom and United States. (author)

  3. 78 FR 63265 - Self-Regulatory Organizations; Chicago Board Options Exchange, Incorporated; Notice of Filing and...

    Science.gov (United States)

    2013-10-23

    ... strike prices expressed in percentage terms. Values for such options are expressed in percentage terms... from one day to the next when values are expressed in percentage terms. The fees that MDX charges for...'s Statement of the Terms of Substance of the Proposed Rule Change Chicago Board Options Exchange...

  4. 29 CFR 4002.3 - Board of Directors, Chair, and Representatives of Board Members.

    Science.gov (United States)

    2010-07-01

    ... 29 Labor 9 2010-07-01 2010-07-01 false Board of Directors, Chair, and Representatives of Board... CORPORATION GENERAL BYLAWS OF THE PENSION BENEFIT GUARANTY CORPORATION § 4002.3 Board of Directors, Chair, and... Labor shall be the Chair of the Board of Directors and shall call and preside over all Board meetings...

  5. Institutional Evolution and Corporate Boards

    DEFF Research Database (Denmark)

    Chen, Victor Zitian; Hobdari, Bersant; Sun, Pei

    2014-01-01

    We argue that corporate boards are a dynamic repository of human- and social capital in response to external institutional evolution. Theoretically, integrating institutional economics, agency theory and resource dependence theory, we explain that evolution of market-, legal- and political...... institutions restructures the particular context in which board members play their two primary roles: monitoring the CEO on behalf of the shareholders, suggested by the agency theory, and supporting the CEO by providing resources, knowledge and information, suggested by the resource dependence theory......, since the board changes are typically proposed by the block shareholders, whose motivation for doing so is closely associated with a corporation’s financial performance, we further argue that financial performance is a key moderator of the relationships between institutional evolution and changes...

  6. Controlling electronics boards with PVSS

    CERN Document Server

    Jacobsson, Richard

    2005-01-01

    This paper addresses several aspects of implementing a control system for electronics boards in order to perform remote Field Programmable Gate Array (FPGA) programming, hardware configuration, register control, and monitoring, as well as interfacing it to an expert system. The paper presents an implementation, using the Distributed Information Management (DIM) package and the industrial SCADA system PVSS II from ETM, in which the access mechanisms to the board resources are completely generic and in which the device prescription and the handling of mapping between functional parameters and physical registers follow a common structure independent of the board type. The control system also incorporates mechanisms by which it may be controlled from a finite state machine based expert system. Finally the paper suggests an improvement in which the mapping between logical parameters and physical registers is represented by descriptors in the device description such that the translation can be handled by a common m...

  7. A study of an orbital radar mapping mission to Venus. Volume 2: Configuration comparisons and systems evaluation

    Science.gov (United States)

    1973-01-01

    Configuration comparisons and systems evaluation for the orbital radar mapping mission of the planet Venus are discussed. Designs are recommended which best satisfy the science objectives of the Venus radar mapping concept. Attention is given to the interaction and integration of those specific mission-systems recommendations with one another, and the final proposed designs are presented. The feasibility, cost, and scheduling of these configurations are evaluated against assumptions of reasonable state-of-the-art growth and space funding expectations.

  8. Foxa2-venus fusion reporter mouse line allows live-cell analysis of endoderm-derived organ formation.

    Science.gov (United States)

    Burtscher, Ingo; Barkey, Wenke; Lickert, Heiko

    2013-08-01

    The Foxa2-winged helix/forkhead box transcription factor (TF) is absolutely required for endoderm formation and organogenesis. Foxa2 plays essential roles during lung, liver, pancreas, and gastrointestinal tract development and regulates cell-type specific programs in the adult organism. To specifically address Foxa2 function during organ development and homeostasis, we generated a Foxa2-Venus fusion (FVF) reporter protein by gene targeting in embryonic stem (ES) cells. The FVF knock-in reporter is expressed under endogenous Foxa2 control and the fluorescent protein fusion does not interfere with TF function, as homozygous mice are viable and fertile. Moreover, the FVF protein localizes to the nucleus, associates with chromatin during mitosis, and reflects the endogenous Foxa2 protein distribution pattern in several tissues in heterozygous animals. Importantly, live-cell imaging on single-cell level of the FVF and Sox17-Cherry fusion double knock-in reporter ES cell line reveals the dynamics of endoderm TF accumulation during ES cell differentiation. The FVF reporter also allowed us to identify the endoderm progenitors during gastrulation and to visualize the different branching morphogenesis modes of the lung and pancreas epithelium in ex vivo embryo and organ cultures. In summary, the generation of the FVF reporter line adds an important new tool to visualize and analyse endoderm-derived organ development and homeostasis on the cellular and molecular level. Copyright © 2013 Wiley Periodicals, Inc.

  9. Effects of variation in coagulation and photochemistry parameters on the particle size distributions in the Venus clouds

    Science.gov (United States)

    McGouldrick, Kevin

    2017-12-01

    This paper explores the effects that variation in the coalescence efficiency of the Venus cloud particles can have on the structure of the Venus cloud. It is motivated by the acknowledgment of uncertainties in the measured parameters—and the assumptions made to account for them—that define our present knowledge of the particle characteristics. Specifically, we explore the consequence of allowing the coalescence efficiency of supercooled sulfuric acid in the upper clouds to tend to zero. This produces a cloud that occasionally exhibits an enhancement of small particles at altitude (similar to the upper hazes observed by Pioneer Venus and subsequently shown to be somewhat transient). This simulated cloud occasionally exhibits a rapid growth of particle size near cloud base, exhibiting characteristics similar to those seen in the controversial Mode 3 particles. These results demonstrate that a subset of the variations observed as near-infrared opacity variations in the lower and middle clouds of Venus can be explained by microphysical, in addition to dynamical, variations. Furthermore, the existence of a population of particles exhibiting less efficient coalescence efficiencies would support the likelihood of conditions suitable for charge exchange, hence lightning, in the Venus clouds. We recommend future laboratory studies on the coalescence properties of sulfuric acid under the range of conditions experienced in the Venus clouds. We also recommend future in situ measurements to better characterize the properties of the cloud particles themselves, especially composition and particle habits (shapes).[Figure not available: see fulltext.

  10. Seismic generated infrasounds on Telluric Planets: Modeling and comparisons between Earth, Venus and Mars

    Science.gov (United States)

    Lognonne, P. H.; Rolland, L.; Karakostas, F. G.; Garcia, R.; Mimoun, D.; Banerdt, W. B.; Smrekar, S. E.

    2015-12-01

    Earth, Venus and Mars are all planets in which infrasounds can propagate and interact with the solid surface. This leads to infrasound generation for internal sources (e.g. quakes) and to seismic waves generations for atmospheric sources (e.g. meteor, impactor explosions, boundary layer turbulences). Both the atmospheric profile, surface density, atmospheric wind and viscous/attenuation processes are however greatly different, including major differences between Mars/Venus and Earth due to the CO2 molecular relaxation. We present modeling results and compare the seismic/acoustic coupling strength for Earth, Mars and Venus. This modeling is made through normal modes modelling for models integrating the interior, atmosphere, both with realistic attenuation (intrinsic Q for solid part, viscosity and molecular relaxation for the atmosphere). We complete these modeling, made for spherical structure, by integration of wind, assuming the later to be homogeneous at the scale of the infrasound wavelength. This allows us to compute either the Seismic normal modes (e.g. Rayleigh surface waves), or the acoustic or the atmospheric gravity modes. Comparisons are done, for either a seismic source or an atmospheric source, on the amplitude of expected signals as a function of distance and frequency. Effects of local time are integrated in the modeling. We illustrate the Rayleigh waves modelling by Earth data (for large quakes and volcanoes eruptions). For Venus, very large coupling can occur at resonance frequencies between the solid part and atmospheric part of the planet through infrasounds/Rayleigh waves coupling. If the atmosphere reduced the Q (quality coefficient) of Rayleigh waves in general, the atmosphere at these resonance soffers better propagation than Venus crust and increases their Q. For Mars, Rayleigh waves excitations by atmospheric burst is shown and discussed for the typical yield of impacts. The new data of the Nasa INSIGHT mission which carry both seismic and

  11. A pattern recognition system for locating small volvanoes in Magellan SAR images of Venus

    Science.gov (United States)

    Burl, M. C.; Fayyad, U. M.; Smyth, P.; Aubele, J. C.; Crumpler, L. S.

    1993-01-01

    The Magellan data set constitutes an example of the large volumes of data that today's instruments can collect, providing more detail of Venus than was previously available from Pioneer Venus, Venera 15/16, or ground-based radar observations put together. However, data analysis technology has not kept pace with data collection and storage technology. Due to the sheer size of the data, complete and comprehensive scientific analysis of such large volumes of image data is no longer feasible without the use of computational aids. Our progress towards developing a pattern recognition system for aiding in the detection and cataloging of small-scale natural features in large collections of images is reported. Combining classical image processing, machine learning, and a graphical user interface, the detection of the 'small-shield' volcanoes (less than 15km in diameter) that constitute the most abundant visible geologic feature in the more that 30,000 synthetic aperture radar (SAR) images of the surface of Venus are initially targeted. Our eventual goal is to provide a general, trainable tool for locating small-scale features where scientists specify what to look for simply by providing examples and attributes of interest to measure. This contrasts with the traditional approach of developing problem specific programs for detecting Specific patterns. The approach and initial results in the specific context of locating small volcanoes is reported. It is estimated, based on extrapolating from previous studies and knowledge of the underlying geologic processes, that there should be on the order of 10(exp 5) to 10(exp 6) of these volcanoes visible in the Magellan data. Identifying and studying these volcanoes is fundamental to a proper understanding of the geologic evolution of Venus. However, locating and parameterizing them in a manual manner is forbiddingly time-consuming. Hence, the development of techniques to partially automate this task were undertaken. The primary

  12. Joint Advisory Appeals Board report

    CERN Document Server

    Lalande, Amanda

    2018-01-01

    With regard to the internal appeal procedure, Article R VI 1.18 of the Staff Rules and Regulations states that unless the member of the personnel objects, (the) decision and report of the JAAB (Joint Advisory Appeals Board) shall be brought to the attention of the members of the personnel.

  13. The importance of board independence

    NARCIS (Netherlands)

    Zijl, N.J.M.

    2012-01-01

    Although the attributed importance of board independence is high, a clear definition of independence does not exist. Furthermore, the aim and consequences of independence are the subject of discussion and empirical evidence about the impact of independence is weak and disputable. Despite this lack

  14. The Audit Committee. Board Basics

    Science.gov (United States)

    Ostrom, John S.

    2004-01-01

    The Effective Committees set of booklets comprises publications on the following committees: investment, buildings and grounds, academic affairs, student affairs, finance, development, trustees, audit, compensation, and executive. It is part of the AGB Board Basics Series. This report describes the primary role of an audit committee. The primary…

  15. School Board Ethics and Effectiveness

    Science.gov (United States)

    Feuerstein, Abe

    2009-01-01

    Since the early 1980s, educational policy has increasingly been focused on improving student performance (Conley, 2003, Murphy, 1990). School governance in general, and school boards in particular, have often been viewed as either the means of implementing needed reforms or as roadblocks in their way (Boyd, 2003; Delagardelle, M.; 2008; Howell,…

  16. Where do international board members come from? Country-level antecedents of international board member selection in European boards

    NARCIS (Netherlands)

    van Veen, Kees; Sahib, Padma Rao; Aangeenbrug, Evelien

    In this paper, it is argued that boards internationalize by recruiting international directors in order to increase companies' performance. However, increasing nationality diversity on a board can be costly considering that it potentially creates cooperative problems on a board due to fault-lines

  17. Observation of intense wave bursts at very low altitudes within the Venus nightside ionosphere

    Science.gov (United States)

    Strangeway, R. J.; Russell, C. T.; Ho, C. M.

    1993-12-01

    Intense ELF (100 Hz) bursts were detected by the Pioneer Venus (PV) Orbiter plasma wave instrument during the final operations of the spacecraft prior to atmospheric entry. These bursts were detected at approx. 130 km altitude around 0400 local time. The wave activity lasted for several tens of seconds. Furthermore the bursts were not symmetric about periapsis, unlike instrument noise caused by neutral impacts on the spacecraft. The bursts had a vertical attenuation scale height of the order 1 km, consistent with that expected for whistler-mode waves propagating through a collisional ionosphere. Since the decay of the signals appears to be due to attenuation, the source must persist for several tens of seconds. The wave bursts could therefore be the signature of electromagnetic radiation entering the bottomside ionosphere from several distant sources, as would be expected if lightning were a relatively persistent phenomenon within the Venus atmosphere.

  18. Regional fracture patterns around volcanoes: Possible evidence for volcanic spreading on Venus

    Science.gov (United States)

    López, I.; Lillo, J.; Hansen, V. L.

    2008-06-01

    Magellan data show that the surface of Venus is dominated by volcanic landforms including large flow fields and a wide range of volcanic edifices that occur in different magmatic and tectonic environments. This study presents the results from a comprehensive survey of volcano-rift interaction in the BAT region and its surroundings. We carried out structural mapping of examples where interaction between volcanoes and regional fractures results in a deflection of the fractures around the volcanic features and discuss the nature of the local volcano-related stress fields that might be responsible for the observed variations of the regional fracture systems. We propose that the deflection of the regional fractures around these venusian volcanoes might be related to volcanic spreading, a process recognized as of great importance in the tectonic evolution of volcanoes on Earth and Mars, but not previously described on Venus.

  19. Effects of inclination and eccentricity on optimal trajectories between earth and Venus

    Science.gov (United States)

    Gravier, J.-P.; Marchal, C.; Culp, R. D.

    1973-01-01

    The true optimal transfers, including the effects of the inclination and eccentricity of the planets' orbits, between earth and Venus are presented as functions of the corresponding idealized Hohmann transfers. The method of determining the optimal transfers using the calculus of variations is presented. For every possible Hohmann window, specified as a continuous function of the longitude of perihelion of the Hohmann trajectory, the corresponding numerically exact optimal two-impulse transfers are given in graphical form. The cases for which the optimal two-impulse transfer is the absolute optimal, and those for which a three-impulse transfer provides the absolute optimal transfer are indicated. This information furnishes everything necessary for quick and accurate orbit calculations for preliminary Venus mission analysis. This makes it possible to use the actual optimal transfers for advanced planning in place of the standard Hohmann transfers.

  20. The twin sister planets Venus and Earth why are they so different?

    CERN Document Server

    Malcuit, Robert J

    2014-01-01

    This book explains how it came to be that Venus and Earth, while very similar in chemical composition, zonation, size and heliocentric distance from the Sun, are very different in surface environmental conditions. It is argued here that these differences can be accounted for by planetoid capture processes and the subsequent evolution of the planet-satellite system. Venus captured a one-half moon-mass planetoid early in its history in the retrograde direction and underwent its "fatal attraction scenario" with its satellite (Adonis). Earth, on the other hand, captured a moon-mass planetoid (Luna) early in its history in prograde orbit and underwent a benign estrangement scenario with its captured satellite.

  1. How the Venus flytrap actively snaps: hydrodynamic measurements at the cellular level

    Science.gov (United States)

    Colombani, Mathieu; Forterre, Yoel; GEP Team

    2012-11-01

    Although they lack muscle, plants have evolved a remarkable range of mechanisms to create rapid motion, from the rapid folding of sensitive plants to seed dispersal. Of these spectacular examples that have long fascinated scientists, the carnivorous plant Venus flytrap, whose leaves snap together in a fraction of second to capture insects, has long been a paradigm for study. Recently, we have shown that this motion involves a snap-buckling instability due to the shell-like geometry of the leaves of the trap. However, the origin of the movement that allows the plant to cross the instability threshold and actively bend remains largely unknown. In this study, we investigate this active motion using a micro-fluidic pressure probe that gives direct hydraulic and mechanical measurements at the cellular level (osmotic pressure, cell membrane permeability, cell wall elasticity). Our results challenge the role of osmotically-driven water flows usually put forward to explain Venus flytrap's active closure.

  2. Scientific Advisory Board FY92 Annual Report.

    Science.gov (United States)

    1993-03-01

    Implementation Board for the North American Waterfowl Management Plan; Chairman, Chief of Engineers’ Environmental Advisory Board. Awards: Aldo ... Leopold Medal, Wildlife Society; Barbara Swain Medal, Natural Resources Council of America. Authored numerous papers and reports, assisted editing and

  3. Sustainability issues in circuit board recycling

    DEFF Research Database (Denmark)

    Legarth, Jens Brøbech; Alting, Leo; Baldo, Gian Luca

    1995-01-01

    The resource recovery and environmental impact issues of printed circuit board recycling by secondary copper smelters are discussed. Guidelines concerning material selection for circuit board manufacture and concerning the recycling processes are given to enhance recovery efficiency and to lower...

  4. 75 FR 67351 - Environmental Management Advisory Board

    Science.gov (United States)

    2010-11-02

    ... Environmental Management Advisory Board AGENCY: Department of Energy. ACTION: Notice of Open Teleconference. SUMMARY: This notice announces a teleconference of the Environmental Management Advisory Board (EMAB). The... is to provide the Assistant Secretary for Environmental Management (EM) with advice and...

  5. WEGENER: Solid Body Dynamics Investigation of Venus. Results from Summer School Alpbach 2014.

    Science.gov (United States)

    Bialek, A.; Coyle, S.; Czeluschke, A.; Donaldson Hanna, K.; Donohoe, A.; Hu, H.; Koopmans, R.-J.; Lucchetti, A.; Mannel, T.; Nachon, M.; Nilsson, D.; Shelakhaev, N.; Suer, A.; Timoney, R.

    2015-10-01

    The work presented in this paper was performed by the Orange Team during Summer School Alpbach 2014, which mainly concerns about geophysics of terrestrial planets. A mission is designed to investigate the past and current tectonic and volcanic activity on Venus. During the mission, a simultaneous observations from topographic, magnetic and gravitational measurements will be performed and the combination of the information has the potential to provide an improved understanding of the formation and evolution of the planet.

  6. Effects of selective fusion on the thermal history of the Moon, Mars, and Venus

    Science.gov (United States)

    Lee, W.H.K.

    1968-01-01

    A comparative study on the thermal history of the Moon, Mars, and Venus was made by numerical solutions of the heat equation including and excluding selective fusion of silicates. Selective fusion was approximated by melting in a multicomponent system and redistribution of radioactive elements. Effects on selective fusion on the thermal models are (1) lowering (by several hundred degrees centigrade) and stabilizing the internal temperature distribution, and (2) increasing the surface heat-flow. ?? 1968.

  7. Latitudinal distribution of carbon monoxide in the deep atmosphere of Venus

    Science.gov (United States)

    Collard, A. D.; Taylor, F. W.; Calcutt, S. B.; Carlson, R. W.; Kamp, L. W.; Baines, K. H.; Encrenaz, TH.; Drossart, P.; Lellouch, E.; Bezard, B.

    1993-01-01

    A large number of i.r. spectra of Venus was obtained using the Near-Infrared Mapping Spectrometer (NIMS) on the Galileo spacecraft, during the February 1990 encounter. Preliminary results show an apparent increase in the tropospheric CO volume mixing ratio (vmr) in the northern polar region. Other possible explanations of the observations are examined and rejected and an increase of the CO abundance north of 47 deg N of (35 +/- 15)% is inferred. Some possible causes of this enhancement are suggested.

  8. Harry Potter and the Upcoming Venus-Jupiter Conjunction: A Unique Outreach Opportunity

    Science.gov (United States)

    Larsen, K.

    2008-09-01

    As we prepare for the International Year of Astronomy 2009 (IYA2009), we should be on the lookout for celestial events which we can use not only to popularise the IYA2009 and practise our outreach skills, but which also have natural connections to popular culture. The Venus-Jupiter conjunction this autumn is such an opportunity, given several direct connections to the use of astronomy in J. K. Rowling's famous Harry Potter universe.

  9. Triggering a false alarm: Wounding mimics prey capture in the carnivorous venus flytrap (dionaea muscipula)

    Czech Academy of Sciences Publication Activity Database

    Pavlovič, A.; Jakšová, Jana; Novák, Ondřej

    2017-01-01

    Roč. 216, č. 3 (2017), s. 927-938 ISSN 0028-646X R&D Projects: GA MŠk(CZ) LO1204 Institutional support: RVO:61389030 Keywords : Action potential * Carnivorous plant * Defence * Digestive enzyme * Electrical signal * Jasmonic acid (JA) * Systemic response * Venus flytrap Subject RIV: EB - Genetics ; Molecular Biology OBOR OECD: Plant sciences, botany Impact factor: 7.330, year: 2016

  10. Formation, stratification, and mixing of the cores of Earth and Venus

    OpenAIRE

    Jacobson, Seth A.; Rubie, David C.; Hernlund, John; Morbidelli, Alessandro; Nakajima, Miki

    2017-01-01

    Earth possesses a persistent, internally-generated magnetic field, whereas no trace of a dynamo has been detected on Venus, at present or in the past, although a high surface temperature and recent resurfacing events may have removed paleomagnetic evidence. Whether or not a terrestrial body can sustain an internally generated magnetic field by convection inside its metallic fluid core is determined in part by its initial thermodynamic state and its compositional structure, both of which are i...

  11. Social Media Planning for the June 5, 2012 transit of Venus

    Science.gov (United States)

    Young, C.; Wawro, M.; Cline, T. D.; Schenk, L. C.; Durscher, R.

    2012-12-01

    On June 5, 2012 at sunset on the East Coast of North America and earlier for other parts of the U.S., the planet Venus made its final trek across the face of the sun as seen from Earth until the year 2117! The NASA Goddard Sun-Earth Day and Solar Dynamics Observatory EPO teams developed a social media strategy to support NASAs Transit of Venus event and webcast from Mauna Kea, Hawaii, on June 5, 2012. Our goal was to connect our contacts with a growing and vibrant social media community during all phases of this celestial event! We also wanted to help spread the word about the Transit of Venus by sharing content, facts, videos, images and links about the transit with our networks. Although social media events occurred throughout the world, our strategy was to provide an additional focus on NASA related events in key locations including those events happening in Hawaii, Alaska, and NASA Ames thereby amplifying our outreach efforts while ensuring that a strong connection existed across geographical and cultural borders. We also wanted to provide the public with information that would help them understand the importance of staying connected via social media even if viewing the transit was possible from their own locations. The social media strategy and the transit of Venus events were a great success and well as a learning experience for future social media events. We present the results of our plan as well as ways to improve and expand for future events. In addition, we present our social media template developed for the transit and now used by other heliophysics EPO teams.

  12. Plasma waves observed at low altitudes in the tenuous Venus nightside ionosphere

    Science.gov (United States)

    Strangeway, R. J.; Russell, C. T.; Ho, C. M.; Brace, L. H.

    1993-12-01

    The Pioneer Venus (PV) Orbiter Electric Field Detector (OEFD) measured many plasma wave bursts throughout the low altitude ionosphere during the final entry phase of the spacecraft. Apart from 100 Hz bursts observed at very low altitudes (approx. 130 km), the bursts fall into two classes. The first of these is a wideband signal that is observed in regions of low magnetic field, but average densities, in comparison to the prevailing ionospheric condition. This wideband signal is not observed in the 30 kHz channel of the OEFD, but is restricted to the 5.4 kHz channel and lower. Since these bursts are observed with roughly constant burst rate above 160 km altitude, we attribute them to ion acoustic mode waves generated by precipitating solar wind electrons. The second type of signal is restricted to 100 Hz only, and is observed in the regions of low electron beta, consistent with whistler-mode waves. These waves could be generated by lightning in the Venus atmosphere if the vertical component of the magnetic field greater than 3.6 nT. Because the ionosphere is very different during the entry phase, compared to the ionosphere as observed early in the Pioneer Venus mission, any conclusions regarding the source of the plasma waves detected during entry phase cannot be applied directly to the earlier observations.

  13. Ground-based observations of Mars and Venus water vapor during 1972 and 1973

    International Nuclear Information System (INIS)

    Barker, E.S.

    1974-01-01

    The Venus water vapor line at 8197.71 A has been monitored at several positions on the disk of Venus and at phase angles between 22 0 and 91 0 . Variations in the abundance have been found with both position and time. The total two-way transmission has varied from less than 5 to 77 μ of water vapor. Comparisons are made between water vapor abundance, presence of UV features and the CO 2 abundance determined from near simultaneous observations of CO 2 bands at the same position on the disk of Venus. The amount of Martian atmospheric water vapor has been monitored during the past two years at McDonald Observatory using the echelle coude scanner of the 272cm reflector. Two periods of the Martain year have been monitored. The first period was during and after the great 1971 dust storm (Lsub(s)=290 0 to 20 0 or summer in the southern hemisphere). The results obtained are compared to the Mariner 9 IRIS and Mars 3 observations made during the same period. During the second period (Lsub(s)=124 0 to 266 0 ) observations were made to follow the seasonal latitudinal and diurnal changes in the water abundance in the Martian atmosphere. Studies of the latitudinal and diurnal vapor distributions indicate the location of maximum and minimum abundances for this season are positively correlated with surface temperature variations. (Auth.)

  14. An electrodynamic model of the solar wind interaction with the ionospheres of Mars and Venus

    International Nuclear Information System (INIS)

    Cloutier, P.A.; Daniell, R.E. Jr.

    1979-01-01

    the electrodynamic model for the solar wind interaction with non-magnetic planets (Cloutier and Daniell, Planet. Space Sci. 21, 463, 1973; Daniell and Cloutier, Planet. Space Sci. 25, 621, 1977) is modified to include the effects of non-ohmic currents in the upper ionosphere. The model is then used to calculate convection patterns induced by the solar wind in the ionospheres of Mars and Venus. For Mars the observations of the neutral mass spectrometer or Vikings 1 and 2 provided the neutral atmosphere. Model calculations reproduced the retarding potential analyzer data and indicate that the ionosphere above about 200 km is probably controlled by convection rather than chemistry or diffusion. For Venus a model atmosphere based on Dickenson and Ridley, J. Atmos. Sci. 32, 1219 (1975) and Mayr et al., J. Geophys. Res. 83, 4411 (1978) was used. The resulting model calculations were compared to radio occultation data from Mariners 5 and 10 and Venera 9 which represent extremes in the variability of the upper Cytherean ionosphere. The model calculations are shown to fall within this variation. These results represent the state of the theory immediately prior to the Pioneer-Venus encounter. (author)

  15. Advanced Stirling Duplex Materials Assessment for Potential Venus Mission Heater Head Application

    Science.gov (United States)

    Ritzert, Frank; Nathal, Michael V.; Salem, Jonathan; Jacobson, Nathan; Nesbitt, James

    2011-01-01

    This report will address materials selection for components in a proposed Venus lander system. The lander would use active refrigeration to allow Space Science instrumentation to survive the extreme environment that exists on the surface of Venus. The refrigeration system would be powered by a Stirling engine-based system and is termed the Advanced Stirling Duplex (ASD) concept. Stirling engine power conversion in its simplest definition converts heat from radioactive decay into electricity. Detailed design decisions will require iterations between component geometries, materials selection, system output, and tolerable risk. This study reviews potential component requirements against known materials performance. A lower risk, evolutionary advance in heater head materials could be offered by nickel-base superalloy single crystals, with expected capability of approximately 1100C. However, the high temperature requirements of the Venus mission may force the selection of ceramics or refractory metals, which are more developmental in nature and may not have a well-developed database or a mature supporting technology base such as fabrication and joining methods.

  16. Lavoisier: A Low Altitude Balloon Network for Probing the Deep Atmosphere and Surface of Venus

    Science.gov (United States)

    Chaasefiere, E.; Berthelier, J. J.; Bertaux, J.-L.; Quemerais, E.; Pommereau, J.-P.; Rannou, P.; Raulin, F.; Coll, P.; Coscia, D.; Jambon, A.; hide

    2005-01-01

    The in-situ exploration of the low atmosphere and surface of Venus is clearly the next step of Venus exploration. Understanding the geochemistry of the low atmosphere, interacting with rocks, and the way the integrated Venus system evolved, under the combined effects of inner planet cooling and intense atmospheric greenhouse, is a major challenge of modern planetology. Due to the dense atmosphere (95 bars at the surface), balloon platforms offer an interesting means to transport and land in-situ measurement instruments. Due to the large Archimede force, a 2 cubic meter He-pressurized balloon floating at 10 km altitude may carry up to 60 kg of payload. LAVOISIER is a project submitted to ESA in 2000, in the follow up and spirit of the balloon deployed at cloud level by the Russian Vega mission in 1986. It is composed of a descent probe, for detailed noble gas and atmosphere composition analysis, and of a network of 3 balloons for geochemical and geophysical investigations at local, regional and global scales.

  17. Formation, stratification, and mixing of the cores of Earth and Venus

    Science.gov (United States)

    Jacobson, Seth A.; Rubie, David C.; Hernlund, John; Morbidelli, Alessandro; Nakajima, Miki

    2017-09-01

    Earth possesses a persistent, internally-generated magnetic field, whereas no trace of a dynamo has been detected on Venus, at present or in the past, although a high surface temperature and recent resurfacing events may have removed paleomagnetic evidence. Whether or not a terrestrial body can sustain an internally generated magnetic field by convection inside its metallic fluid core is determined in part by its initial thermodynamic state and its compositional structure, both of which are in turn set by the processes of accretion and differentiation. Here we show that the cores of Earth- and Venus-like planets should grow with stable compositional stratification unless disturbed by late energetic impacts. They do so because higher abundances of light elements are incorporated into the liquid metal that sinks to form the core as the temperatures and pressures of metal-silicate equilibration increase during accretion. We model this process and determine that this establishes a stable stratification that resists convection and inhibits the onset of a geodynamo. However, if a late energetic impact occurs, it could mechanically stir the core creating a single homogenous region within which a long-lasting geodynamo would operate. While Earth's accretion has been punctuated by a late giant impact with likely enough energy to mix the core (e.g. the impact that formed the Moon), we hypothesize that the accretion of Venus is characterized by the absence of such energetic giant impacts and the preservation of its primordial stratifications.

  18. Venus High Temperature Atmospheric Dropsonde and Extreme-Environment Seismometer (HADES)

    Science.gov (United States)

    Boll, Nathan J.; Salazar, Denise; Stelter, Christopher J.; Landis, Geoffrey A.; Colozza, Anthony J.

    2014-01-01

    The atmospheric composition and geologic structure of Venus have been identified by the US National Research Council's Decadal Survey for Planetary Science as priority targets for scientific exploration, however the high temperature and pressure at the surface, along with the highly corrosive chemistry of the Venus atmosphere, present significant obstacles to spacecraft design that have severely limited past and proposed landed missions. Following the methodology of the NASA Innovative Advanced Concepts (NIAC) proposal regime and the Collaborative Modeling and Parametric Assessment of Space Systems (COMPASS) design protocol, this paper presents a conceptual study and initial feasibility analysis for a Discovery-class Venus lander capable of an extended-duration mission at ambient temperature and pressure, incorporating emerging technologies within the field of high temperature electronics in combination with novel configurations of proven, high Technology Readiness Level (TRL) systems. Radioisotope Thermal Power (RTG) systems and silicon carbide (SiC) communications and data handling are examined in detail, and various high-temperature instruments are proposed, including a seismometer and an advanced photodiode imager. The study combines this technological analysis with proposals for a descent instrument package and a relay orbiter to demonstrate the viability of an integrated atmospheric and in-situ geologic exploratory mission that differs from previous proposals by greatly reducing the mass, power requirements, and cost, while achieving important scientific goals.

  19. Venus, Mars, and the ices on Mercury and the moon: astrobiological implications and proposed mission designs.

    Science.gov (United States)

    Schulze-Makuch, Dirk; Dohm, James M; Fairén, Alberto G; Baker, Victor R; Fink, Wolfgang; Strom, Robert G

    2005-12-01

    Venus and Mars likely had liquid water bodies on their surface early in the Solar System history. The surfaces of Venus and Mars are presently not a suitable habitat for life, but reservoirs of liquid water remain in the atmosphere of Venus and the subsurface of Mars, and with it also the possibility of microbial life. Microbial organisms may have adapted to live in these ecological niches by the evolutionary force of directional selection. Missions to our neighboring planets should therefore be planned to explore these potentially life-containing refuges and return samples for analysis. Sample return missions should also include ice samples from Mercury and the Moon, which may contain information about the biogenic material that catalyzed the early evolution of life on Earth (or elsewhere). To obtain such information, science-driven exploration is necessary through varying degrees of mission operation autonomy. A hierarchical mission design is envisioned that includes spaceborne (orbital), atmosphere (airborne), surface (mobile such as rover and stationary such as lander or sensor), and subsurface (e.g., ground-penetrating radar, drilling, etc.) agents working in concert to allow for sufficient mission safety and redundancy, to perform extensive and challenging reconnaissance, and to lead to a thorough search for evidence of life and habitability.

  20. Existence of collisional trajectories of Mercury, Mars and Venus with the Earth.

    Science.gov (United States)

    Laskar, J; Gastineau, M

    2009-06-11

    It has been established that, owing to the proximity of a resonance with Jupiter, Mercury's eccentricity can be pumped to values large enough to allow collision with Venus within 5 Gyr (refs 1-3). This conclusion, however, was established either with averaged equations that are not appropriate near the collisions or with non-relativistic models in which the resonance effect is greatly enhanced by a decrease of the perihelion velocity of Mercury. In these previous studies, the Earth's orbit was essentially unaffected. Here we report numerical simulations of the evolution of the Solar System over 5 Gyr, including contributions from the Moon and general relativity. In a set of 2,501 orbits with initial conditions that are in agreement with our present knowledge of the parameters of the Solar System, we found, as in previous studies, that one per cent of the solutions lead to a large increase in Mercury's eccentricity-an increase large enough to allow collisions with Venus or the Sun. More surprisingly, in one of these high-eccentricity solutions, a subsequent decrease in Mercury's eccentricity induces a transfer of angular momentum from the giant planets that destabilizes all the terrestrial planets approximately 3.34 Gyr from now, with possible collisions of Mercury, Mars or Venus with the Earth.

  1. 42 CFR 405.1840 - Board jurisdiction.

    Science.gov (United States)

    2010-10-01

    ... 42 Public Health 2 2010-10-01 2010-10-01 false Board jurisdiction. 405.1840 Section 405.1840... Appeals § 405.1840 Board jurisdiction. (a) General rules. (1) After a request for a Board hearing is filed...) of this section, whether or not it has jurisdiction to grant a hearing on each of the specific...

  2. 75 FR 8699 - Good Neighbor Environmental Board

    Science.gov (United States)

    2010-02-25

    ... ENVIRONMENTAL PROTECTION AGENCY [FRL-9117-9] Good Neighbor Environmental Board AGENCY: Environmental Protection Agency (EPA). ACTION: Notice of meeting. SUMMARY: Under the Federal Advisory Committee Act, Public Law 92-463, EPA gives notice of a meeting of the Good Neighbor Environmental Board (Board...

  3. 7 CFR 1205.308 - Cotton Board.

    Science.gov (United States)

    2010-01-01

    ... 7 Agriculture 10 2010-01-01 2010-01-01 false Cotton Board. 1205.308 Section 1205.308 Agriculture... AND ORDERS; MISCELLANEOUS COMMODITIES), DEPARTMENT OF AGRICULTURE COTTON RESEARCH AND PROMOTION Cotton Research and Promotion Order Definitions § 1205.308 Cotton Board. Cotton Board means the administrative...

  4. 7 CFR 1216.4 - Board.

    Science.gov (United States)

    2010-01-01

    ... ORDERS; MISCELLANEOUS COMMODITIES), DEPARTMENT OF AGRICULTURE PEANUT PROMOTION, RESEARCH, AND INFORMATION ORDER Peanut Promotion, Research, and Information Order Definitions § 1216.4 Board. Board means the administrative body referred to as the National Peanut Board established pursuant to § 1216.40. ...

  5. 7 CFR 1206.2 - Board.

    Science.gov (United States)

    2010-01-01

    ... ORDERS; MISCELLANEOUS COMMODITIES), DEPARTMENT OF AGRICULTURE MANGO PROMOTION, RESEARCH, AND INFORMATION Mango Promotion, Research, and Information Order Definitions § 1206.2 Board. Board or National Mango Promotion Board means the administrative body established pursuant to § 1206.30, or such other name as...

  6. 49 CFR 1151.4 - Board determination.

    Science.gov (United States)

    2010-10-01

    ... 49 Transportation 8 2010-10-01 2010-10-01 false Board determination. 1151.4 Section 1151.4 Transportation Other Regulations Relating to Transportation (Continued) SURFACE TRANSPORTATION BOARD, DEPARTMENT OF TRANSPORTATION RULES OF PRACTICE FEEDER RAILROAD DEVELOPMENT PROGRAM § 1151.4 Board determination...

  7. 77 FR 15091 - Environmental Management Advisory Board

    Science.gov (United States)

    2012-03-14

    ... Environmental Management Advisory Board AGENCY: Department of Energy. ACTION: Notice of Solicitation of Nominations for Appointment as a member of the Environmental Management Advisory Board. SUMMARY: In accordance... soliciting nominations for candidates to fill vacancies on the Environmental Management Advisory Board (EMAB...

  8. 76 FR 21877 - Environmental Management Advisory Board

    Science.gov (United States)

    2011-04-19

    ... Environmental Management Advisory Board AGENCY: Department of Energy. ACTION: Notice of call for nominations for appointment to the Environmental Management Advisory Board. SUMMARY: This notice constitutes an open call to the public to submit nominations for membership on the Environmental Management Advisory Board. DATES...

  9. 76 FR 8848 - Disciplinary Appeals Board Panel

    Science.gov (United States)

    2011-02-15

    ... AFFAIRS Disciplinary Appeals Board Panel AGENCY: Department of Veterans Affairs. ACTION: Notice with... constitute the Disciplinary Appeals Board Panel from which Board members in a case are appointed. This notice announces that the roster of employees on the Panel is available for review and comment. Employees, employee...

  10. 77 FR 71873 - Disciplinary Appeals Board Panel

    Science.gov (United States)

    2012-12-04

    ... AFFAIRS Disciplinary Appeals Board Panel AGENCY: Department of Veterans Affairs. ACTION: Notice with... constitute the Disciplinary Appeals Board Panel from which Board members in a case are appointed. This notice announces that the roster of employees on the Panel is available for review and comment. Employees, employee...

  11. 76 FR 77327 - Disciplinary Appeals Board Panel

    Science.gov (United States)

    2011-12-12

    ... AFFAIRS Disciplinary Appeals Board Panel AGENCY: Department of Veterans Affairs. ACTION: Notice with... constitute the Disciplinary Appeals Board Panel from which Board members in a case are appointed. This notice announces that the roster of employees on the Panel is available for review and comment. Employees, employee...

  12. Boys' boarding school management: understanding the choice ...

    African Journals Online (AJOL)

    marketing principles to compete effectively with boarding schools throughout the country and beyond. Customers .... the school, such as food in the boarding establishment) and the process of delivering the service (Palmer .... factors other than the academic performance of the school alone may play a role, as the boarding ...

  13. Mutations in the pqe-1 Gene Enhance Transgene Expression in Caenorhabditis elegans

    Science.gov (United States)

    Yamada, Koji; Tsuchiya, Jun-ichi; Iino, Yuichi

    2012-01-01

    Although various genetic tools have been developed and used as transgenes, the expression of the transgenes often is hampered by negative regulators. Disrupting such negative regulators of gene expression is potentially a way to overcome the common problem of low expression of transgenes. To find such regulators whose mutations enhance transgene expression in Caenorhabditis elegans, we took advantage of a newly developed reporter transgene, lin-11pAΔ::venus. This transgene induces expression of a fluorescent protein, Venus, in specific neurons including AIZ, where the expression was stochastic. The frequency of reporter expression in AIZ seemed to be correlated with the strength of transgene expression. By using this system, in which a moderate increase of expression was converted to all-or-none expression states, we describe here a forward genetic screen for mutations that enhance the expression of transgenes. Through the screen, we found that mutations in the pqe-1 gene, which encodes a Q/P-rich nuclear protein with an exonuclease domain, increase the chance of reporter expression in AIZ. The fluorescence intensity in RIC, in which all lin-11pAΔ::venus animals show reporter expression, was increased in pqe-1 mutants, suggesting that pqe-1 reduces the expression level of the transgene. Expression of transgenes with other promoters, 3′UTR, or reporter genes was also enhanced by the pqe-1 mutation, suggesting that the effect was not specific to a particular type of transgenes, whereas the effect did not seem to extend to endogenous genes. We propose that pqe-1 mutants can be used to increase the expression of various useful transgenes. PMID:22870397

  14. 14 CFR 250.9 - Written explanation of denied boarding compensation and boarding priorities.

    Science.gov (United States)

    2010-01-01

    ... 14 Aeronautics and Space 4 2010-01-01 2010-01-01 false Written explanation of denied boarding compensation and boarding priorities. 250.9 Section 250.9 Aeronautics and Space OFFICE OF THE SECRETARY... explanation of denied boarding compensation and boarding priorities. (a) Every carrier shall furnish...

  15. 14 CFR 250.5 - Amount of denied boarding compensation for passengers denied boarding involuntarily.

    Science.gov (United States)

    2010-01-01

    ... 14 Aeronautics and Space 4 2010-01-01 2010-01-01 false Amount of denied boarding compensation for passengers denied boarding involuntarily. 250.5 Section 250.5 Aeronautics and Space OFFICE OF THE SECRETARY... boarding compensation for passengers denied boarding involuntarily. (a) Subject to the exceptions provided...

  16. The Perceptions of Georgia School Board Members' Need for Training on School Board Governance

    Science.gov (United States)

    Nutt, Pamela Studdard

    2010-01-01

    This study explored the perceptions of training needs of school board members in Georgia. The study examined perceptions of school board chairs, board members with 1 to 5 years experience, members with 6 to 10 years experience, members with 11 to 15 years experience and board members with 16 plus years experience in the areas of school board…

  17. 77 FR 5020 - Civilian Board of Contract Appeals; Information Collection; Civilian Board of Contract Appeals...

    Science.gov (United States)

    2012-02-01

    ...] Civilian Board of Contract Appeals; Information Collection; Civilian Board of Contract Appeals Rules of... regarding the Civilian Board of Contract Appeals (CBCA) Rules of Procedure. Public comments are particularly... Information Collection IC 3090-0221, Civilian Board of Contract Appeals Rules of Procedure, by any of the...

  18. The Atomic Energy Control Board

    International Nuclear Information System (INIS)

    Doern, G.B.

    1976-01-01

    This study describes and assesses the regulatory and administrative processes and procedures of the Atomic Energy Control Board, the AECB. The Atomic Energy Control Act authorized the AECB to control atomic energy materials and equipment in the national interest and to participate in measures for the international control of atomic energy. The AECB is authorized to make regulations to control atomic energy materials and equipment and to make grants in support of atomic energy research. (author)

  19. The Role of Board of Directors in the Establishment of Risk Management Committee

    Directory of Open Access Journals (Sweden)

    Ishak Suhaimi

    2017-01-01

    Full Text Available The objective of the study is to discuss the roles of board of directors in the establishment of risk management committee for Malaysian’s public listed companies. In Malaysia, based on the Malaysian Code on Corporate Governance (MCCG, (2007; 2012 clearly stated the role and responsibility of the board of directors toward the risk management activities. At the Corporate Governance Week 2010 and 2011 as well, the chairman of the Security Commission Malaysia highlighted the responsibility of the board of directors in risk management processes and she expressed concern over the failure of the board of directors to establish appropriate measures for the risk management process in the company. The statement of the chairman of Security Commission Malaysia is in line with MCCG’s best practices (2000; 2007; 2012, i.e., the board of directors should identify principle risks and ensure the implementation of an appropriate system to manage these risks.

  20. Graedel named to AIP Board

    Science.gov (United States)

    Maggs, William Ward

    Thomas E. Graedel, an atmospheric scientist at AT&T Bell Laboratories (Murray Hill, N.J.), has been made an AGU representative to the Governing Board of the American Institute of Physics (AIP). The board oversees the operations of AIP, a nonprofit umbrella organization for 10 member societies, including AGU. Other AGU members currently on the governing board include Orson Anderson, a geophysicist at the University of California, Los Angeles; AGU General Secretary Peter M. Bell of the Norton Company, Worcester, Mass.; AGU Executive Director A. F. Spilhaus, Jr.; and Martin Walt, a geophysicist with the Lockheed Corporation in Palo Alto, Calif.All AGU members receive the benefits of membership in AIP, including the monthly magazine Physics Today. Other AIP services available to AGU members include access to an employment service, AIP's electronic network Pi-NET, and an insurance program. AGU members can also subscribe to journals published by the American Physical Society, another AIP member society, at discounted rates.—WWM

  1. Integrated reporting and board features

    Directory of Open Access Journals (Sweden)

    Rares HURGHIS

    2017-02-01

    Full Text Available In the last two decades the concept of sustainability reporting gained more importance in the companies’ annual reports, a trend which is embedded also in integrated reporting. Issuing an integrated report became a necessity, because the report explains to the investors how the organization creates value over time. The governance structure, more exactly the board of directors, decides whether or not the company will issue an integrated report. Thus, are there certain features of the board that might influence the issue of an integrated report? Do the companies which issue an integrated report have certain features of the governance structure? Looking for an answer to these questions, we seek for any possible correlations between a disclosure index and the corporate governance structure characteristics, on a sample from the companies participating at the International Integrated Reporting Council Examples Database. The results highlight that only the size of the board influences the extent to which the issued integrated report is in accordance with the International Framework.

  2. Board Saver for Use with Developmental FPGAs

    Science.gov (United States)

    Berkun, Andrew

    2009-01-01

    A device denoted a board saver has been developed as a means of reducing wear and tear of a printed-circuit board onto which an antifuse field programmable gate array (FPGA) is to be eventually soldered permanently after a number of design iterations. The need for the board saver or a similar device arises because (1) antifuse-FPGA design iterations are common and (2) repeated soldering and unsoldering of FPGAs on the printed-circuit board to accommodate design iterations can wear out the printed-circuit board. The board saver is basically a solderable/unsolderable FPGA receptacle that is installed temporarily on the printed-circuit board. The board saver is, more specifically, a smaller, square-ring-shaped, printed-circuit board (see figure) that contains half via holes one for each contact pad along its periphery. As initially fabricated, the board saver is a wider ring containing full via holes, but then it is milled along its outer edges, cutting the via holes in half and laterally exposing their interiors. The board saver is positioned in registration with the designated FPGA footprint and each via hole is soldered to the outer portion of the corresponding FPGA contact pad on the first-mentioned printed-circuit board. The via-hole/contact joints can be inspected visually and can be easily unsoldered later. The square hole in the middle of the board saver is sized to accommodate the FPGA, and the thickness of the board saver is the same as that of the FPGA. Hence, when a non-final FPGA is placed in the square hole, the combination of the non-final FPGA and the board saver occupy no more area and thickness than would a final FPGA soldered directly into its designated position on the first-mentioned circuit board. The contact leads of a non-final FPGA are not bent and are soldered, at the top of the board saver, to the corresponding via holes. A non-final FPGA can readily be unsoldered from the board saver and replaced by another one. Once the final FPGA design

  3. From Global Firms to Global Boards?

    DEFF Research Database (Denmark)

    Thomsen, Steen; Gregoric, Aleksandra; Randøy, Trond

    2011-01-01

    This paper examines the internationalization of Nordic company boards during 2001-2008. Using Poisson pooled and panel estimators we find that financial rather than commercial internationalization drives the recruitment of international board members. Foreign listing and foreign ownership...... are significant whereas international sales and operations are not. When we extend “board internationalization” to encompass national directors with international experience we find that shareholders may opt for domestic board members with that experience to match the firm’s commercial internationalization....... This indicates some support for the view that different kinds of firm internationalization – commercial versus financial - might lead to different types of board internationalization. We find no evidence that the internationalization of boards is limited by the conservatism of existing national board members...

  4. VENUS: cold prototype installation of the head-end of the reprocessing of HTR fuel elements. Activity report, 1 July 1976--31 December 1976

    International Nuclear Information System (INIS)

    Boehnert, R.; Walter, C.

    The purpose of the VENUS Project is advance planning for the construction of a cold prototype system to incinerate HTR fuel element graphite. The Venus Project is organized into four phases between advance planning and experimental operation, corresponding to the maturity of the work. It is in the advance planning phase. Status of individual studies is given

  5. Preserving the Legitimacy of Board Certification.

    Science.gov (United States)

    Hanemann, Michael S; Wall, Holly C; Dean, John A

    2017-06-01

    The aims of this discussion were to inform the medical community about the American Board of Cosmetic Surgery's ongoing attempts in Louisiana to achieve equivalency to American Board of Medical Specialties (ABMS) member boards so that its diplomates may use the term "board certified" in advertising and to ensure public safety by upholding the standards for medical board certification. In 2011, Louisiana passed a truth in medical advertising law, which was intended to protect the public by prohibiting the use of the term "board certified" by improperly credentialed physicians. An American Board of Cosmetic Surgery diplomate petitioned the Louisiana State Board of Medical Examiners to approve a rule that would establish a pathway to equivalency for non-ABMS member boards, whose diplomates have not completed training approved by the Accreditation Council for Graduate Medical Education (ACGME) in the specialty they are certifying. Physicians and physician organizations representing multiple specialties (facial plastic and reconstructive surgery, otolaryngology [head and neck surgery], orthopedic spine surgery, pediatric neurosurgery, dermatology, and plastic surgery) urged the Louisiana State Board of Medical Examiners to clarify its advertising policy, limiting the use of the term "board certified" to physicians who have completed ACGME-approved training in the specialty or subspecialty named in the certificate. The public equates the term "board certified" with the highest level of expertise in a medical specialty. When a certifying board does not require completion of ACGME or American Osteopathic Association (AOA)-accredited training in the specialty it certifies, the result is an unacceptable degree of variability in the education and training standards applied to its diplomates. Independent, third-party oversight of certifying boards and training programs is necessary to ensure quality standards are upheld. Any system that assesses a non-ABMS member or non

  6. Across the board: Licheng Sun.

    Science.gov (United States)

    Sun, Licheng

    2015-01-01

    In this series of articles the board members of ChemSusChem discuss recent research articles that they consider of exceptional quality and importance for sustainability. In this entry, Prof. Licheng Sun discusses how solar fuel production (such as water splitting) can be made more efficient and economic on an industrial scale. Recommended is the work by Prof. Xuping Sun, who use non-noble metal-phosphorus-based nanostructures as efficient electrocatalysts for hydrogen generation from water. © 2015 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

  7. The fourth Board of Governors

    International Nuclear Information System (INIS)

    1961-01-01

    The General Conference of the International Atomic Energy Agency at its fourth regular session, which was held in Vienna from 20 September to 1 October 1960, elected five Member States to serve a two-year term on the Agency's Board of Governors. The five were Argentina, El Salvador, the Federal Republic of Germany, Iraq and Thailand. The new members succeed Indonesia, the Netherlands, Peru, the United Arab Republic and Venezuela, which were elected for a two-year term by the second session of the General Conference in 1958

  8. Vesper - Venus Chemistry and Dynamics Orbiter - A NASA Discovery Mission Proposal: Submillimeter Investigation of Atmospheric Chemistry and Dynamics

    Science.gov (United States)

    Chin, Gordon

    2011-01-01

    Vesper conducts a focused investigation of the chemistry and dynamics of the middle atmosphere of our sister planet- from the base of the global cloud cover to the lower thermosphere. The middle atmosphere controls the stability of the Venus climate system. Vesper determines what processes maintain the atmospheric chemical stability, cause observed variability of chemical composition, control the escape of water, and drive the extreme super-rotation. The Vesper science investigation provides a unique perspective on the Earth environment due to the similarities in the middle atmosphere processes of both Venus and the Earth. Understanding key distinctions and similarities between Venus and Earth will increase our knowledge of how terrestrial planets evolve along different paths from nearly identical initial conditions.

  9. Earliest depiction of vitiligo in "Venus at a Mirror" (1615) by Peter Paul Rubens (1577-1640).

    Science.gov (United States)

    Ashrafian, Hutan

    2017-09-27

    The 1615 painting of Venus at a Mirror by Peter Paul Rubens is considered a powerful example of the Flemish Baroque movement. Recently it has been identified that the Venus character in the image has a goitre, however on studying the image further, I note dermato-pathology in another of the painting's main characters; the dark-skinned female typically described as the Venus' maidservant who clearly demonstrates patches of skin pigment loss on her face and neck with a concurrent streak of white hair. Together these suggest the underlying diagnosis of vitiligo. There is also a goitre in this individual suggesting thyroid disease. This new finding may offer additional insight into the historical epidemiology of disease in northern Europe but also offers further understanding of the method, origin, and pathological associations of this prominent painting from a genius artist. © 2017 Wiley Periodicals, Inc.

  10. The Atmospheres of the Terrestrial Planets:Clues to the Origins and Early Evolution of Venus, Earth, and Mars

    Science.gov (United States)

    Baines, Kevin H.; Atreya, Sushil K.; Bullock, Mark A.; Grinspoon, David H,; Mahaffy, Paul; Russell, Christopher T.; Schubert, Gerald; Zahnle, Kevin

    2015-01-01

    We review the current state of knowledge of the origin and early evolution of the three largest terrestrial planets - Venus, Earth, and Mars - setting the stage for the chapters on comparative climatological processes to follow. We summarize current models of planetary formation, as revealed by studies of solid materials from Earth and meteorites from Mars. For Venus, we emphasize the known differences and similarities in planetary bulk properties and composition with Earth and Mars, focusing on key properties indicative of planetary formation and early evolution, particularly of the atmospheres of all three planets. We review the need for future in situ measurements for improving our understanding of the origin and evolution of the atmospheres of our planetary neighbors and Earth, and suggest the accuracies required of such new in situ data. Finally, we discuss the role new measurements of Mars and Venus have in understanding the state and evolution of planets found in the habitable zones of other stars.

  11. The Editorial Board is Changing

    Directory of Open Access Journals (Sweden)

    LE Nicolle

    2005-01-01

    Full Text Available The success of The Canadian Journal of Infectious Diseases & Medical Microbiology over the past 16 years is largely attributable to the continuing and substantial support from a dedicated and enthusiastic Editorial Board. The individuals who have participated are listed on the masthead in each issue of the Journal. Many of the current Editorial Board members have participated continually since the initiation of the Journal - a commitment of over 16 years. They have provided oversight as the Journal has evolved, and their critical insights in the discussion of issues as they have developed, as well as their suggestions for new directions, have significantly contributed to the maintenance of Journal quality. Our associate editors have been particularly active. They have coordinated and, frequently, developed much of the content for the special sections - adult and paediatric infectious disease notes, clinical vignettes and reviews. They have also facilitated the peer review of submitted manuscripts by identifying reviewers and making recommendations for revisions and publication. These contributions have been essential to the continuing operation and high, scientific quality of the Journal.

  12. Optimal back-to-front airplane boarding.

    Science.gov (United States)

    Bachmat, Eitan; Khachaturov, Vassilii; Kuperman, Ran

    2013-06-01

    The problem of finding an optimal back-to-front airplane boarding policy is explored, using a mathematical model that is related to the 1+1 polynuclear growth model with concave boundary conditions and to causal sets in gravity. We study all airplane configurations and boarding group sizes. Optimal boarding policies for various airplane configurations are presented. Detailed calculations are provided along with simulations that support the main conclusions of the theory. We show that the effectiveness of back-to-front policies undergoes a phase transition when passing from lightly congested airplanes to heavily congested airplanes. The phase transition also affects the nature of the optimal or near-optimal policies. Under what we consider to be realistic conditions, optimal back-to-front policies lead to a modest 8-12% improvement in boarding time over random (no policy) boarding, using two boarding groups. Having more than two groups is not effective.

  13. Modeling and isomorphisms of positional board games.

    Science.gov (United States)

    Antoy, S

    1987-05-01

    A model is proposed for a class of two-person games based on the occupation of positions on a board. Well-known games that can be rephrased within or with the help of the model are, for example, tic-tac-toe, qubic, go-moku, hex, and connect-four. The model is formulated in terms of a composite algebraic structure called board. A notion of board isomorphism is defined, a few concepts fundamental for positional board game playing are identified, and necessary and sufficient conditions for establishing the isomorphism of two boards are proved. The formalism of the model provides criteria for the description and analysis of a board that are more abstract than its physical characteristics such as size and dimensionality. The application of the isomorphism results to the implementation of more general and efficient software modules for game playing is discussed. Related work is briefly outlined and compared.

  14. Internationalilzation of the Firm and its Board

    DEFF Research Database (Denmark)

    Oxelheim, Lars; Gregoric, Aleksandra; Randøy, Trond

    In this paper we study the internationalization of corporate supervisory boards. We use Poisson random effects and negative binominal random effect estimators to analyze the determinants of foreign board membership in listed firms from four Nordic countries in 2001-2007. We find that financial...... competencies required by firm internationalization positively affect board internationalization, whereas the impact of the internationalization of a firm’s commercial operations is positive but not significant across all model specifications. We find that the higher the number of national board members...... with international experience, the higher is the number of foreign supervisory board members. A significantly positive impact is also found for foreign ownership; the greater foreign ownership of a firm, the higher is the number of foreigners we can expect on the firm’s supervisory board. For Norway and Sweden...

  15. Optimal back-to-front airplane boarding

    Science.gov (United States)

    Bachmat, Eitan; Khachaturov, Vassilii; Kuperman, Ran

    2013-06-01

    The problem of finding an optimal back-to-front airplane boarding policy is explored, using a mathematical model that is related to the 1+1 polynuclear growth model with concave boundary conditions and to causal sets in gravity. We study all airplane configurations and boarding group sizes. Optimal boarding policies for various airplane configurations are presented. Detailed calculations are provided along with simulations that support the main conclusions of the theory. We show that the effectiveness of back-to-front policies undergoes a phase transition when passing from lightly congested airplanes to heavily congested airplanes. The phase transition also affects the nature of the optimal or near-optimal policies. Under what we consider to be realistic conditions, optimal back-to-front policies lead to a modest 8-12% improvement in boarding time over random (no policy) boarding, using two boarding groups. Having more than two groups is not effective.

  16. Reentry response of the lightweight radioisotope heater unit resulting from a Cassini Venus-Venus-Earth-Jupiter gravity assist maneuver accident

    International Nuclear Information System (INIS)

    1996-12-01

    Reentry analyses consisting of ablation response, thermal response and thermal stress response have been conducted on the Lightweight Radioisotope Heater Unit (LWRHU) for Cassini/Venus-Venus-Earth-Jupiter-Gravity-Assist (VVEJGA) reentry conditions. Sequential ablation analyses of the LWRHU aeroshell, and the fuel pellet have been conducted in reentry regimes where the aeroshell has been deemed to fail. The failure criterion for ablation is generally assumed to be recession corresponding to 75% and 100% of the wall thickness. The 75% recession failure criteria allows for uncertainties that result mainly because of the high energies involved in the VVEJGA reentries compared to orbital decay reentries. Risk evaluations should consider the fact that for shallow flight paths the unit may disassemble at high-altitude as a result of ablation or may remain intact with a clad that had been molten. Within the limitations of the methodologies and assumptions of the analyses, the results indicate that: (1) For a side-on stable LWRHU reentry, aeroshell ablation failures occur for all reentry angles. (2)For a side-on spinning LWRHU reentry, aeroshell ablation failures are minimal. (3) For the tumbling LWRHU reentry, the aeroshell survives for most angles. (4) For the thermostructural analyses, using both a 1% and 5% allowable strain, all reentry angles and orientations examined resulted in small localized failures, but aeroshell breach is not predicted for any case. The analyses included in this report concentrate on VVEJGA reentry scenarios. Analyses reported previously have demonstrated that the LWRHU has adequate design margin to survive reentry from orbital decay scenarios and most injection scenarios at speeds up to escape speeds. The exception is a narrow range of flight path angles that produce multiple skip trajectories which may have excessive ablation

  17. Reentry response of the lightweight radioisotope heater unit resulting from a Cassini Venus-Venus-Earth-Jupiter gravity assist maneuver accident

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    1996-12-01

    Reentry analyses consisting of ablation response, thermal response and thermal stress response have been conducted on the Lightweight Radioisotope Heater Unit (LWRHU) for Cassini/Venus-Venus-Earth-Jupiter-Gravity-Assist (VVEJGA) reentry conditions. Sequential ablation analyses of the LWRHU aeroshell, and the fuel pellet have been conducted in reentry regimes where the aeroshell has been deemed to fail. The failure criterion for ablation is generally assumed to be recession corresponding to 75% and 100% of the wall thickness. The 75% recession failure criteria allows for uncertainties that result mainly because of the high energies involved in the VVEJGA reentries compared to orbital decay reentries. Risk evaluations should consider the fact that for shallow flight paths the unit may disassemble at high-altitude as a result of ablation or may remain intact with a clad that had been molten. Within the limitations of the methodologies and assumptions of the analyses, the results indicate that: (1) For a side-on stable LWRHU reentry, aeroshell ablation failures occur for all reentry angles. (2)For a side-on spinning LWRHU reentry, aeroshell ablation failures are minimal. (3) For the tumbling LWRHU reentry, the aeroshell survives for most angles. (4) For the thermostructural analyses, using both a 1% and 5% allowable strain, all reentry angles and orientations examined resulted in small localized failures, but aeroshell breach is not predicted for any case. The analyses included in this report concentrate on VVEJGA reentry scenarios. Analyses reported previously have demonstrated that the LWRHU has adequate design margin to survive reentry from orbital decay scenarios and most injection scenarios at speeds up to escape speeds. The exception is a narrow range of flight path angles that produce multiple skip trajectories which may have excessive ablation.

  18. Global scale concentrations of volcanic activity on Venus: A summary of three 23rd Lunar and Planetary Science Conference abstracts. 1: Venus volcanism: Global distribution and classification from Magellan data. 2: A major global-scale concentration of volcanic activity in the Beta-Atla-Themis region of Venus. 3: Two global concentrations of volcanism on Venus: Geologic associations and implications for global pattern of upwelling and downwelling

    Science.gov (United States)

    Crumpler, L. S.; Aubele, Jayne C.; Head, James W.; Guest, J.; Saunders, R. S.

    1992-01-01

    As part of the analysis of data from the Magellan Mission, we have compiled a global survey of the location, dimensions, and subsidiary notes of all identified volcanic features on Venus. More than 90 percent of the surface area was examined and the final catalog comprehensively identifies 1548 individual volcanic features larger than approximately 20 km in diameter. Volcanic features included are large volcanoes, intermediate volcanoes, fields of small shield volcanoes, calderas, large lava channels, and lava floods as well as unusual features first noted on Venus such as coronae, arachnoids, and novae.

  19. Progress Towards providing Heat-Shield for Extreme Entry Environment Technology (HEEET) for Venus and other New Froniters Missions

    Science.gov (United States)

    Venkatapathy, Ethiraj; Ellerby, Don; Gage, Peter

    2017-01-01

    Heat-shield for Extreme Entry Environment Technology (HEEET) has been in development since 2014 with the goal of enabling missions to Venus, Saturn and other high-speed sample return missions. It is offered as a new technology and incentivized for mission use in the New Frontiers 4 AO by NASA. The current plans are to mature the technology to TRL 6 by FY18. The HEEET Team has been working closely with multiple NF-4 proposals to Venus, Saturn and has been supporting recent Ice-Giants mission studies. This presentation will provide progress made to date and the plans for development in FY18.

  20. Comparative study on neutron data in integral experiments of MYRRHA mockup critical cores in the VENUS-F reactor

    Directory of Open Access Journals (Sweden)

    Krása Antonín

    2017-01-01

    Full Text Available VENUS-F is a fast, zero-power reactor with 30% wt. metallic uranium fuel and solid lead as coolant simulator. It serves as a mockup of the MYRRHA reactor core. This paper describes integral experiments performed in two critical VENUS-F core configurations (with and without graphite reflector. Discrepancies between experiments and Monte Carlo calculations (MCNP5 of keff, fission rate spatial distribution and reactivity effects (lead void and fuel Doppler depending on a nuclear data library used (JENDL-4.0, ENDF-B-VII.1, JEFF-3.1.2, 3.2, 3.3T2 are presented.

  1. Venus monópoda y Marte soñador. Confidencias y recelos ante un cuadro de Botticelli

    OpenAIRE

    Salabert, Pere

    2003-01-01

    A la Venus romana, asimilada desde el siglo II a. C. a la griega Afrodita, diosa del Amor y la Belleza, con rasgos derivados de su primitiva función de protectora de los huertos, se le atribuye el mes de abril con el despertar de la naturaleza. No necesitamos retroceder hasta la antigua Ishtar, ni aludir a la prostituta sagrada que copula con su esclavo antes de echarlo al fuego: tan lejos como vayamos a mirar, Venus es la clara expresión de la existencia humana, contradictoria, hecha de sati...

  2. Comparative study on neutron data in integral experiments of MYRRHA mockup critical cores in the VENUS-F reactor

    Science.gov (United States)

    Krása, Antonín; Kochetkov, Anatoly; Baeten, Peter; Vittiglio, Guido; Wagemans, Jan; Bécares, Vicente

    2017-09-01

    VENUS-F is a fast, zero-power reactor with 30% wt. metallic uranium fuel and solid lead as coolant simulator. It serves as a mockup of the MYRRHA reactor core. This paper describes integral experiments performed in two critical VENUS-F core configurations (with and without graphite reflector). Discrepancies between experiments and Monte Carlo calculations (MCNP5) of keff, fission rate spatial distribution and reactivity effects (lead void and fuel Doppler) depending on a nuclear data library used (JENDL-4.0, ENDF-B-VII.1, JEFF-3.1.2, 3.2, 3.3T2) are presented.

  3. Remote Raman Spectroscopy of Minerals at Elevated Temperature Relevant to Venus Exploration

    Science.gov (United States)

    Sharma, Shiv K.; Misra, Anupam K.; Singh, Upendra N.

    2008-01-01

    We have used a remote time-resolved telescopic Raman system equipped with 532 nm pulsed laser excitation and a gated intensified CCD (ICCD) detector for measuring Raman spectra of a number of minerals at high temperature to 970 K. Remote Raman measurements were made with samples at 9-meter in side a high-temperature furnace by gating the ICCD detector with 2 micro-sec gate to minimize interference from blackbody emission from mineral surfaces at high temperature as well as interference from ambient light. A comparison of Raman spectra of gypsum (CaSO4.2H2O), dolomite (CaMg(CO3)2), and olivine (Mg2Fe2-xSiO4), as a function of temperature shows that the Raman lines remains sharp and well defined even in the high-temperature spectra. In the case of gypsum, Raman spectral fingerprints of CaSO4.H2O at 518 K were observed due to dehydration of gypsum. In the case of dolomite, partial mineral dissociation was observed at 973 K at ambient pressure indicating that some of the dolomite might survive on Venus surface that is at approximately 750 K and 92 atmospheric pressure. Time-resolved Raman spectra of low clino-enstatite (MgSiO3) measured at 75 mm from the sample in side the high-temperature furnace also show that the Raman lines remains sharp and well defined in the high temperature spectra. These high-temperature remote Raman spectra of minerals show that time-resolved Raman spectroscopy can be used as a potential tool for exploring Venus surface mineralogy at shorter (75 mm) and long (9 m) distances from the samples both during daytime and nighttime. The remote Raman system could also be used for measuring profiles of molecular species in the dense Venus atmosphere during descent as well as on the surface.

  4. Limb darkening in Venus night-side disk as viewed from Akatsuki IR2

    Science.gov (United States)

    Satoh, Takehiko; Nakakushi, Takashi; Sato, Takao M.; Hashimoto, George L.

    2017-10-01

    Night-side hemisphere of Venus exhibits dark and bright regions as a result of spatially inhomogeneous cloud opacity which is illuminated by infrared radiation from deeper atmosphere. The 2-μm camera (IR2) onboard Akatsuki, Japan's Venus Climate Orbiter, is equipped with three narrow-band filters (1.735, 2.26, and 2.32 μm) to image Venus night-side disk in well-known transparency windows of CO2 atmosphere (Allen and Crawford 1984). In general, a cloud feature appears brightest when it is in the disk center and becomes darker as the zenith angle of emergent light increases. Such limb darkening was observed with Galileo/NIMS and mathematically approximated (Carlson et al., 1993). Limb-darkening correction helps to identify branches, in a 1.74-μm vs. 2.3-μm radiances scatter plot, each of which corresponds to a group of aerosols with similar properties. We analyzed Akatsuki/IR2 images to characterize the limb darkening for three night-side filters.There is, however, contamination from the intense day-side disk blurred by IR2's point spread function (PSF). It is found that infrared light can be multiplly reflected within the Si substrate of IR2 detector (1024x1024 pixels PtSi array), causing elongated tail in the actual PSF. We treated this in two different ways. One is to mathematically approximate the PSF (with a combination of modified Lorentz functions) and another is to differentiate 2.26-μm image from 2.32-μm image so that the blurred light pattern can directly be obtained. By comparing results from these two methods, we are able to reasonablly clean up the night-side images and limb darkening is extracted. Physical interpretation of limb darkening, as well as "true" time variations of cloud brightness will be presented/discussed.

  5. 25 CFR 81.8 - Election board.

    Science.gov (United States)

    2010-04-01

    ... 25 Indians 1 2010-04-01 2010-04-01 false Election board. 81.8 Section 81.8 Indians BUREAU OF... STATUTE § 81.8 Election board. (a) There shall be an election board consisting of the officer in charge... interpreter and as many clerks and poll watchers as he/she deems necessary, but they shall not be members of...

  6. New Rationales for Women on Boards

    OpenAIRE

    Choudhury, B.

    2014-01-01

    Should measures promoting women to corporate boards be solely justified in terms of economic arguments? Traditionally, such measures have tended to rely on utilitarian arguments, despite the fact that the most prominent of these arguments—the relationship between women’s presence on boards and firm financial performance—is equivocal. Conversely, this article argues that rationales for increasing women on boards should be based on both equality and economics grounds. An equality rationale is n...

  7. Simulation and beam line experiments for the superconducting ECRion source VENUS

    Energy Technology Data Exchange (ETDEWEB)

    Todd, Damon S.; Leitner, Daniela; Grote, David P.; Lyneis, ClaudeM.

    2007-09-10

    The particle-in-cell code Warp has been enhanced toincorporate both two- and three-dimensional sheath extraction modelsgiving Warp the capability of simulating entire ion beam transportsystems including the extraction of beams from plasma sources. In thisarticle we describe a method of producing initial ion distributions forplasma extraction simulations in electron cyclotron resonance (ECR) ionsources based on experimentally measured sputtering on the source biaseddisc. Using this initialization method, we present preliminary resultsfor extraction and transport simulations of an oxygen beam and comparethem with experimental beam imaging on a quartz viewing plate for thesuperconducting ECR ion source VENUS.

  8. Radiative forcing of the Venus mesosphere. II - Thermal fluxes, cooling rates, and radiative equilibrium temperatures

    Science.gov (United States)

    Crisp, David

    1989-01-01

    A radiative heat-transfer model is presently used to ascertain the way in which radiative forcing contributes to the up to 20 K higher temperature of the Venus polar regions, by comparison with the tropics, in the 60-100 km mesospheric levels. Model global-mean radiative equilibrium temperatures for 55-100 km are compared with observations to show how each opacity source contributes to the thermal structure. The results obtained from latitude-dependent radiative equilibrium experiments indicate that meridional variations in radiative forcing obliterate observed mesospheric temperature gradients and yield polar temperatures up to 40 K cooler than the tropics.

  9. Gravity anomalies, compensation mechanisms, and the geodynamics of western Ishtar Terra, Venus

    Science.gov (United States)

    Grimm, Robert E.; Phillips, Roger J.

    1991-01-01

    Pioneer Venus line-of-sight orbital accelerations were utilized to calculate the geoid and vertical gravity anomalies for western Ishtar Terra on various planes of altitude z sub 0. The apparent depth of isostatic compensation at z sub 0 = 1400 km is 180 + or - 20 km based on the usual method of minimum variance in the isostatic anomaly. An attempt is made here to explain this observation, as well as the regional elevation, peripheral mountain belts, and inferred age of western Ishtar Terra, in terms of one or three broad geodynamic models.

  10. Gamma-ray burst observations with the Compton/Ulysses/Pioneer-Venus network

    International Nuclear Information System (INIS)

    Cline, T.L.; Hurley, K.C.; Sommer, M.; Boer, M.; Niel, M.; Fishman, G.J.; Kouveliotou, C.; Meegan, C.A.; Paciesas, W.S.; Wilson, R.B.; Fenimore, E.E.; Laros, J.G.; Klebesadel, R.W.

    1993-01-01

    The third and latest interplanetary network for the precise directional analysis of gamma ray bursts consists of the Burst and Transient Source Experiment in Compton Gamma Ray Observatory and instruments on Pioneer-Venus Orbiter and the deep-space mission Ulysses. The unsurpassed resolution of the BATSE instrument, the use of refined analysis techniques, and Ulysses' distance of up to 6 AU all contribute to a potential for greater precision than had been achieved with former networks. Also, the departure of Ulysses from the ecliptic plane in 1992 avoids any positional alignment of the three instruments that would lessen the source directional accuracy

  11. Simulation and beam line experiments for the superconducting ECR ion source VENUS

    International Nuclear Information System (INIS)

    Todd, Damon S.; Leitner, Daniela; Grote, David P.; Lyneis, ClaudeM.

    2007-01-01

    The particle-in-cell code Warp has been enhanced to incorporate both two- and three-dimensional sheath extraction models giving Warp the capability of simulating entire ion beam transport systems including the extraction of beams from plasma sources. In this article we describe a method of producing initial ion distributions for plasma extraction simulations in electron cyclotron resonance (ECR) ion sources based on experimentally measured sputtering on the source biased disc. Using this initialization method, we present preliminary results for extraction and transport simulations of an oxygen beam and compare them with experimental beam imaging on a quartz viewing plate for the superconducting ECR ion source VENUS

  12. Shocklike soliton because of an impinge of protons and electrons solar particles with Venus ionosphere

    Science.gov (United States)

    Moslem, W. M.; Rezk, S.; Abdelsalam, U. M.; El-Labany, S. K.

    2018-04-01

    This paper introduces an investigation of shocklike soliton or small amplitude Double Layers (DLs) in a collisionless plasma, consisting of positive and negative ions, nonthermal electrons, as well as solar wind streaming protons and electrons. Gardner equation is derived and its shocklike soliton solution is obtained. The model is employed to recognize a possible nonlinear wave at Venus ionosphere. The results indicate that the number densities and velocities of the streaming particles play crucial role to determine the polarity and characteristic features (amplitude and width) of the shocklike soliton waves. An electron streaming speed modifies a negative shocklike wave profile, while an ion streaming speed modulates a positive shocklike wave characteristic.

  13. An astro-comb calibrated solar telescope to search for the radial velocity signature of Venus

    Science.gov (United States)

    Phillips, David F.; Glenday, Alex G.; Dumusque, Xavier; Buchschacher, Nicolas; Cameron, Andrew Collier; Cecconi, Massimo; Charbonneau, David; Cosentino, Rosario; Ghedina, Adriano; Haywood, Raphäelle; Latham, David W.; Li, Chih-Hao; Lodi, Marcello; Lovis, Christophe; Molinari, Emilio; Pepe, Francesco; Sasselov, Dimitar; Szentgyorgyi, Andrew; Udry, Stephane; Walsworth, Ronald L.

    2016-07-01

    We recently demonstrated sub-m/s sensitivity in measuring the radial velocity (RV) between the Earth and Sun using a simple solar telescope feeding the HARPS-N spectrograph at the Italian National Telescope, which is calibrated with a green astro-comb. We are using the solar telescope to characterize the effects of stellar (solar) RV jitter due to activity on the solar surface with the goal of detecting the solar RV signal from Venus, thereby demonstrating the sensitivity of these instruments to detect true Earth-twin exoplanets.

  14. The Venus Emissivity Mapper - Investigating the Atmospheric Structure and Dynamics of Venus’ Polar Region

    Science.gov (United States)

    Widemann, Thomas; Marcq, Emmanuel; Tsang, Constantine; Mueller, Nils; Kappel, David; Helbert, Joern; Dyar, Melinda; Smrekar, Suzanne

    2017-10-01

    Venus displays the best-known case of polar vortices evolving in a fast-rotating atmosphere. Polar vortices are pervasive in the Solar System and may also be present in atmosphere-bearing exoplanets. While much progress has been made since the early suggestion that the Venus clouds are H2O-H2SO4 liquid droplets (Young 1973), several cloud parameters are still poorly constrained, particularly in the lower cloud layer and optically thicker polar regions. The average particle size is constant over most of the planet but increases toward the poles. This indicates that cloud formation processes are different at latitudes greater than 60°, possibly as a result of the different dynamical regimes that exist in the polar vortices (Carlson et al. 1993, Wilson et al. 2008, Barstow et al. 2012).Few wind measurements exist in the polar region due to unfavorable viewing geometry of currently available observations. Cloud-tracking data indicate circumpolar circulation close to solid-body rotation. E-W winds decrease to zero velocity close to the pole. N-S circulation is marginal, with extremely variable morphology and complex vorticity patterns (Sanchez-Lavega et al. 2008, Luz et al. 2011, Garate-Lopez et al. 2013).The Venus Emissivity Mapper (VEM; Helbert et al., 2016) proposed for NASA’s Venus Origins Explorer (VOX) and the ESA M5/EnVision orbiters has the capability to better constrain the microphysics (vertical, horizontal, time dependence of particle size distribution, or/and composition) of the lower cloud particles in three spectral bands at 1.195, 1.310 and 1.510 μm at a spatial resolution of ~10 km. Circular polar orbit geometry would provide an unprecedented simultaneous study of both polar regions within the same mission. In addition, VEM’s pushbroom method will allow short timescale cloud dynamics to be assessed, as well as local wind speeds, using repeated imagery at 90 minute intervals. Tracking lower cloud motions as proxies for wind measurements at high

  15. The role of Late Veneer impacts in the evolution of Venus

    Science.gov (United States)

    Gillmann, C.; Golabek, G.; Tackley, P.; Raymond, S.

    2017-09-01

    We study how different mechanisms contribute to changes in long term evolution. In particular, the primitive history (the first Gy) of terrestrial planets is heavily influenced by collisions. We investigate how the coupled evolution of Venus' atmosphere and mantle is modified by those impacts. We focus on volatile fluxes: atmospheric escape and mantle degassing. We observe that large impacts are unlikely to erode the atmosphere significantly. They are, on the contrary, an important source of volatiles for the primitive planet. Collisions also generate a lot of melting and rapidly dries the mantle through degassing. Without recycling of volatiles into the mantle (like in plate tectonics regime), the mantle is efficiently depleted.

  16. Venus upper clouds and the UV-absorber from MESSENGER/MASCS observations

    Science.gov (United States)

    Perez-Hoyos, Santiago; Sanchez-Lavega, Agustin; Garcia Munoz, Antonio; Irwin, Patrick; Peralta, Javier; Holsclaw, Greg; McClintock, William

    2014-11-01

    In June 2007, the MESSENGER spacecraft performed its second Venus flyby on its route to Mercury. The spacecraft’s MASCS instrument (VIRS channel) acquired numerous spectra of the sunlight reflected from the equatorial region of the planet at wavelengths from the near ultraviolet (300nm) to the near infrared (1450 nm). In this work we present an analysis of the data and their spectral and spatial variability following the mission footprint on the Venus disk. In order to reproduce the observed reflectivity and obtain information on the upper clouds and the unknown UV absorber, we use the NEMESIS retrieval code, including SO2 , CO2 and H2O absorption together with absorption and scattering by mode-1, -2 and -3 cloud particles. This spectral range provides sensitivity to the uppermost cloud levels, above 60 km. Vertical profiles of the mode-1 and mode-2 particles have been retrieved along the equatorial region of Venus, with average retrieved sounding levels of 70 +/- 2 km at 1 micron, in good agreement with previous investigations. This spectral range is also very interesting because of the existence of a mysterious absorber in the blue and UV side of the reflected spectra, whose origin remains as one of the key questions about the Venus atmosphere. Here we report a comparison with some of the previously proposed absorbers: (1) sulfur-related compounds (amorphous and liquid sulfur, S3, S4, S8, S2O); (2) chlorine related species (Cl2, FeCl3); (3) organics (C3O2, Croconic acid). Preliminary results show that the first group provides better fits to the data, although combinations of the proposed agents might be required in order to produce better results. Acknowledgements: This work was supported by the Spanish MICIIN projects AYA2009- 10701, AYA2012-38897-C02-01, and AYA2012-36666 with FEDER support, PRICIT-S2009/ESP-1496, Grupos Gobierno Vasco IT765-13, and UPV/EHU UFI11/55. S.P.-H. acknowledges support from the Jose Castillejo Program funded by Ministerio de Educaci

  17. Analysis of radiation damage in on-orbit solar array of Venus explorer Akatsuki

    International Nuclear Information System (INIS)

    Toyota, Hiroyuki; Shimada, Takanobu; Takahashi, You; Imamura, Takeshi; Hada, Yuko; Ishii, Takako T.; Isobe, Hiroaki; Asai, Ayumi; Shiota, Daikou

    2013-01-01

    This paper describes an analysis of radiation damage in solar array of Venus explorer Akatsuki observed on orbit. The output voltage of the solar array have shown sudden drops, which are most reasonably associated with radiation damage, three times since its launch. The analysis of these radiation damages is difficult, because no direct observation data of the spectra and the amount of the high-energy particles is available. We calculated the radiation damage using the relative damage coefficient (RDC) method assuming a typical spectral shape of protons. (author)

  18. Conformal Ablative Thermal Protection Systems (CA-TPS) for Venus and Saturn Backshells

    Science.gov (United States)

    Beck, R.; Gasch, M.; Stackpoole, M.; Wilder, M.; Boghozian, T.; Chavez-Garcia, J.; Prabhu, Dinesh; Kazemba, Cole D.; Venkatapathy, E.

    2016-01-01

    This poster provides an overview of the work performed to date on the Conformal Ablative TPS (CA-TPS) element of the TPSM project out of GCDP. Under this element, NASA is developing improved ablative TPS materials based on flexible felt for reinforcement rather than rigid reinforcements. By replacing the reinforcements with felt, the resulting materials have much higher strain-to-failure and are much lower in thermal conductivity than their rigid counterparts. These characteristics should allow for larger tile sizes, direct bonding to aeroshells and even lower weight TPS. The conformal phenolic impregnated carbon felt (C-PICA) is a candidate for backshell TPS for both Venus and Saturn entry vehicles.

  19. The Ontario Energy Board's proposed new mandate

    International Nuclear Information System (INIS)

    Laughren, F.

    1998-01-01

    The Ontario Energy Board's proposed new mandate was reviewed. The role of the Board will be to regulate the monopoly delivery components of the electricity and natural gas industry and to smooth the transition to competition. The Board will monitor market performance and will encourage electricity and natural gas monopoly services to be compatible where possible. The Board will also assist local restructuring efforts when called upon do so and ensure that the marketplace operates efficiently and effectively. Gas marketers' licensing is scheduled to begin in early 1999. Licenses will also apply to the electric industry. The objectives of the proposed licensing, the regulatory requirements and the proposed regulatory approach are described

  20. The Inner Workings of the Board

    DEFF Research Database (Denmark)

    de Haas, Ralph; Ferreira, Daniel; Kirchmaier, Tom

    We survey non-executive directors in emerging markets to obtain detailed information about the inner workings of corporate boards across a variety of institutional settings. We document substantial variation in the structure and conduct of boards as well as in directors’ perceptions about the local...... legal environment. Further analysis indicates that directors who feel adequately empowered by local legislation are less likely to actively vote against board proposals. They also form boards that play a stronger role in the company’s strategic decision-making. This suggests that a supportive legal...