WorldWideScience

Sample records for airglow

  1. Enhanced airglow at Titan

    Science.gov (United States)

    Royer, Emilie; Esposito, Larry; Wahlund, Jan-Erik

    2016-06-01

    The Cassini Ultraviolet Imaging Spectrograph (UVIS) instrument made thousand of observations of Titan since its arrival in the Saturnian system in 2004, but only few of them have been analyzed yet. Using the imaging capability of UVIS combined to a big data analytics approach, we have been able to uncover an unexpected pattern in this observations: on several occasions the Titan airglow exhibits an enhanced brightness by approximately a factor of 2, generally combined with a lower altitude of the airglow emission peak. These events typically last from 10 to 30 minutes and are followed and preceded by an airglow of regular and expected level of brightness and altitude. Observations made by the Cassini Plasma Spectrometer (CAPS) instrument onboard Cassini allowed us to correlate the enhanced airglow observed on T-32 with an electron burst. The timing of the burst and the level of energetic electrons (1 keV) observed by CAPS correspond to a brighter and lower than typical airglow displayed on the UVIS data. Furthermore, during T-32 Titan was inside the Saturn's magnetosheath and thus more subject to bombardment by energetic particles. However, our analysis demonstrates that the presence of Titan inside the magnetosheath is not a necessary condition for the production of an enhanced airglow, as we detected other similar events while Titan was within Saturn's magnetosphere. The study presented here aims to a better understanding of the interactions of Titan's upper atmosphere with its direct environment.

  2. Berkeley extreme-ultraviolet airglow rocket spectrometer - BEARS

    Science.gov (United States)

    Cotton, D. M.; Chakrabarti, S.

    1992-01-01

    The Berkeley EUV airglow rocket spectrometer (BEARS) instrument is described. The instrument was designed in particular to measure the dominant lines of atomic oxygen in the FUV and EUV dayglow at 1356, 1304, 1027, and 989 A, which is the ultimate source of airglow emissions. The optical and mechanical design of the instrument, the detector, electronics, calibration, flight operations, and results are examined.

  3. Equatorial airglow depletions induced by thermospheric winds

    Energy Technology Data Exchange (ETDEWEB)

    Meriwether, J.W.; Biondi, M.A.; Anderson, D.N.

    1985-08-01

    Interferometric observations on the 630.0 nm nightglow brightness at the equatorial station at Arequipa, Peru (16.2 S, 71.4 W geographic, 3.2 S dip latitude) have revealed widespread areas of airglow depletion, with reductions in intensity as large as factors of 3 or 4. These depletions correlated closely with large increases of the equatorward (northward) wind and the 630.0 nm kinetic temperature. On occasion, the usually small meridional wind reached a velocity of 100 m/s near 22h LT lasting for 1 to 2 hours. The temperature increases of 100K or more existed only in the poleware (southward) direction. Comparisons with modeling calculations suggest that this effect results from an upward movement of the ionosphere along the inclined magnetic field lines, driven by the equatorward neutral wind. The airglow column integrated emission rate is consequently decreased by the slower rate of formation and subsequent dissociative recombination of molecular oxygen ions within the higher F-layer. We conclude that the transient period of equatorward wind is a result of the passage of the midnight pressure bulge. (Author)

  4. Equatorial airglow depletions induced by thermospheric winds

    Energy Technology Data Exchange (ETDEWEB)

    Meriwether J.W. Jr.; Biondi, M.A.; Anderson, D.N.

    1985-08-01

    Interferometric observations of the 630.0 nm nightglow brightness at the equatorial station of Arequipa. Peru (16.2/sup 0/S, 71.4/sup 0/W geographic, 3.2/sup 0/S dip latitude) have revealed widespread areas of airglow depletion, with reductions in intensity as large as factors of 3 or 4. These depletions correlated closely with large increases of the equatorward (northward) wind and the 630.0 nm kinetic temperature. On occasion, the usually small meridonal wind reached a velocity of 100 m/s near 22/sup h/ LT lasting for 1 or 2 hours. The temperature increases of 10 K or more existed only in the poleward (southward) direction. Comparisons with modeling calculations suggest that this effect results from an upward movement of the ionosphere along the inclined magnetic field lines, driven by the equatorward neutral wind. The airglow column integrated emission rate is consequently decreased by the slower rate of formation and subsequent dissociative recombination of molecular oxygen ions within the higher F-layer. We conclude that the transient period of equatorward wind is a result of the passage of the midnight pressure bulge.

  5. Mesopause region wind, temperature and airglow irradiance above Eureka, Nunavut

    Science.gov (United States)

    Kristoffersen, Samuel; Ward, William E.; Vail, Christopher; Shepherd, Marianna

    2016-07-01

    The PEARL All Sky Imager (PASI, airglow images), the Spectral Airglow Temperature Imager (SATI, airglow irradiance and temperature) and the E-Region Wind Interferometer II (ERWIN2, wind, airglow irradiance and temperature) are co-located at the Polar Environment Atmospheric Research Laboratory (PEARL)in Eureka, Nunavut (80 N, 86 W). These instruments view the wind, temperature and airglow irradiance of hydroxyl (all three) O2 (ERWIN2 and SATI), sodium (PASI), and oxygen green line (PASI and ERWIN2). The viewing locations and specific emissions of the various instruments differ. Nevertheless, the co-location of these instruments provides an excellent opportunity for case studies of specific events and for intercomparison between the different techniques. In this paper we discuss the approach we are using to combine observations from the different instruments. Case studies show that at times the various instruments are in good agreement but at other times they differ. Of particular interest are situations where gravity wave signatures are evident for an extended period of time and one such situation is presented. The discussion includes consideration of the filtering effect of viewing through airglow layers and the extent to which wind, airglow and temperature variations can be associated with the same gravity wave.

  6. Venus Night Airglow Distibutions and Variability: NCAR VTGCM Simulations

    Science.gov (United States)

    Brecht, Amanda; Bougher, S.; Gerard, J.; Rafkin, S.; Foster, B.

    2008-09-01

    The National Center for Atmospheric Research (NCAR) thermospheric general circulation model for Venus (VTGCM) is producing results that are comparative to Pioneer Venus and Venus Express data. The model is a three dimensional model that can calculate temperatures, zonal winds, meridional winds, vertical winds, and concentration of specific species. The VTGCM can also compute the O2-IR and NO-UV night airglow intensity distributions. With a lower boundary set at 70 Km and a range of sensitivity tests, the VTGCM is able to show consistent set of results with the nightside temperature and the night airglows. These results can show possible controlling parameters of the O2-IR, NO-UV night airglow layers, and the nightside hot spot. Being able to understand the night airglow distribution and variability provides valuable insight into the changing circulation of Venus’ upper atmosphere and leads to an overall planetary perception of the atmospheric dynamics.

  7. HF-induced airglow at magnetic zenith: theoretical considerations

    Directory of Open Access Journals (Sweden)

    E. V. Mishin

    2005-01-01

    Full Text Available Observations of airglow at 630nm (red line and 557.7nm (green line during HF modification experiments at the High Frequency Active Auroral Research Program (HAARP heating facility are analyzed. We propose a theoretical framework for understanding the generation of Langmuir and ion acoustic waves during magnetic zenith injections. We show that observations of HF-induced airglow in an underdense ionosphere as well as a decrease in the height of the emitting volume are consistent with this scenario.

  8. The Nonlinear Model of the Response of Airglow to Gravity Waves

    Institute of Scientific and Technical Information of China (English)

    J. Y. Xu; H. Gao; A.V. Mikhalev

    2005-01-01

    In this paper, we develope a timodependent, nonlinear, photochemical-dynamical 2-D model which is composed of 3 models: dynamical gravity wave model, middle atmospheric photochemical model, and airglow layer photochemical model. We use the model to study the effect of the gravity wave propagation on the airglow layer. The comparison between the effects of the different wavelength gravity wave on the airglow emission distributions is made. When the vertical wavelength of the gravity wave is close to or is shorter than the thickness of the airglow layer, the gravity wave can make complex structure of the airglow layer, such as the double and multi-peak structures of the airglow layer. However, the gravity wave that has long vertical wavelength can make large scale perturbation of the airglow emission distribution.

  9. Measurements of airglow on Maunakea at Gemini Observatory

    Science.gov (United States)

    Roth, Katherine C.; Smith, Adam; Stephens, Andrew; Smirnova, Olesja

    2016-07-01

    Gemini Observatory on Maunakea has been collecting optical and infrared science data for almost 15 years. We have begun a program to analyze imaging data from two of the original facility instruments, GMOS and NIRI, in order to measure sky brightness levels in multiple infrared and optical broad-band filters. The present work includes data from mid-2016 back through late-2008. We present measured background levels as a function of several operational quantities (e.g. moon phase, hours from twilight, season). We find that airglow is a significant contributor to background levels in several filters. Gemini is primarily a queue scheduled telescope, with observations being optimally executed in order to provide the most efficient use of telescope time. We find that while most parameters are well-understood, the atmospheric airglow remains challenging to predict. This makes it difficult to schedule observations which require dark skies in these filters, and we suggest improvements to ensure data quality.

  10. Issues in Quantitative Analysis of Ultraviolet Imager (UV) Data: Airglow

    Science.gov (United States)

    Germany, G. A.; Richards, P. G.; Spann, J. F.; Brittnacher, M. J.; Parks, G. K.

    1999-01-01

    The GGS Ultraviolet Imager (UVI) has proven to be especially valuable in correlative substorm, auroral morphology, and extended statistical studies of the auroral regions. Such studies are based on knowledge of the location, spatial, and temporal behavior of auroral emissions. More quantitative studies, based on absolute radiometric intensities from UVI images, require a more intimate knowledge of the instrument behavior and data processing requirements and are inherently more difficult than studies based on relative knowledge of the oval location. In this study, UVI airglow observations are analyzed and compared with model predictions to illustrate issues that arise in quantitative analysis of UVI images. These issues include instrument calibration, long term changes in sensitivity, and imager flat field response as well as proper background correction. Airglow emissions are chosen for this study because of their relatively straightforward modeling requirements and because of their implications for thermospheric compositional studies. The analysis issues discussed here, however, are identical to those faced in quantitative auroral studies.

  11. OH Airglow and Equatorial Variations Observed by ISUAL Instrument on Board the FORMOSAT 2 Satellite

    Directory of Open Access Journals (Sweden)

    Jan-Bai Nee

    2010-01-01

    Full Text Available OH airglow observed by the ISUAL (Imager of Sprites and Upper Atmospheric Lightning instrument on board the FORMOSAT 2 satellite is reported in this paper. The satellite is sun-synchronous and it returns to the same orbit at the same local time daily. By using this property, we can study the upper atmosphere in detail. With a CCD camera, ISUAL has measured the emission layers of OH Meinel band at 630 nm for several two-week periods in 2004 and 2007 in equatorial regions. ISUAL images are snapshots of the atmosphere 250 km (height _ 1200 km (horizontal distance. These images of OH airglow are analyzed to derive its peak height and latitudinal variations. ISUAL observation is unique in its capability of continuous observation of the upper atmosphere as the satellite travels from south to north along a specific orbit. However, 630 nm filter also measured O(1D at 200 km, and there are interferences between O(1D and OH airglows as as observed from a distance in space. We have studied the overlap of two airglows by simulations, and our final analyses show that OH airglow can be correctly derived with its average peak height of 89 _ 2.1 km usually lying within _ latitude about the equator. ISUAL data reveal detailed structures of equatorial OH airglow such as the existences of a few secondary maxima within the equatorial regions, and the oscillations of the peak latitudes. These results are discussed and compared with previous reports.

  12. All-reflection interferometer for extreme-ultraviolet airglow studies

    Science.gov (United States)

    Cotton, Daniel M.; Chakrabarti, Supriya

    1993-12-01

    We describe a possible sounding rocket payload consisting of an interferometer that would observe O I 1304 equals angstroms solar and airglow emissions simultaneously and a low-resolution (15-angstroms) extreme ultraviolet (EUV) spectrometer with a band pass between 250 and 1050 angstroms to measure the solar EUV flux, a primary source for the O I 1304-angstroms dayglow emission. The solar measurements, the first of their kind, could provide detailed information on the column of O along the line of sight of the instrument as well as information on the full disk solar line profile, which is important to planetary as well as cometary physics. The information gained through line profile studies of the dayglow includes the relative contribution of the two main excitation mechanisms, photoelectron impact and solar resonance scattering, and a means to verify cross sections and branching ratios. All such information will substantiate sophisticated models, electron and radiative transport, that can be utilized in the remote sensing of the thermosphere.

  13. The observation of chemiluminescent NiO* emissions in the laboratory and in the night airglow

    Directory of Open Access Journals (Sweden)

    A. L. Broadfoot

    2011-04-01

    Full Text Available The recent finding of an orange spectral feature in OSIRIS/Odin spectra of the night airglow near 85 km has raised interest in the origin of the emission. The feature was positively identified as the chemiluminescent FeO* emission where the iron is of meteoric origin. Since the meteorite source of atomic metals in the mesosphere contains both iron and nickel, with Ni being typically 6% of Fe, it is expected that faint emissions involving Ni should also be present in the night airglow. The present study summarizes the laboratory observations of chemiluminescent NiO* emissions and includes a search for the NiO* signature in the night airglow. A faint previously unidentified "continuum" extending longwave of 440 nm has been identified in night airglow spectra obtained with two space-borne limb viewing instruments and through a comparison with laboratory spectra this continuum is identified as arising from the NiO* emission. The FeO* and NiO* emissions both originate from a reaction of the metal atoms with mesospheric ozone and so support the presence of NiO* in the night airglow.

  14. The observation of chemiluminescent NiO* emissions in the laboratory and in the night airglow

    Directory of Open Access Journals (Sweden)

    W. F. J. Evans

    2011-09-01

    Full Text Available The recent finding of an orange spectral feature in OSIRIS/Odin spectra of the night airglow near 87 km has raised interest in the origin of the emission. The feature was positively identified as the chemiluminescent FeO* emission where the iron is of meteoric origin. Since the meteorite source of atomic metals in the mesosphere contains both iron and nickel, with Ni being typically 6 % of Fe, it is expected that faint emissions involving Ni should also be present in the night airglow. The present study summarizes the laboratory observations of chemiluminescent NiO* emissions and includes a search for the NiO* signature in the night airglow. A very faint previously unidentified "continuum" extending longwave of 440 nm has been detected in the night airglow spectra obtained with two space-borne limb viewing instruments. Through a comparison with laboratory spectra this continuum is identified as arising from the NiO* emission. The altitude profile of the new airglow emission has also been measured. The similarity of the altitude profiles of the FeO* and NiO* emissions also suggests the emission is NiO as both can originate from reaction of the metal atoms with mesospheric ozone. The observed NiO* to FeO* ratio exhibits considerable variability; possible causes of this observed variation are briefly discussed.

  15. Simulations of airglow variations induced by the CO2 increase and solar cycle variation from 1980 to 1991

    Science.gov (United States)

    Huang, Tai-Yin

    2016-09-01

    Airglow intensity and Volume Emission Rate (VER) variations induced by the increase of CO2 gas concentration and F10.7 variation (used as a proxy for the 11-year solar cycle variation) were investigated for the period from 1980 to 1991, encompassing a full solar cycle. Two airglow models are used to simulate the induced variations of O(1S) greenline, O2(0,1) atmospheric band , and OH(8,3) airglow for this study. The results show that both the airglow intensities and peak VERs correlate positively with the F10.7 solar cycle variation and display a small linear trend due to the increase of CO2 gas concentration. The solar-cycle induced airglow intensity variations show that O(1S) greenline has the largest variation (~26%) followed by the O2(0,1) atmospheric band (~23%) and then OH(8,3) airglow (~8%) over the 11 year timespan. The magnitudes of the induced airglow intensity variations by the increase of CO2 gas concentration are about an order of magnitude smaller than those by the F10.7 solar cycle variation. In general, the F10.7 solar cycle variation and CO2 increase do not seem to systematically alter the VER peak altitude of the airglow emissions, though the OH(8,3) VER peak altitude moves up slightly during the years when the F10.7 value falls under 100 SFU.

  16. Simulations and observations of plasma depletion, ion composition, and airglow emissions in two auroral ionospheric depletion experiments

    Science.gov (United States)

    Yau, A. W.; Whalen, B. A.; Harris, F. R.; Gattinger, R. L.; Pongratz, M. B.

    1985-01-01

    Observations of plasma depletion, ion composition modification, and airglow emissions in the Waterhole experiments are presented. The detailed ion chemistry and airglow emission processes related to the ionospheric hole formation in the experiment are examined, and observations are compared with computer simulation results. The latter indicate that the overall depletion rates in different parts of the depletion region are governed by different parameters.

  17. OH Airglow and Equatorial Variations Observed by ISUAL Instrument on Board the FORMOSAT 2 Satellite

    Directory of Open Access Journals (Sweden)

    Jan-Bai Nee

    2010-01-01

    Full Text Available OH airglow observed by the ISUAL (Imager of Sprites and Upper Atmospheric Lightning instrument on board the FORMOSAT 2 satellite is reported in this paper. The satellite is sun-synchronous and it returns to the same orbit at the same local time daily. By using this property, we can study the upper atmosphere in detail. With a CCD camera, ISUAL has measured the emission layers of OH Meinel band at 630 nm for several two-week periods in 2004 and 2007 in equatorial regions. ISUAL images are snapshots of the atmosphere 250 km (height ¡_ 1200 km (horizontal distance. These images of OH airglow are analyzed to derive its peak height and latitudinal variations. ISUAL observation is unique in its capability of continuous observation of the upper atmosphere as the satellite travels from south to north along a specific orbit. However, 630 nm filter also measured O(1D at 200 km, and there are interferences between O(1D and OH airglows as as observed from a distance in space. We have studied the overlap of two airglows by simulations, and our final analyses show that OH airglow can be correctly derived with its average peak height of 89 ¡_ 2.1 km usually lying within ¡_10¢X latitude about the equator. ISUAL data reveal detailed structures of equatorial OH airglow such as the existences of a few secondary maxima within the equatorial regions, and the oscillations of the peak latitudes. These results are discussed and compared with previous reports.

  18. Hydroxyl (6−2 airglow emission intensity ratios for rotational temperature determination

    Directory of Open Access Journals (Sweden)

    R. P. Lowe

    Full Text Available OH(6–2 Q1/P1 and R1/P1 airglow emission intensity ratios, for rotational states up to j' = 4.5, are measured to be lower than implied by transition probabilities published by various authors including Mies, Langhoff et al. and Turnbull and Lowe. Experimentally determined relative values of j' transitions yield OH(6–2 rotational temperatures 2 K lower than Langhoff et al., 7 K lower than Mies and 13 K lower than Turnbull and Lowe.Key words: Atmospheric composition and structure (airglow and aurora; pressure, density and temperature

  19. Characteristics of equatorial gravity waves derived from mesospheric airglow imaging observations

    Directory of Open Access Journals (Sweden)

    S. Suzuki

    2009-04-01

    Full Text Available We present the characteristics of small-scale (<100 km gravity waves in the equatorial mesopause region derived from OH airglow imaging observations at Kototabang (100.3° E, 0.2° S, Indonesia, from 2002 to 2005. We adopted a method that could automatically detect gravity waves in the airglow images using two-dimensional cross power spectra of gravity waves. The propagation directions of the waves were likely controlled by zonal filtering due to stratospheric mean winds that show a quasi-biennial oscillation (QBO and the presence of many wave sources in the troposphere.

  20. Characteristics of equatorial gravity waves derived from mesospheric airglow imaging observations

    Energy Technology Data Exchange (ETDEWEB)

    Suzuki, S. [Univ. of Electro-Communications, Chofu, Tokyo (Japan). Sugadaira Space Radio Observatory; Shiokawa, K.; Otsuka, Y.; Ogawa, T. [Nagoya Univ., Aichi (Japan). Solar-Terrestrial Environment Lab.; Liu, A.Z. [Illinois Univ., Urbana-Champaign, IL (United States). Dept. of Electrical and Computer Engineering; Nakamura, T. [Kyoto Univ., Uji (Japan). Research Inst. for Sustainable Humanosphere

    2009-07-01

    We present the characteristics of small-scale (<100 km) gravity waves in the equatorial mesopause region derived from OH airglow imaging observations at Kototabang (100.3 E, 0.2 S), Indonesia, from 2002 to 2005. We adopted a method that could automatically detect gravity waves in the airglow images using two-dimensional cross power spectra of gravity waves. The propagation directions of the waves were likely controlled by zonal filtering due to stratospheric mean winds that show a quasi-biennial oscillation (QBO) and the presence of many wave sources in the troposphere. (orig.)

  1. Satellite-based observations of tsunami-induced mesosphere airglow perturbations

    Science.gov (United States)

    Yang, Yu-Ming; Verkhoglyadova, Olga; Mlynczak, Martin G.; Mannucci, Anthony J.; Meng, Xing; Langley, Richard B.; Hunt, Linda A.

    2017-01-01

    Tsunami-induced airglow emission perturbations were retrieved by using space-based measurements made by the Sounding of the Atmosphere using Broad-band Emission Radiometry (SABER) instrument on board the Thermosphere-Ionosphere-Mesosphere Energetics Dynamics spacecraft. At and after the time of the Tohoku-Oki earthquake on 11 March 2011, and the Chile earthquake on 16 September 2015, the spacecraft was performing scans over the Pacific Ocean. Significant ( 10% relative to the ambient emission profiles) and coherent nighttime airglow perturbations were observed in the mesosphere following Sounding of the Atmosphere using Broad-band Emission Radiometry limb scans intercepting tsunami-induced atmospheric gravity waves. Simulations of emission variations are consistent with the physical characteristics of the disturbances at the locations of the corresponding SABER scans. Airglow observations and model simulations suggest that atmospheric neutral density and temperature perturbations can lead to the observed amplitude variations and multipeak structures in the emission profiles. This is the first time that airglow emission rate perturbations associated with tsunamis have been detected with space-based measurements.

  2. Photometric instrument for studies of ionospheric artificial airglow emission caused by antropogenous disturbances

    Science.gov (United States)

    Nasyrov, Igor; Gumerov, Rustam; Nasyrov, Albert; Nikonenkov, Andrey

    One of informative methods of ionospheric processes data acquisition is based on registration of artificial airglow emission. In fact, artificial modifications of the ionosphere by powerful decameter radiowaves cause airglow emission on waves lengths 1270, 630, 557.7, 427.8 nm. In these experiments airglow emission were found at long expositions only as the registration systems of low sensitivity were used. It has allowed investigating the stages when developing of thermal parametric instabilities mechanism contribute mainly into the electron acceleration. The increase of artificial airglow emission at 557.7 nm was caused by impulses with 5 ms duration that corresponds to times of development of pondermotive parametric instability of ionosphere. That effect was found for the first time at the Kazan State University in collabora-tion with NIRFI (N. Novgorod) [Gumerov R.I., Kapkov V.B. et al. //Radiophysics and Quant. Electronics. 1999. Vol 42. P. 463.]. A new mobile photometric instrument equipped with a high-sensitive photometer and CCD-camera, system of GPS time-synchronization, system of "SURA"-channel review by HF-receiver, and systems of experimental data automatic registration by computer was engineered in the Kazan University. One makes possible the investigation of physical processes at the ionosphere disturbed by powerful radioemission, injections of chemically active substances and plasmas beams. The authors gratefully acknowledge Russian Foundation for Basic Research (Grant No 08-02-01188) for the financial support.

  3. HF-induced airglow structure as a proxy for ionospheric irregularity detection

    Science.gov (United States)

    Kendall, E. A.

    2013-12-01

    The High Frequency Active Auroral Research Program (HAARP) heating facility allows scientists to test current theories of plasma physics to gain a better understanding of the underlying mechanisms at work in the lower ionosphere. One powerful technique for diagnosing radio frequency interactions in the ionosphere is to use ground-based optical instrumentation. High-frequency (HF), heater-induced artificial airglow observations can be used to diagnose electron energies and distributions in the heated region, illuminate natural and/or artificially induced ionospheric irregularities, determine ExB plasma drifts, and measure quenching rates by neutral species. Artificial airglow is caused by HF-accelerated electrons colliding with various atmospheric constituents, which in turn emit a photon. The most common emissions are 630.0 nm O(1D), 557.7 nm O(1S), and 427.8 nm N2+(1NG). Because more photons will be emitted in regions of higher electron energization, it may be possible to use airglow imaging to map artificial field-aligned irregularities at a particular altitude range in the ionosphere. Since fairly wide field-of-view imagers are typically deployed in airglow campaigns, it is not well-known what meter-scale features exist in the artificial airglow emissions. Rocket data show that heater-induced electron density variations, or irregularities, consist of bundles of ~10-m-wide magnetic field-aligned filaments with a mean depletion depth of 6% [Kelley et al., 1995]. These bundles themselves constitute small-scale structures with widths of 1.5 to 6 km. Telescopic imaging provides high resolution spatial coverage of ionospheric irregularities and goes hand in hand with other observing techniques such as GPS scintillation, radar, and ionosonde. Since airglow observations can presumably image ionospheric irregularities (electron density variations), they can be used to determine the spatial scale variation, the fill factor, and the lifetime characteristics of

  4. Application of tomographic inversion in studying airglow in the mesopause region

    Directory of Open Access Journals (Sweden)

    T. Nygrén

    Full Text Available It is pointed out that observations of periodic nightglow structures give excellent information on atmospheric gravity waves in the mesosphere and lower thermosphere. The periods, the horizontal wavelengths and the phase speeds of the waves can be determined from airglow images and, using several cameras, the approximate altitude of the luminous layer can also be determined by triangulation. In this paper the possibility of applying tomographic methods for reconstructing the airglow structures is investigated using numerical simulations. A ground-based chain of cameras is assumed, two-dimensional airglow models in the vertical plane above the chain are constructed, and simulated data are calculated by integrating the models along a great number of rays with different elevation angles for each camera. After addition of random noise, these data are then inverted to obtain reconstructions of the models. A tomographic analysis package originally designed for satellite radiotomography is used in the inversion. The package is based on a formulation of stochastic inversion which allows the input of a priori information to the solver in terms of regularization variances. The reconstruction is carried out in two stages. In the first inversion, constant regularization variances are used within a wide altitude range. The results are used in determining the approximate altitude range of the airglow structures. Then, in the second inversion, constant non-zero regularization variances are used inside this region and zero variances outside it. With this method reliable reconstructions of the models are obtained. The number of cameras as well as their separations are varied in order to find out the limitations of the method.

    Key words. Tomography · Airglow · Mesopause · Gravity waves

  5. Cassini UVIS observations of Titan ultraviolet airglow intensity dependence with solar zenith angle

    Science.gov (United States)

    Royer, E. M.; Ajello, J. M.; Holsclaw, G. M.; West, R. A.; Esposito, L. W.; Bradley, E. T.

    2017-01-01

    The Cassini Ultraviolet Imaging Spectrometer (UVIS) observed the airglow (dayglow and nightglow) of Titan over a range of solar zenith angles (SZA) from 14 to 150° on five separate observations obtained between 2008 and 2012. The modeling of the solar cycle normalized UVIS observations indicates that a Chapman layer function provides a satisfactory fit to the intensity of the EUV and FUV airglow molecular emissions of the N2 Lyman-Birge-Hopfield band system (LBH a1Πg→X1>∑g+), the Carroll-Yoshino band system (c4'1>∑u+→X1>∑g+), and of several atomic multiplets of nitrogen (NI, II) as a function of SZA. This result shows that the strongest contribution to the Titan dayglow occurs by processes (photoelectrons and photodissociation) involving the solar EUV flux rather than magnetospheric particle precipitation that dominates emission excitation in the nightglow.

  6. Mars dayside temperature from airglow limb profiles : comparison with in situ measurements and models

    Science.gov (United States)

    Gérard, Jean-Claude; Bougher, Stephen; Montmessin, Franck; Bertaux, Jean-Loup; Stiepen, A.

    The thermal structure of the Mars upper atmosphere is the result of the thermal balance between heating by EUV solar radiation, infrared heating and cooling, conduction and dynamic influences such as gravity waves, planetary waves, and tides. It has been derived from observations performed from different spacecraft. These include in situ measurements of orbital drag whose strength depends on the local gas density. Atmospheric temperatures were determined from the altitude variation of the density measured in situ by the Viking landers and orbital drag measurements. Another method is based on remote sensing measurements of ultraviolet airglow limb profiles obtained over 40 years ago with spectrometers during the Mariner 6 and 7 flybys and from the Mariner 9 orbiter. Comparisons with model calculations indicate that they both reflect the CO_2 scale height from which atmospheric temperatures have been deduced. Upper atmospheric temperatures varying over the wide range 270-445 K, with a mean value of 325 K were deduced from the topside scale height of the airglow vertical profile. We present an analysis of limb profiles of the CO Cameron (a(3) Pi-X(1) Sigma(+) ) and CO_2(+) doublet (B(2) Sigma_u(+) - X(2) PiΠ_g) airglows observed with the SPICAM instrument on board Mars Express. We show that the temperature in the Mars thermosphere is very variable with a mean value of 270 K, but values ranging between 150 and 400 K have been observed. These values are compared to earlier determinations and model predictions. No clear dependence on solar zenith angle, latitude or season is apparent. Similarly, exospheric variations with F10.7 in the SPICAM airglow dataset are small over the solar minimum to moderate conditions sampled by Mars Express since 2005. We conclude that an unidentified process is the cause of the large observed temperature variability, which dominates the other sources of temperature variations.

  7. Imaging mesospheric winds using the Michelson interferometer for airglow dynamics imaging

    Science.gov (United States)

    Langille, Jeffery; Ward, William E.

    2016-07-01

    The first ground based images of mesospheric winds in airglow are presented and discussed in this paper. These were obtained with the Michelson Interferometer for Airglow Dynamics Imaging (MIADI)a ground based field widened Michelsoin interferometer designed to obtain two dimensional images of the line of sight Doppler wind and irradiance field in the mesosphere. The purpose of this instrument is to measure perturbations in line-of-sight wind and airglow irradiance associated with gravity waves. In its current configuration, the instrument observes an ~80 km x ~80 km region of the night sky in ~33 minutes using the O(1S) emission at 557.73 nm and the OH (6, 2) P1 (2) emission at 839.918 nm. The instrument was installed and tested at a field site outside Fredericton, NB (45.96 N, 66.65 W) during the summer of 2014. Successful measurements over a six hour period were obtained on July 31, 2014. Variations in the meridional and zonal wind were observed that are consistent with a semi-diurnal tide with an amplitude of ˜ 35 m/s. Small scale variations (< 10 m/s) were also observed that indicate the presence of gravity waves. In this paper, the instrument concept will be presented and the field measurements and their precision and accuracy discussed.

  8. Equatorial Spread F structures and associated airglow intensity variations observed over Gadanki

    Directory of Open Access Journals (Sweden)

    R. Sekar

    2008-12-01

    Full Text Available Co-ordinated campaigns have been conducted from Gadanki (13.5° N, 79.2° E, dip lat 6.4° N by operating simultaneously the Indian MST radar in ionospheric coherent backscatter mode and by monitoring thermosphere airglow line emissions (630.0 nm and 777.4 nm using a narrow band multi-wavelength scanning photometer during January-March for the past five years (2003–2007 and also during April 2006, as a special campaign. Simultaneous radar and optical observations reveal optical signatures corresponding to a variety of equatorial spread F (ESF structures. The optical signatures corresponding to ESF structures with wave-like bottomside modulations with plasma plumes, confined bottomside flat and wavelike structures, vertically extended plume structure in the absence of bottomside structure apart from the classical plasma depletions and enhancements are obtained during these campaigns. The plasma depletions and enhancements were identified using optical measurements. In addition, estimations of zonal wavelength of the bottomside structures and the inference of shears in the zonal plasma drift in the presence of confined structures, were carried out using bi-directional airglow measurements. Furthermore, it is found that the vertical columnar intensity of OI 630.0 nm airglow exceeded the slanted columnar intensity in the presence of large bottomside structure. The need for the appropriate physical mechanisms for some of the ESF structures and their characterizations with optical observations are discussed.

  9. Calibration of imaging parameters for space-borne airglow photography using city light positions

    Science.gov (United States)

    Hozumi, Yuta; Saito, Akinori; Ejiri, Mitsumu K.

    2016-09-01

    A new method for calibrating imaging parameters of photographs taken from the International Space Station (ISS) is presented in this report. Airglow in the mesosphere and the F-region ionosphere was captured on the limb of the Earth with a digital single-lens reflex camera from the ISS by astronauts. To utilize the photographs as scientific data, imaging parameters, such as the angle of view, exact position, and orientation of the camera, should be determined because they are not measured at the time of imaging. A new calibration method using city light positions shown in the photographs was developed to determine these imaging parameters with high accuracy suitable for airglow study. Applying the pinhole camera model, the apparent city light positions on the photograph are matched with the actual city light locations on Earth, which are derived from the global nighttime stable light map data obtained by the Defense Meteorological Satellite Program satellite. The correct imaging parameters are determined in an iterative process by matching the apparent positions on the image with the actual city light locations. We applied this calibration method to photographs taken on August 26, 2014, and confirmed that the result is correct. The precision of the calibration was evaluated by comparing the results from six different photographs with the same imaging parameters. The precisions in determining the camera position and orientation are estimated to be ±2.2 km and ±0.08°, respectively. The 0.08° difference in the orientation yields a 2.9-km difference at a tangential point of 90 km in altitude. The airglow structures in the photographs were mapped to geographical points using the calibrated imaging parameters and compared with a simultaneous observation by the Visible and near-Infrared Spectral Imager of the Ionosphere, Mesosphere, Upper Atmosphere, and Plasmasphere mapping mission installed on the ISS. The comparison shows good agreements and supports the validity

  10. First mesospheric wind images using the Michelson interferometer for airglow dynamics imaging.

    Science.gov (United States)

    Langille, J A; Ward, W E; Nakamura, T

    2016-12-10

    The Michelson interferometer for airglow dynamics imaging (MIADI) is a ground-based instrument that combines an imaging capability with the Doppler Michelson interferometry in order to remotely detect motions in the mesopause region using spectrally isolated airglow emissions: the O(S1) emission at 557.73 nm and the OH (6, 2) P1 (2) at 839.918 nm. A measurement and analysis approach has been developed that allows simultaneous images of the line-of-sight Doppler wind field and irradiance field to be obtained. A working field instrument was installed and tested at a field site outside Fredericton, NB (45.96 N, 66.65 W) during the summer of 2014. Successful measurements over a 6 h period were obtained on 31 July 2014. This paper describes the MIADI measurement and analysis approach and presents the work that has been done to extract images of the line-of-sight Doppler wind field and irradiances from these observations. The imaging capability is validated by identifying the presence of large-scale and small-scale geophysical perturbations in the images.

  11. Modeling of Na airglow emission and first results on the nocturnal variation at midlatitude

    Science.gov (United States)

    Bag, T.; Sunil Krishna, M. V.; Singh, Vir

    2015-12-01

    A model for sodium airglow emission is developed by incorporating all the known reaction mechanisms. The neutral, ionic, and photochemical mechanisms are successfully implemented into this model. The values of reaction rate coefficients are based upon the theoretical calculations as well as from experimental observations. The densities of major species are calculated using the continuity equations, whereas for the minor, intermediating, and short-lived species steady state approximation method is used. The modeled results are validated with the rocket, lidar, and photometer observations for a branching ratio of 0.04 for the production of Na(2P) in the reaction NaO + O → Na(2P, 2S). The inputs have been obtained from other physics-based models and ground- and satellite-based observations to give the combined volume emission rate (VER) of Na airglow between 80 and 110 km altitude. In the present study, the model is used to understand the nocturnal variation of Na VER during the solstice conditions. The model results suggest a variation of peak emission layer between 85 and 90 km during summer solstice condition, indicating a lower value of peak emission rate during summer solstice. The emission rates bear a strong correlation with the O3 density during summer solstice, whereas the magnitude of VER follows the Na density during winter solstice. The altitude of peak VER shows an upward shift of 5 km during winter solstice.

  12. Monitoring Saturn's Upper Atmosphere Density Variations Using Helium 584 Å Airglow

    Science.gov (United States)

    Parkinson, Chris

    2016-10-01

    The study of He 584 Å brightness of Saturn is interesting as the EUV planetary airglow have the potential to yield useful information about mixing and other important parameters in its thermosphere. Resonance scattering of sunlight by He atoms is the principal source of the planetary emission of He 585 Å. The helium is embedded in an absorbing atmosphere of H2 and since it is heavier than the background atmosphere, it's concentration falls off rapidly above the homopause. The scattering region (i.e. where the absorption optical depth in H2 is greatly improved estimate of the mixing ratio of He in the upper atmosphere and below. The second topic addressed is regarding constraining the dynamics in the atmosphere by using the estimate of the He mixing ratio from the main objective. Once we have an estimate of the He mixing ratio in the lower atmosphere that agrees with both occultations and airglow, helium becomes an effective tracer species as any variations in the Cassini UVIS helium data are direct indicator of changes in Kzz i.e., dynamics.

  13. First Light from Triple-Etalon Fabry-Perot Interferometer for Atmospheric OI Airglow (6300 A)

    Science.gov (United States)

    Watchorn, S.; Noto, J.; Pedersen, T.; Betremieux, Y.; Migliozzi, M.; Kerr, R. B.

    2006-05-01

    Scientific Solutions, Inc. (SSI) has developed a triple-etalon Fabry-Perot interferometer (FPI) to observe neutral winds in the ionosphere by measuring neutral oxygen (O I) emission at 630.0 nm during the day. This instrument is to be deployed in the SSI airglow building at the Cerro Tololo observatory (30.17S 70.81W) in Chile, in support of the Comm/Nav Outage Forecast System (C/NOFS) project. Post-deployment observation will be made in conjunction with two other Clemson University Fabry-Perots in Peru, creating a longitudinal chain of interferometers for thermospheric observations. These instruments will make autonomous day and night observations of thermospheric dynamics. Instruments of this type can be constructed for a global chain of autonomous airglow observatories. The FPI presented in this talk consists of three independently pressure-controlled etalons, fed collimated light by a front optical train headed by an all-sky lens with a 160-degree field of view. It can be controlled remotely via a web-based service which allows any internet-connected computer to mimic the control computer at the instrument site. In fall 2005, the SSI system was first assembled at the Millstone Hill Observatory in Westford, Massachusetts, and made day and evening observations. It was then moved to the High-frequency Active Auroral Research Project (HAARP) site in Gakona, Alaska, to participate in joint optical/ionospheric heating campaigns. Additionally, natural airglow observations were made, both locally and remotely via the internet from Massachusetts. The Millstone and HAARP observations with two etalons yielded strong 630-nm atmospheric Fraunhofer absorption lines, with some suggestion of the Ring effect. By modeling the atmospheric absorption line as the constant times the corresponding solar absorption -- itself modeled as a Gaussian plus a polynomial -- the absorption feature is subtracted, leaving only the emission feature. Software ring-summing tools developed at the

  14. Collocated infrasound/airglow observations of eruptive activity at Etna volcano

    Science.gov (United States)

    Marchetti, Emanuele; Ripepe, Maurizio; Wüst, Sabine; Schmidt, Carsten; Kramer, Ricarda; Bittner, Michael

    2014-05-01

    In the framework of the FP7 ARISE design study project, a collocated infrasound and airglow observation campaign has been organized on Etna volcano. The experiment, carried out during the first 2 years of the project (January 2012-December 2013), consists of simultaneous observations with an infrasound array, operated by UNIFI, and a GRIPS airglow spectrometers, operated by DLR. The infrasound array, deployed on the eastern flank of the volcano at ~2000 m elevation and at a distance of ~5 km from the active craters, allows to detect and analyse infrasound radiated by eruptive activity from Etna volcano and provides the detailed time history of the infrasonic pressure related to the Etna explosive activity. The GRIPS spectrometer is deployed in the city of Catania at a distance of ~ 30 km from the craters and targeting the sky above the summit craters, allowing to measure temperature fluctuations of the airglow layer and thus to retrieve pressure fluctuations in the mesopause region. Given the high efficiency of the Etna volcano to radiate infrasound, the campaign aimed to study the infrasound propagation from the ground to the high atmosphere, as well as to investigate relationship between the eruptive plume and the atmospheric dynamics. Mass injection into a stratified atmosphere results into gravity waves controlled by the Brunt-Vaisala frequency. Here volcanic eruption, able to inject rapidly a large quantity of hot material into a stratified atmosphere is able to excite gravity waves into the atmosphere, that in turn will control the evolution of the eruptive umbrella clouds. Moreover, gravity waves generated by atmospheric dynamics can somehow control the evolution and dispersal of eruptive plume. Gravity waves during the 2012-2013 period are detected from GRIPS measurements, and detailed infrasonic time history is derived from infrasound observation. Here activity from Etna volcano during the experiment was very intense, and was punctuated by 30 lava fountain

  15. A GIANO-TNG high resolution IR spectrum of the airglow emission

    CERN Document Server

    Oliva, E; Maiolino, R; Baffa, C; Biliotti, V; Bruno, P; Falcini, G; Gavriousev, V; Ghinassi, F; Giani, E; Gonzalez, M; Leone, F; Lodi, M; Massi, F; Montegriffo, P; Mochi, I; Pedani, M; Rossetti, E; Scuderi, S; Sozzi, M; Tozzi, A; Valenti, E

    2013-01-01

    A flux-calibrated high resolution spectrum of the airglow emission is a practical lambda-calibration reference for astronomical spectral observations. It is also useful for constraining the molecular parameters of the OH molecule and the physical conditions in the upper mesosphere. methods: We use the data collected during the first technical commissioning of the GIANO spectrograph at the Telescopio Nazionale Galileo (TNG). The high resolution (R~50,000) spectrum simultaneously covers the 0.95-2.4 micron wavelength range. Relative flux calibration is achieved by the simultaneous observation of spectrophotometric standard star. results: We derive a list of improved positions and intensities of OH infrared lines. The list includes Lambda-split doublets many of which are spectrally resolved. Compared to previous works, the new results correct errors in the wavelengths of the Q-branch transitions. The relative fluxes of OH lines from different vibrational bands show remarkable deviations from theoretical predicti...

  16. Use of O2 airglow for calibrating direct atomic oxygen measurements from sounding rockets

    Directory of Open Access Journals (Sweden)

    G. Witt

    2009-12-01

    Full Text Available Accurate knowledge about the distribution of atomic oxygen is crucial for many studies of the mesosphere and lower thermosphere. Direct measurements of atomic oxygen by the resonance fluorescence technique at 130 nm have been made from many sounding rocket payloads in the past. This measurement technique yields atomic oxygen profiles with good sensitivity and altitude resolution. However, accuracy is a problem as calibration and aerodynamics make the quantitative analysis challenging. Most often, accuracies better than a factor 2 are not to be expected from direct atomic oxygen measurements. As an example, we present results from the NLTE (Non Local Thermodynamic Equilibrium sounding rocket campaign at Esrange, Sweden, in 1998, with simultaneous O2 airglow and O resonance fluorescence measurements. O number densities are found to be consistent with the nightglow analysis, but only within the uncertainty limits of the resonance fluorescence technique. Based on these results, we here describe how better atomic oxygen number densities can be obtained by calibrating direct techniques with complementary airglow photometer measurements and detailed aerodynamic analysis. Night-time direct O measurements can be complemented by photometric detection of the O2 (b1∑g+−X3∑g- Atmospheric Band at 762 nm, while during daytime the O2 (a1Δg−X3∑g- Infrared Atmospheric Band at 1.27 μm can be used. The combination of a photometer and a rather simple resonance fluorescence probe can provide atomic oxygen profiles with both good accuracy and good height resolution.

  17. Mesoscale field-aligned irregularity structures (FAIs) of airglow associated with medium-scale traveling ionospheric disturbances (MSTIDs)

    Science.gov (United States)

    Sun, Longchang; Xu, Jiyao; Wang, Wenbin; Yue, Xinan; Yuan, Wei; Ning, Baiqi; Zhang, Donghe; Meneses, F. C.

    2015-11-01

    In this paper, we report the evolution (generation, amplification, and dissipation) of optically observed mesoscale field-aligned irregularity structures (FAIs) (~150 km) associated with a medium-scale traveling ionospheric disturbance (MSTID) event. There have not been observations of mesoscale FAIs of airglow before. The mesoscale FAIs were generated in an airglow-depleted front of southwestward propagating MSTIDs that were simultaneously observed by an all-sky imager, a GPS monitor, and a digisonde around Xinglong (40.4°N, 30.5° magnetic latitude), China, on 17/18 February 2012. A normalized cross-correlation method has been used to obtain the velocities of mesoscale FAIs and MSTIDs. The mesoscale FAIs had an obvious northwestward relative velocity to main-body MSTIDs (about 87.0 m/s on average). The direction of this relative velocity was roughly parallel to the depleted fronts. Furthermore, the evolution of the mesoscale FAIs was mostly controlled by the intensity of the depleted fronts. Occurred in a highly elevated ionosphere that had a total electron content depletion associated with large negative airglow perturbations (-25%), the mesoscale FAIs grew rapidly when they experienced southeastward wind, which had a speed of about 100 m/s and were measured by a Fabry-Perot interferometer. A northeastward polarization electric field within a depleted airglow front can play a controlling role in the development of the mesoscale FAIs. The electric field can significantly elevate the ionosphere and move the mesoscale FAIs northwestward by the E × B drift. The processes for the generation and development of the polarization electric field and the mesoscale FAIs, however, need further study.

  18. Partially light-controlled imager based on liquid crystal plate and image intensifier for aurora and airglow measurement.

    Science.gov (United States)

    Tang, Yuanhe; Cao, Xiangang; Liu, Hanchen; Shepherd, G G; Liu, Shulin; Gao, Haiyang; Yang, Xusan; Wu, Yong; Wang, Shuiwei

    2012-04-20

    In order to obtain information both of aurora and airglow in one image by the same detector, a PLCI based on liquid crystal plate LCP and super second-generation image intensifier SSGII is proposed in this research. The detection thresholds of the CCD for aurora and airglow are calculated. For the detectable illumination range of 10(4)-10(-2) lx, the corresponding electron count is 1.57×10(5) - 0.2 for every pixel of CCD. The structure and work principle of the PLCI are described. An LC is introduced in the front of CCD to decrease the intensities of aurora in overexposure areas by means of controlling transmittances pixel by pixel, while an image intensifier is set between the LC and CCD to increase the intensity of the weak airglow. The modulation transfer function MTF of this system is calculated as 0.391 at a Nyquist frequency of 15 lp/mm. The curve of transmittance with regard to gray level for the LC is obtained by calibration experiment. Based on the design principle, the prototype is made and used to take photos of objects under strong light greater than 2×10(5) lx. The clear details of [symbols: see text] presented in the image indicate that the PLCI can greatly improve the imaging quality. The theoretical calculations and experiment results prove that this device can extend the dynamic range and it provides a more effective method for upper atmospheric wind measurement.

  19. Helium 584 Å and H Lyman-α Airglow in Giant Planetary Atmospheres: Modeling, Observations, and Implications

    Science.gov (United States)

    Parkinson, Christopher; Esposito, Larry W.

    2016-07-01

    The atmosphere of the outer planets is mainly composed of H2 and neutral atomic helium. The study of He 584 Å and H Lyman-α brightnesses is interesting as the EUV and FUV (Extreme and Far Ultraviolet) planetary airglow have the potential to yield useful information about mixing and other important parameters in their thermospheres. Time variation, asymmetries, and polar enhancement of the airglow are also possible and analysis of the public archived NASA mission data sets (i.e. Voyager and Cassini) can help solve some of the outstanding problems associated with these phenomena. The comparison of observations with results from sophisticated photochemical and radiative transfer models can also help ameliorate unexplained differences in the dynamical processes operating within planetary upper atmospheres. Powerful analysis techniques allow us to extract information on atmospheric mixing, temperatures, and temporal changes due to the solar and seasonal cycles from the variations in distribution and intensity of airglow emissions that result. The presentation will discuss the implications of interpretations from comparison of modeling and observations in giant planetary atmospheres.

  20. New approach of gravity wave detection in mesopause temperatures operating an array of airglow spectrometers

    Science.gov (United States)

    Wachter, Paul; Schmidt, Carsten; Wüst, Sabine; Bittner, Michael

    2014-05-01

    GRIPS (Ground based Infrared P-branch Spectrometer) airglow measurements allow the derivation of kinetic temperature in the mesopause region averaged over a field of view of some 10km x 10km. In 2011, three identical GRIPS instruments were setup at Oberpfaffenhofen (11.28°E, 48.09°N), Germany, in a way that their fields of view form an equilateral triangle shape in the mesopause with a horizontal dimension of approximately 70km. Using this setup, GRIPS time series cannot only be analyzed with respect to gravity wave periods, but also spatial wave parameters can be derived. Based on the results of the harmonic analysis the horizontal wavelength, phase speed and the direction of propagation were determined for gravity wave events from February to July 2011. We present distinct relationships between periods, amplitudes, phase speeds and wavelengths, which were identified in this dataset. Further data analysis of the derived wave parameters show preferred directions of propagation and suggest seasonal variations of the wave characteristics. The presentation will be concluded by the introduction of a measurement setup relying on one GRIPS instrument which is equipped with a variably adjustable mirror optic. The capability to scan multiple fields of view during nightly measurements will offer longer-term investigations of mesopause gravity waves.

  1. Tidal and gravity waves study from the airglow measurements at Kolhapur (India)

    Indian Academy of Sciences (India)

    R N Ghodpage; Devendraa Siingh; R P Singh; G K Mukherjee; P Vohat; A K Singh

    2012-12-01

    Simultaneous photometric measurements of the OI 557.7 nm and OH (7, 2) band from a low latitude station, Kolhapur (16.8°N, 74.2°E) during the period 2004–2007 are analyzed to study the dominant waves present in the 80–100 km altitude region of the atmosphere. The nocturnal intensity variations of different airglow emissions are observed using scanning temperature controlled filter photometers. Waves having period lying between 2 and 12 hours have been recorded. Some of these waves having subharmonic tidal oscillation periods 4, 6, 8 and 12 hours propagate upward with velocity lying in the range 1.6–11.3 m/s and the vertical wave length lying between 28.6 and 163 kms. The other waves may be the upward propagating gravity waves or waves resulting from the interaction of inter-mode tidal oscillations, interaction of tidal waves with planetary waves and gravity waves. Some times, the second harmonic wave has higher vertical velocity than the corresponding fundamental wave. Application of these waves in studying the thermal structure of the region is discussed.

  2. Case study of convective instability observed in airglow images over the Northeast of Brazil

    Science.gov (United States)

    Carvalho, A. J. A.; Paulino, I.; Medeiros, A. F.; Lima, L. M.; Buriti, R. A.; Paulino, A. R.; Wrasse, C. M.; Takahashi, H.

    2017-02-01

    An intense activity of ripples during the nighttime was observed in airglow images over São João do Cariri (36.5° W, 7.4° S) on 10 October 2004 which lasted for two hours. Those ripples appeared simultaneously with the crossing of a mesospheric front and medium scale gravity waves. The ripples occurred ahead of the mesospheric front and their phase front were almost parallel to the phase of the mesospheric front and were almost perpendicular to the phase front of the gravity wave. Using wind measurements from a meteor radar located at São João do Cariri and simultaneous vertical temperature profiles from the TIMED/SABER satellite, on the night of the events and within the imager field of view, the atmospheric background environment in the mesosphere and lower thermosphere (MLT) was investigated in order to understand the instability process that caused the appearance of the ripples. Dynamic and convective instabilities have been pointed out as responsible for creation of ripples in the MLT. The observed ripples were advected by the neutral wind, they occurred into a region with negative lapse rate of the potential temperature and the Richardson number was negative as well. According to these characteristics, the ripple structures could be generated in the MLT region due to the predominance of convective instability.

  3. Atmospheric wave induced O2 and OH airglow intensity variations: effect of vertical wavelength and damping

    Directory of Open Access Journals (Sweden)

    D. Gobbi

    2011-04-01

    Full Text Available From nocturnal variations of the airglow O2 (0-1 and OH Meinel (6-2 band emission intensity and the rotational temperature, gravity waves and the damping effect in the MLT region were investigated. The data set was obtained from photometer measurements at Rikubetsu (43.5° N, 143.8° E, Japan, from March 2004 to August 2005. The ratio of the amplitude of oscillation and their phase difference between the two emissions were calculated when simultaneous periodic variations were observed. The ratio showed a linear correlation with the phase difference. The vertical wavelength and damping rate were estimated by using a model calculation carried out by previous works. The results show that the wave damping is significant when the vertical wavelength is shorter than 30–40 km. Krassovsky's parameter η, which represents a ratio between the emission intensity and temperature oscillations, was also calculated. The results show that the η also depends on the damping effect.

  4. The first coordinated observations of mid-latitude E-region quasi-periodic radar echoes and lower thermospheric 557.7-nm airglow

    Directory of Open Access Journals (Sweden)

    M. Yamamoto

    2005-10-01

    Full Text Available We present the first coordinated observations of quasi-periodic (QP radar echoes from sporadic-E (Es field-aligned irregularities (FAIs, OI 557.7-nm airglow, and neutral winds in a common volume over Shigaraki, Japan (34.9° N, 136.1° E on the night of 5 August 2002 during the SEEK-2 campaign. QP echo altitudes of 90-110 km were lower than usual by 10 km, enabling us to make a detailed comparison among QP echoes, airglow intensity, and neutral wind at around 96 km altitude. Eastward movement of the QP echo regions is consistent with the motions of neutral winds, airglow structures, and FAIs, suggesting that the electrodynamics of Es-layers is fundamentally controlled by the neutral atmospheric dynamics. During the QP echo event, the echo altitudes clearly went up (down in harmony with an airglow enhancement (subsidence that also moved to the east. This fact suggests that the eastward-moving enhanced airglow region included an upward (downward component of neutral winds to raise (lower the altitude of the wind-shear node responsible for the Es formation. The airglow intensity, echo intensity, and Doppler velocity of FAIs at around 96 km altitude fluctuated with periods from 10 min to 1h, indicating that these parameters were modulated with short-period atmospheric disturbances. Some QP echo regions below 100km altitude contained small-scale QP structures in which very strong neutral winds exceeding 100 m/s existed. The results are compared with recent observations, theories, and simulations of QP echoes. Keywords. Ionosphere (Ionosphere-atmosphere interactions; Ionospheric irregularities; Mid-latitude ionosphere

  5. Metal Retrievals in the Mesosphere and lower Thermosphere by remote Sensing of Airglow with SCIAMACHY/Envisat

    Science.gov (United States)

    Langowski, M.; von Savigny, C.; Sinnhuber, M.; Aikin, A. C.; Burrows, J. P.

    2013-12-01

    Meteors entering the earth atmosphere containing metals ablate in an altitude of approximately 100 km due to frictional heating. The ablated metals undergo a series of chemical processes, which finally leads to a formation of metal layers between 85-95 km and metal ion layers 5 to 15 km above the metal layer. Although the densities of the metals and their ions are only in the magnitude of a few thousands of particles per cubic centimeter, they strongly emit airglow radiation due to their strong absorption cross sections and oscillator strength. This Airglow can be detected e.g. by grating spectrometers and the the density of the metals and ions can be obtained by inversion of a radiative transfer model. Since the Mesosphere and lower Thermosphere can hardly be accessed by in-situ measurement, as ballons fly to low and satellites typically too high and rockets to sparsly, the airglow emission of the metals and ions is one of the few means in this region to obtain information about transport and wave activities. Furthermore the total meteoric input to earth, which is quite uncertain in a range from 2 to 300 t/day can be estimated from the densties in the metal layers. We present metal and ion retrievals from SCIAMACHY/Envisat which is a satellite based grating spectrometer with a wavelength range of 230 to 2300 nm. The presented results are retrieved from the limb MLT states scanning the atmosphere with tangent altitudes from 50 to 150 km every 2 weeks for one day of data since 2008 until 2012.

  6. Spatial gravity wave characteristics obtained from multiple OH(3-1) airglow temperature time series

    Science.gov (United States)

    Wachter, Paul; Schmidt, Carsten; Wüst, Sabine; Bittner, Michael

    2015-12-01

    We present a new approach for the detection of gravity waves in OH-airglow observations at the measurement site Oberpfaffenhofen (11.27°E, 48.08°N), Germany. The measurements were performed at the German Remote Sensing Data Center (DFD) of the German Aerospace Center (DLR) during the period from February 4th, 2011 to July 6th, 2011. In this case study the observations were carried out by three identical Ground-based Infrared P-branch Spectrometers (GRIPS). These instruments provide OH(3-1) rotational temperature time series, which enable spatio-temporal investigations of gravity wave characteristics in the mesopause region. The instruments were aligned in such a way that their fields of view (FOV) formed an equilateral triangle in the OH-emission layer at a height of 87 km. The Harmonic Analysis is applied in order to identify joint temperature oscillations in the three individual datasets. Dependent on the specific gravity wave activity in a single night, it is possible to detect up to four different wave patterns with this method. The values obtained for the waves' periods and phases are then used to derive further parameters, such as horizontal wavelength, phase velocity and the direction of propagation. We identify systematic relationships between periods and amplitudes as well as between periods and horizontal wavelengths. A predominant propagation direction towards the East and North-North-East characterizes the waves during the observation period. There are also indications of seasonal effects in the temporal development of the horizontal wavelength and the phase velocity. During late winter and early spring the derived horizontal wavelengths and the phase velocities are smaller than in the subsequent period from early April to July 2011.

  7. Spatial and Temporal Stability of Airglow Measured in the Meinel Band Window at 1191.3 nm

    CERN Document Server

    Nguyen, Hien T; Battle, John; Bock, James J; Hristov, Viktor; Korngut, Philip; Meek, Andrew

    2015-01-01

    We report on the temporal and spatial fluctuations in the atmospheric brightness in the narrow band between Meinel emission lines at 1191.3 nm using an R=320 near-infrared instrument. We present the instrument design and implementation, followed by a detailed analysis of data taken over the course of a night from Table Mountain Observatory. The absolute sky brightness at this wavelength is found to be 5330 +/- 30 nW m^-2 sr^-1, consistent with previous measurements of the inter-band airglow at these wavelengths. This amplitude is larger than simple models of the continuum component of the airglow emission at these wavelengths, confirming that an extra emissive or scattering component is required to explain the observations. We perform a detailed investigation of the noise properties of the data and find no evidence for a noise component associated with temporal instability in the inter-line continuum. This result demonstrates that in several hours of ~100s integrations the noise performance of the instrument ...

  8. Statistical characteristics of gravity wave activities observed by an OH airglow imager at Xinglong, in northern China

    Directory of Open Access Journals (Sweden)

    Q. Li

    2011-08-01

    Full Text Available An all-sky airglow imager (ASAI was installed at Xinglong, in northern China (40.2° N, 117.4° E in November 2009 to study the morphology of atmospheric gravity waves (AGWs in the mesosphere and lower thermosphere (MLT region. Using one year of OH airglow imager data from December 2009 to November 2010, the characteristics of short-period AGWs are investigated and a yearlong AGW climatology in northern China is first ever reported. AGW occurrence frequency in summer and winter is higher than that in equinoctial months. Observed bands mainly have horizontal wavelengths from 10 to 35 km, observed periods from 4 to 14 min and observed horizontal phase speeds in the range of 30 to 60 m s−1. Most of the bands propagate in the meridional direction. The propagation directions of the bands show a strong southwestward preference in winter, while almost all bands propagate northeastward in summer. Although the wind filtering in the middle atmosphere may control AGW propagations in the zonal direction, the non-uniform distribution of wave sources in the lower atmosphere may contribute to the anisotropy in the meridional direction in different seasons. Additionally, as an indication of local instability, the characteristics of ripples are also analyzed. It also shows seasonal variations, occurring more often in summer and winter and mainly moving westward in summer and eastward in winter.

  9. Spatial and Temporal Stability of Airglow Measured in the Meinel Band Window at 1191.3 nm

    Science.gov (United States)

    Nguyen, Hien T.; Zemcov, Michael; Battle, John; Bock, James J.; Hristov, Viktor; Korngut, Phillip; Meek, Andrew

    2016-09-01

    We report on the temporal and spatial fluctuations in the atmospheric brightness in the narrow band between Meinel emission lines at 1191.3 nm using a λ/Δλ = 320 near-infrared instrument. We present the instrument design and implementation, followed by a detailed analysis of data taken over the course of a night from Table Mountain Observatory. At low airmasses, the absolute sky brightness at this wavelength is found to be 5330 ± 30 nW m-2 sr-1, consistent with previous measurements of the inter-band airglow at these wavelengths. This amplitude is larger than simple models of the continuum component of the airglow emission at these wavelengths, confirming that an extra emissive or scattering component is required to explain the observations. We perform a detailed investigation of the noise properties of the data and find no evidence for a noise component associated with temporal instability in the inter-line continuum. This result demonstrates that in several hours of ˜100 s integrations the noise performance of the instrument does not appear to significantly degrade from expectations, giving a proof of concept that near-infrared line intensity mapping may be feasible from ground-based sites.

  10. Atmospheric Gravity Wave Properties for TOMEX as Observed With Na wind/temperature Lidar and Airglow Instrumentation From Albuquerque, NM

    Science.gov (United States)

    Li, F.; Tang, J.; Liu, A.; Swenson, G.; Gardner, C.

    2002-12-01

    On the night of October 26, 2000, the TOMEX sounding rocket was launched from White Sands rocket range ~5 hours after sunset. Na lidar, airglow imagers, and a Michelson interferometer observed the perturbations in the mesosphere. In addition, the Na lidar measured the winds which were applied to the observed motion field from which intrinsic wave speeds were resolved. The extracted wave field from combined lidar and airglow observations included waves with periods of 5 hours, 1.5 hours, and 13 minutes present for the period leading to, and during the rocket launch. The vertical structures of the 13-minute and 1.5-hour period waves were determined primarily by the thermal structure, which was characterized by a small Brunt-Vaisala frequency between 90 km and 92 km with a strong gradient above and below. The 5-hour period waves exhibited a standing wave pattern, indicative of strong wave reflection in the mesopause region. In addition to the intrinsic wave parameters, the vertical flux of horizontal momentum and acceleration rate as a function of altitude was calculated for each of the waves. Momentum fluxes and accelerations were dominated by contributions from the 13-minute period waves.

  11. A Method of Inversing the Peak Density of Atomic Oxygen Vertical Distribution in the MLT Region From the OI (557.7nm) Night Airglow Intensity

    Institute of Scientific and Technical Information of China (English)

    H. Gao; J.Y. Xu; W. Yuan

    2005-01-01

    In this paper, using the MSISE-90 model as the reference atmosphere, we discuss the feasibility and method of deducing the peak densities of the undisturbed atomic oxygen profiles in the MLT region (the mesosphere and lower thermosphere region) from OI (557.7 nm) night airglow intersities. The peak densities for different seasons, latitudes and longitudes are deduced from OI (557.7nm) airglow intensities through this expression. We analyze the features of inversion relative errors and discuss the influence of the variations in temperature on inversion errors. The results indicate that all inversion errors are less than 5% except for those at high altitudes in the summer hemisphere. And the impact of the variations in temperature on errors is not significant.

  12. Preliminary observations and simulation of nocturnal variations of airglow temperature and emission rates at Pune (18.5°N), India

    Science.gov (United States)

    Fadnavis, S.; Feng, W.; Shepherd, Gordon G.; Plane, J. M. C.; Sonbawne, S.; Roy, Chaitri; Dhomse, S.; Ghude, S. D.

    2016-11-01

    Preliminary observations of the nocturnal variations of the OH(6-2) and O2b(0-1) nighttime airglow in the mesosphere and lower thermosphere are investigated in the context of tidal influence for the tropical latitude station Pune (18.5°N, 73.85°E). This is the only tropical Spectral Airglow Temperature Imager (SATI) station where the tidal variations of mesosphere and lower thermosphere (MLT) temperature have been determined from ground based SATI observations. The SATI observations obtained since October 2012 reveal the influence of the migrating semidiurnal tides during solstice at this tropical station. There is variability in amplitude and phase obtained from SATI observations. In this paper, SATI observations on 10 Dec 2012 and 3 March 2013 are compared with Whole Atmosphere Community Climate Model (WACCM) simulations. The amplitude of semidiurnal tides is ~25 K/30 K on 10 Dec 2012 during solstice for OH/O2 temperature. During equinox SATI data indicates existence of semidiurnal tide also. The airglow observations are compared with simulations from the WACCM. The model underestimates the amplitude of the semi diurnal tide during equinox (1.6 K/2.7 K at 87 km/96 km) and solstice (~3.8 K/4.8 K at 87 km/96 km) for these days. The reason may be related to dampening of tides in the model due to the effect of strong latitudinal shear in zonal wind. The diurnal variation of airglow emission - which the model simulates well - is related to the vertical advection associated with the tides and downward mixing of atomic oxygen.

  13. Relationship between propagation direction of gravity waves in OH and OI airglow images and VHF radar echo occurrence during the SEEK-2 campaign

    Directory of Open Access Journals (Sweden)

    F. Onoma

    2005-10-01

    Full Text Available We report simultaneous observations of atmospheric gravity waves (AGW in OI (557.7nm and OH airglow images and VHF radar backscatter from field-aligned irregularities (FAI in the E-region during the SEEK-2 (Sporadic-E Experiment over Kyushu 2 campaign period from 29 July to 9 August 2002. An all-sky imager was operated at Nishino-Omote (30.5 N, 130.1 E, Japan. On 14 nights, 17 AGW events were detected in OI and OH airglow images. AGW propagated mostly toward the northeast or southeast. From comparison with the E-region FAI occurrence, which is detected by a nearby VHF radar (31.57MHz, we found that AGW tended to propagate southeastward during FAI events. This result suggests that the interaction between AGW and E-region plasma plays an important role in generating FAI. Furthermore, polarization electric fields generated directly by AGW may contribute to the FAI generation.

    Keywords. Atmospheric composition and structure (Airglow and aurora, Ionosphere (Ionospheric irregularities, Mid-latitude ionosphere

  14. A method for the retrieval of atomic oxygen density and temperature profiles from ground-based measurements of the O(+)(2D-2P) 7320 A twilight airglow

    Science.gov (United States)

    Fennelly, J. A.; Torr, D. G.; Richards, P. G.; Torr, M. R.; Sharp, W. E.

    1991-01-01

    This paper describes a technique for extracting thermospheric profiles of the atomic-oxygen density and temperature, using ground-based measurements of the O(+)(2D-2P) doublet at 7320 and 7330 A in the twilight airglow. In this method, a local photochemical model is used to calculate the 7320-A intensity; the method also utilizes an iterative inversion procedure based on the Levenberg-Marquardt method described by Press et al. (1986). The results demonstrate that, if the measurements are only limited by errors due to Poisson noise, the altitude profiles of neutral temperature and atomic oxygen concentration can be determined accurately using currently available spectrometers.

  15. The N_2 c_4'-X (0,v") Airglow on Titan: What is Required to fit the UVS Observations?

    Science.gov (United States)

    Stevens, M. H.

    1999-09-01

    The N_2 Carroll-Yoshino (CY) c_4'(1Sigma_u ^+-X^1Sigma_g ^+) (0,0) and (0,1) Rydberg bands between 95 and 99 nm were observed to be the most prominent N_2 emission features in Voyager 1 Ultraviolet Spectrometer (UVS) airglow spectra of Titan. In order to study both the observed bright limb peak and the observed variation of CY(0,v") over the sunlit disk, a radiative transfer model is employed which considers both photoelectron excitation and magnetospheric particle precipitation. The resonant (0,0) band is known to be optically thick so multiple scattering and all known loss processes to the CY(0,v") system are included. Results show that only 23-33% of c_4'(0) source excitation appears in (0,0)+(0,1), primarily due to the effects of predissociation compounded over multiple scatterings. Such loss rules out photoelectrons as the only source and requires a flux of 1 keV magnetospheric electrons that is between 0.02-0.04 erg/cm(2) s to fit the disk observations. The relative variation of (0,0)+(0,1) over the sunlit disk can be explained by the variation of solar zenith angle (SZA) specific to each observation. Lower SZAs place photoelectron excitation at lower altitudes where (0,1) optical depths are greater, yielding less emission. The magnitude of the UVS bright limb peak can be accounted for with the same input fluxes, after taking into account the lower incidence angle of precipitating electrons.

  16. Rocket observation of atomic oxygen and night airglow: Measurement of concentration with an improved resonance fluorescence technique

    Directory of Open Access Journals (Sweden)

    K. Kita

    Full Text Available An improved resonant fluorescence instrument for measuring atomic oxygen concentration was developed to avoid the Doppler effect and the aerodynamic shock effect due to the supersonic motion of a rocket. The shock effect is reduced by adopting a sharp wedge-shaped housing and by scanning of the detector field of view to change the distance between the scattering volume and the surface of the housing. The scanning enables us to determine absolute values of atomic oxygen concentration from relative variation of the scattered light signal due to the self-absorption. The instrument was calibrated in the laboratory, and the numerical simulation reproduced the calibration result. Using the instrument, the altitude profile of atomic oxygen concentration was observed by a rocket experiment at Uchinoura (31°N on 28 January 1992. The data obtained from the rocket experiment were not perfectly free from the shock effect, but errors due to the effect were reduced by the data analysis procedure. The observed maximum concentration was 3.8× 1011 cm–3 at altitudes around 94 km. The systematic error is estimated to be less than ±0.7×1011 cm–3 and the relative random error is less than±0.07× 1011 cm–3at the same altitudes. The altitude profile of the OI 557.7-nm airglow was also observed in the same rocket experiment. The maximum volume emission rate was found to be 150 photons cm–3 s–1 at 94 km. The observed altitude profiles are compared with the MSIS model and other in situ observations.

  17. Long-term Trends in Mesospheric Temperatures at high and low latitudes derived from OH airglow spectra of Kiruna FTS and Sloan Digital Sky Survey

    Science.gov (United States)

    Kim, Yongha; Kim, Jeong-Han; Kim, Gawon; Lee, Youngsun

    2016-07-01

    We have analyzed mesospheric temperatures from OH airglow measurements with Fourier Transform Spectrometer (FTS) in the period of 2003 - 2012 at Kiruna (67.9°N, 21.1°E). We also derived mesospheric temperatures from rotational emission lines of the OH airglow (8-3) band in the sky spectra of Sloan Digital Sky Survey (SDSS) in the period of 2000 - 2014. The main objective of SDSS is to make a detailed 3-dimensional map of the universe by observing images and spectra of various celestial objects at Apache Point Observatory (APO, 32°N 105°W). From both temperature sets we first estimated the solar responses of mesospheric temperatures to F10.7 variation and the seasonal variation of mesospheric temperatures. After removing the solar response, we found the long-term mesospheric temperature trends of -4 ˜-6.6 K/decade at Kiruna and -0.02 ± 0.7 K/decade at Apache Point. Our results indicate significant cooling trend at the high latitude but very little or no cooling at the low latitude. Although both trends are comparable and consistent with other studies, the temperature trend from SDSS spectra should be regarded as unique contribution to global monitoring of climate change because the SDSS project is completely independent of climate studies.

  18. Observation of the June 22, 2015 G4 storm by HiT&MiS: an Echelle Spectrograph for Auroral and Airglow Studies

    Science.gov (United States)

    Aryal, S.; Hewawasam, K.; Maguire, R.; Chakrabarti, S.; Cook, T.; Martel, J.; Baumgardner, J. L.

    2015-12-01

    Observation of the June 22, 2015 G4 storm by HiT&MiS: an Echelle Spectrograph for Auroral and Airglow Studies Saurav Aryal1 , Kuravi Hewawasam1, Ryan Maguire1, Supriya Chakrabarti1, Timothy Cook1, Jason Martel1 and Jeffrey L Baumgardner2, (1) University of Massachusetts Lowell, Lowell, MA, United States, (2)Boston University, Boston, MA, United StatesA High-Throughput and Multi-slit Imaging Spectrograph (HiT&MIS) has been developed by our group. The spectrograph uses an echelle grating that operates at high dispersion orders (28-43) such that extended sources for airglow and auroral emissions can be observed at high resolution (about 0.02 nm). By using four slits (instead of the conventional one slit setup), with the appropriate foreoptics it images extended emissions along a long field of view of about 0.1° × 50°. It observes spectral regions around six prominent atmospheric emission lines (HI 656.3 nm, HI 486.1 nm, OI 557.7 nm, OI 630.0 nm, OI 777.4 nm and N+2 427.8 nm) using order sorting interference filters at the entrance slits and a filter mosaic on an image plane. We present observations from the instrument during the June 22, 2015 G4 storm. OI 557.7 nm (green line) and OI 630.0 nm (red line) showed strong brightness enhancements that lasted throughout the night from 8 P.M June 22, 2015 to 3 AM June 23,2015 when compared to the same times after the storm had passed.

  19. Interpretation of satellite airglow observations during the March 22, 1979, magnetic storm, using the coupled ionosphere-thermosphere model developed at University College, London

    Science.gov (United States)

    Parish, H. F.; Gladstone, G. R.; Chakrabarti, S.

    1994-01-01

    The University of California, Berkeley, extreme ultraviolet spectrometer aboard the U.S. Air Force STP 78-1 satellite measured emission features in the Earth's dayglow due to neutral and ionized species in the atmosphere, in the 35 to 140-nm range. The spectrometer was operating between March 1979 and March 1980, including the period of the magnetic storm on March 22, 1979. Some of these measurements are interpreted using the predictions of the three-dimensional time-dependent coupled ionosphere-thermosphere model developed at University College, London. The observations show a reduction in the atomic oxygen 130.4-nm airglow emission at high northern latitudes following the storm. Model simulations show that this reduction in 130.4-nm emission is associated with an increase in the O2/O ratio. Analysis of model results using electron transport and radiative transport codes show that the brightness of 130.4-nm emission at high latitudes due to resonantly scattered sunlight is approximately twice that due to photoelectron impact excitation. However, the observed decrease in the brightness at high northern latitudes is mainly due to a change in the photoelectron impact source, which contributes approximately 75% of the total, as well as its multiple scattering component; for the photoelectron impact source at 70 deg latitude and 200 km altitude, the reduction in multiple scattering is 1.5 times greater than the reduction in the initial excitation. The reduction in the airglow emission is visible only in the norther n hemisphere because the south pole was not sunlit over the storm period. The comparison of model results with observations suggests that 130.4-nm emission may be useful as a tracer for global changes in the concentration of atomic energy.

  20. Long-term ozone decline and its effect on night airglow intensity of Li 6708 Å at Varanasi (25°N, 83°E) and Halley Bay (76°S, 27°W)

    Indian Academy of Sciences (India)

    P K Jana; I Saha; S Mukhopadhyay

    2011-04-01

    A critical analysis has been made on the long-term yearly and seasonal variations of ozone concentration at Varanasi (25°N, 83°E), India and Halley Bay (76°S, 27°W), a British Antarctic Service Station. The effect of O3 depletion on night airglow emission of Li 6708 Å line at Varanasi and Halley Bay has been studied. Calculations based on chemical kinetics show that the airglow intensity of Li 6708 Å line has also been affected due to the depletion of O3 concentration. The yearly variations and seasonal variations of intensities of Li 6708 Å line for the above two stations are shown and compared. It has been shown that the rate of decrease of intensity of Li 6708 Å line was comparatively more at Halley Bay due to dramatic decrease of Antarctic O3 concentration.

  1. Ozone decline and its effect on night airglow intensity of Na 5893°A at Dumdum (22.5°N, 88.5° E) and Halley Bay (76°S, 27°W)

    Indian Academy of Sciences (India)

    P K Jana; S C Nandi

    2006-10-01

    The paper presents the effect of O3 depletion on night airglow emission of Na 5893 A line at Dumdum (22.5°N, 88.5°E), India and Halley Bay (76°S, 27°W), a British Antarctic service station. Calculations based on chemical kinetics show that the airglow intensity of Na 5893 A line will also be affected due to the depletion of O3 concentration. The nature of yearly variation and seasonal variation of the intensity of Na 5893 A line for the above two stations are shown and compared. It is shown that the rate of decrease of intensity of Na 5893 A line is comparatively more at Halley Bay due to the dramatic decrease of Antarctic O3 concentration. A possible explanation for this dramatic decrease of Antarctic O3 concentration is also mentioned.

  2. Mesopause temperatures calculated from the O2(a1Δg twilight airglow emission recorded at Maynooth (53.2°N, 6.4°W

    Directory of Open Access Journals (Sweden)

    J. M. Galligan

    Full Text Available Spectra of the O2(a1Δg airglow emission band at 1.27 µm have been recorded during twilight at Maynooth (53.2°N, 6.4°W using a Fourier transform spectrometer. Synthetic spectra have been generated for comparison with the recorded data by assuming a particular temperature at the emitting altitude, and modelling the absorption of each line in the band as it propagates downward through the atmosphere. The temperature used in generating the synthetic spectra was varied until an optimum fit was obtained between the recorded and synthetic data; this temperature was then attributed to the altitude of the emitting layer. Temperatures derived using this technique for 91 twilight periods over an 18-month period exhibit a strong seasonal behaviour with a maximum in winter and minimum in summer. Results from this study are compared with temperatures calculated from the OH(3, 1 Meinel band recorded simultaneously. In winter OH temperatures exceed O2 values by about 10 K, whereas the opposite situation pertains in summer; this result is interpreted in terms of a possible change in the altitude of the mesopause as a function of season. Estimates of the twilight O2(0, 0 total band intensity indicate that its intensity is lower and that its decay is more rapid in summer than in winter, in agreement with earlier observations.

  3. Implementation of a High-Altitude Balloon Payload to Study Thermospheric Wind Speeds through Redline Airglow Emissions of Atomic Oxygen at 630 nm via a Split-field Etalon Doppler Imager Utilizing a Fabry-Perot Interferometer.

    Science.gov (United States)

    Terry, L. B.; Fullmer, R.; Swenson, C.; Marchant, A.; Hooser, P.; Victors, J.; Muchmore, K.; Yin, L.

    2015-12-01

    Little data exists on the wind velocity characteristics of the upper atmosphere. The Red Line Air Glow Experiment is designed to measure the relative density and velocity of the thermosphere at altitudes approximately ranging between 250 and 350 km. To accomplish this, a Split-Field Etalon Imager will make doppler shift interferometry measurements of the oxygen redline at 630 nm wavelength airglow a using a high altitude balloon platform floating at 36 km. The imager collects up to 10 images per hour. Velocity resolution is within a 5 m/s. The Etalon is thermally controlled to within 1 deg C to achieve this goal. The pointing direction of the sensor is determined post-filght using GPS, IMU and three sun imaging sensors. An experimental star camera is included with a potential pointing accuracy of under 5 arc-min. The instrument first flew from Fort Sumner N,M., on August 26, 2014. Due to the short duration (3.5 hours) of the data collection period on this flight, a second flight was requested and awarded, to take place around September 10, 2015. This flight will allow for data collection over a 24 hour period. Both flight results will be included in the final presentation. This project was designed and built by an undergraduate team including students from physics, aerospace, electrical and mechanical engineering and management at both Utah State University and the University of Maryland Eastern Shores as a NASA's Undergraduate Student Instrument Project (USIP).

  4. On applicability of the photochemical-equilibrium approach for retrieval of O and H mesospheric distributions from the satellite-based measurements of the airglow emission and ozone concentration

    Science.gov (United States)

    Feigin, Alexander; Belikovich, Mikhail; Kulikov, Mikhail

    2016-04-01

    Atomic oxygen and hydrogen are known to be among key components for the photochemistry and energy balance of the Earth's atmosphere between approximately 80 and 100 km altitude (mesopause region). Therefore, obtaining information about the vertical distributions of O and H concentrations is an important task in studies of this region. Solving of this problem is rather difficult due to the absence of regular methods which allow one to direct measurements of distributions of these components in mesosphere. However, indirect methods used to retrieve O and H distributions from the satellite-based measurements of the OH and O2(1D) airglow emission, as well as the data of IR and microwave O3 measurements have a sufficiently long development history. These methods are rooted in the use of the condition of photochemical equilibrium of ozone density in the range of altitudes from 50 to 100 km. A significant factor is that an insufficient volume of such measurement data forces researchers to use approximate ("truncated") photochemical-equilibrium conditions. In particular, it is assumed that in the daytime the ozone production reaction is perfectly balanced by ozone photodissociation, whereas during the night the only ozone sink is the reaction of ozone with atomic hydrogen, which, in its turn, leads to formation of excited OH and airglow emission of the latter. The presentation analyzes applicability of the photochemical-equilibrium conditions both in the total and truncated forms for description of the spatio-temporal evolution of mesospheric ozone during a year. The analysis is based on year-long time series generated by a 3D chemical transport model, which reproduces correctly various types of atmosphere dynamics in the range of altitudes from 50 to 100 km. These data are used to determine statistics of the ratio between the correct (calculated dynamically) distributions of the O3 density and its uncontracted and truncated equilibrium values for the conditions of the

  5. Yearly variation and annual cycle of total column ozone over New Delhi (29°N, 77°E), India and Halley Bay (76°S, 27°W), British Antarctic Survey Station and its effect on night airglow intensity of OH(8, 3) for the period 1979–2005

    Indian Academy of Sciences (India)

    P K Jana; D K Saha; D Sarkar

    2012-12-01

    A critical analysis made on the long-term monthly, seasonal, yearly variation and annual cycle of total column ozone (TCO) concentration at New Delhi (29°N,77°E), India and Halley Bay (76°S, 27°W), a British Antarctic Service Station reveals more decline in yearly mean ozone concentration at Halley Bay than at New Delhi from 1979 to 2005. The nature of variations of monthly mean TCO during the months of August and September was the most identical with that of yearly mean ozone values at New Delhi and Halley Bay, respectively, for the same period. Annual cycles of TCO over these stations are completely different for the above period. The effect of O3 depletion on night airglow emission of OH(8, 3) line at New Delhi and Halley Bay has been studied. Calculations based on chemical kinetics show that the airglow intensity of OH(8, 3) has also been affected due to the depletion of O3 concentration. The yearly variations and annual cycle of intensities of OH(8, 3) line for the above two stations are depicted and compared. It has been shown that the rate of decrease of intensity of OH(8, 3) line was comparatively more at Halley Bay due to dramatic decrease of Antarctic O3 concentration.

  6. SWIR Hemispherical Air-Glow Plotting System SHAPS: Postprint

    Science.gov (United States)

    2010-06-01

    atmosphere, as modeled using the van Rhijn method (4). 60.-~-----~--~- -- 200 10 °07--0~5~~--~15~~-725~ .-3 15 4.5 T.mo (hour!.) Ttm ~ (hou’!!.) a...temporal variations in the irradiance, both short and long term, can be used to validate and calibrate physical models of atmospheric chemistry and...spatio- temporal variations in the irradiance. both short and long term. can be used to validate and calibrate physical models of atmospheric

  7. High Resolution Measurements of OH Infrared Airglow Structure.

    Science.gov (United States)

    1985-01-01

    1-2. Interaction of off-axis rays in a conventional Michelson interferometer ESteed 1978. ...... ................ 11 1-3. Isocon camera system...axis rays in conventionalL Michelson intorfwromotor ESteed 19783. 3 .’-+."...v’.. WAVE.....FRONT. h "%’"’"..~- .4 12 of field-widening or optical...with a self - contained preamplifier and load resistor in a liquid- nitrogen dewar. Figure 2-7 is a picture of the detector dewar. The detector is 5 mm in

  8. High-Resolution Measurement of OH Infrared Airglow Structure.

    Science.gov (United States)

    1985-10-18

    Interaction of off-axis rays In a conventional Michelson interferometer ESteed 197832................. 11 1-3. Isocon camera system spectral range...had proven effective in the past. The detector selected was an RCA Ltd., solid state germanium device with a self - contained preamplifier and load

  9. Allsky Airglow Imagery from Albuquerque, NM; TOMEX 2000

    Science.gov (United States)

    Swenson, G. R.

    2001-12-01

    Allsky imager of OH Meinel and O2 Atmospheric emission bands were observed for the TOMEX rocket campaign from Albuquerque, NM, along with the Na/wind temperature lidar. Motion analysis of imagery describes a main wave propagating from the NW but other secondary waves appear from the NE to present a quasi chaotic wave field. The main wave had a typical horizontal wavelength of a several 10s of km and a period of less than15 minutes. The instrinsic wave parameters of the high frequency waves will be presented.

  10. Advances in remote sensing of the daytime ionosphere with EUV airglow

    Science.gov (United States)

    Stephan, Andrew W.

    2016-09-01

    This paper summarizes recent progress in developing a method for characterizing the daytime ionosphere from limb profile measurements of the OII 83.4 nm emission. This extreme ultraviolet emission is created by solar photoionization of atomic oxygen in the lower thermosphere and is resonantly scattered by O+ in the ionosphere. The brightness and shape of the measured altitude profile thus depend on both the photoionization source in the lower thermosphere and the ionospheric densities that determine the resonant scattering contribution. This technique has greatly matured over the past decade due to measurements by the series of Naval Research Laboratory Special Sensor Ultraviolet Limb Imager (SSULI) instruments flown on Defense Meteorological Satellite Program (DMSP) missions and the Remote Atmospheric and Ionospheric Detection System (RAIDS) on the International Space Station. The volume of data from these missions has enabled a better approach to handling specific biases and uncertainties in both the measurement and retrieval process that affect the accuracy of the result. This paper identifies the key measurement and data quality factors that will enable the continued evolution of this technique into an advanced method for characterization of the daytime ionosphere.

  11. Spatial and temporal behavior of atomic oxygen determined by Ogo 6 airglow observations

    Science.gov (United States)

    Donahue, T. M.; Guenther, B.; Thomas, R. J.

    1974-01-01

    Maps are produced of the atomic oxygen density near 97 km showing a strong variation in latitude, longitude, universal time, and time of year. These densities are deduced from atomic oxygen green nightglow observations carried out from Ogo 6. Meridional wind patterns needed to support the asymmetries observed in local oxygen production and loss rates are deduced.

  12. Spatial Characteristics of Airglow and Solar Scatter Radiance from the Earth’s Atmosphere

    Science.gov (United States)

    1989-08-09

    AD-A2I 1 358 REPORT DOCUMENTATION PAGEIn W.."ariLA11ON AUTHO^ E E T3.DSW TINARNUYO110 1 Jb, DECLASSIFICATION I DOWNORALII Aproe for publiot role... REPORT _11b. TIME COVERED 14. DATE OF REPORT (Yea.Month.OayJ 11S. PAGE COUNT Reprint FROM TO I___ 19A9 A~tigt, 9 1) 16. SUPPLEMENTARY NOTATION...Huguenin, R. Wohlers and M. Weinberg Aerodyne Research, Inc. 45 Manning Road Billerica, HA 01821 and R. Huffman, R. Eastes, and F. Delgreco Air Force

  13. Spatial characteristics of airglow and solar-scatter radiance from the earth's atmosphere

    Energy Technology Data Exchange (ETDEWEB)

    Huguenin, R.; Wohlers, R.; Weinberg, M.; Huffman, R.; Eastes, R.

    1989-08-09

    Data measured by the Polar BEAR/AIRS UV Experiment were processed to extract spatial-radiance characteristics. Photometer-mode 1304A dayside data measured on Julian Day 219, 1987, near mid-day were analyzed. The spatial structure of thermospheric dayside radiance at 1304A appeared to be controlled principally by turbulence over spatial scales of 10 million - 100 meters, with modifications imposed by Rayleigh-scattering effects and magnetospherically forced phenomena. Spatial structure can be adequately modeled fractally, using dimensions based on Kolmogorov formalism modified by the Rayleigh scattering phase function. Mean radiance can be modeled using existing models of radiant intensity, resonance scattering, and absorption combined with thermospheric composition and general circulation models, such as MSIS-83, scaled to the mean and RHS intensities measured by Polar BEAR. The results can be incorporated in a background radiance simulation model that will provide a means for testing and refining phenomenological models of the structured earth background. This will be important not only for improving physical and chemical models of atmospheric features and processes, but it will allow parametric predictions of spatial structure and clutter to be developed for sensor applications.

  14. Polar Bear UV Imaging of Airglow and Aurora - Image Processing and Results

    Science.gov (United States)

    1989-09-24

    in time) over the first half year of Polar BEAR’s life in 12 orbit by plotting a few dosen panes randomly chosen from that era. Figure 5 shows the...intend to expand our processing in the future to include dosens of images in each map. Thus this point, at least regarding the statistical validity of

  15. Dissociative recombination of atmospheric ions : towards unravelling the physics behind airglows

    NARCIS (Netherlands)

    Petrignani, Annemieke

    2005-01-01

    This thesis presents experimental data on the dissociative recombination reaction between electrons and the molecular ions, oxygen, nitric oxide, and nitric-oxide-dimers, as well as a computational study of the reaction. The presented research is performed in the context of aeronomy. The products of

  16. Airglow and magnetic field disturbances over Brazilian region during Chile tsunami (2015)

    CERN Document Server

    Klausner, V; Candido, C M N; Abalde, J R; Fagundes, P R; Kherani, E A

    2015-01-01

    In this work, we present first report on disturbances over Brazilian atmosphere on 16--17 September, 2015 following the Chile tsunami occurrence. Using all-sky imager and magnetometer located at 2330 km away from the epicenter, the presence of disturbances is noted 1--3 hours after the tsunami beginning time and during time which seismic tremor was also felt in the region. We argue that their presence towards continent at 2000-3000 km away from the epicenter offers another example of similar atmospheric response as those observed during Tohoku-Oki tsunami, 2011. This similarity and their appearance during seismic tremor over the region classify them to be of tsunamigenic and/or seismogenic nature.

  17. Spectral wave analysis at the mesopause from SCIAMACHY airglow data compared to SABER temperature spectra

    Directory of Open Access Journals (Sweden)

    M. Ern

    2009-01-01

    Full Text Available Space-time spectral analysis of satellite data is an important method to derive a synoptic picture of the atmosphere from measurements sampled asynoptically by satellite instruments. In addition, it serves as a powerful tool to identify and separate different wave modes in the atmospheric data. In our work we present space-time spectral analyses of chemical heating rates derived from Scanning Imaging Absorption SpectroMeter for Atmospheric CHartographY (SCIAMACHY hydroxyl nightglow emission measurements onboard Envisat for the years 2002–2006 at mesopause heights.

    Since SCIAMACHY nightglow hydroxyl emission measurements are restricted to the ascending (nighttime part of the satellite orbit, our analysis also includes temperature spectra derived from 15 μm CO2 emissions measured by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER instrument. SABER offers better temporal and spatial coverage (daytime and night-time values of temperature and a more regular sampling grid. Therefore SABER spectra also contain information about higher frequency waves.

    Comparison of SCIAMACHY and SABER results shows that SCIAMACHY, in spite of its observational restrictions, provides valuable information on most of the wave modes present in the mesopause region. The main differences between wave spectra obtained from these sensors can be attributed to the differences in their sampling patterns.

  18. Medium-Scale Traveling Ionospheric Disturbances and Plasma Bubbles Observed by an All-Sky Airglow Imager at Yonaguni, Japan

    Directory of Open Access Journals (Sweden)

    Tadahiko Ogawa

    2009-01-01

    Full Text Available We report on night time air glow imaging observations of the low latitude ionosphere by means of a 630-m all-sky imager in stalled in March 2006 at Yonaguni, Japan _ _ _ geomagnetic, about 100 km east of Taiwan. The imager detected medium-scale traveling ionospheric disturbances (MSTIDs for about 7 hours on the night of 26 May 2006. A dense GPS net work in Japan also ob served the same MSTID event on this night. The imager and GEONET data indicate that most of the MSTIDs prop a gated south west ward from the north of Japan to the south of Yonaguni and Taiwan over 4000 km, with a southern limit of _ (geomagnetic latitude _ or lower. On the night of 10 November 2006, the imager observed two weak emission bands that were embedded on the F-region anomaly crest to the south of Yonaguni. The simultaneous electron density profiles from the FORMOSAT-3/COS MIC mission demonstrate that the weak emission bands are due to density depletions in equatorial plasma bubbles. These case studies suggest that the Yonaguni imager in collaboration with other instruments is very suit able for the study of ionospheric disturbances in and around the northern F-region anomaly crest.

  19. Medium-Scale Traveling Ionospheric Disturbances and Plasma Bubbles Observed by an All-Sky Airglow Imager at Yonaguni, Japan

    Directory of Open Access Journals (Sweden)

    Tadahiko Ogawa

    2009-01-01

    Full Text Available We report on night time air glow imaging observations of the low latitude ionosphere by means of a 630-m all-sky imager in stalled in March 2006 at Yonaguni, Japan (24.5°N, 123.0°E; 14.6°N geomagnetic, about 100 km east of Taiwan. The imager detected medium-scale traveling ionospheric disturbances (MSTIDs for about 7 hours on the night of 26 May 2006. A dense GPS net work in Japan also ob served the same MSTID event on this night. The imager and GEONET data indicate that most of the MSTIDs prop a gated south west ward from the north of Japan to the south of Yonaguni and Taiwan over 4000 km, with a southern limit of 19°N (geomagnetic latitude 9°N or lower. On the night of 10 November 2006, the imager observed two weak emission bands that were embedded on the F-region anomaly crest to the south of Yonaguni. The simultaneous electron density profiles from the FORMOSAT-3/COS MIC mission demonstrate that the weak emission bands are due to density depletions in equatorial plasma bubbles. These case studies suggest that the Yonaguni imager in collaboration with other instruments is very suit able for the study of ionospheric disturbances in and around the northern F-region anomaly crest.

  20. Evaluation of Ionospheric Densities Using Coincident OII 83.4 nm Airglow and the Millstone Hill Radar

    CERN Document Server

    Douglas, Ewan S; Stephan, Andrew W; Cashman, Lauren; Bishop, Rebecca L; Budzien, Scott A; Christensen, Andrew B; Hecht, James H; Chakrabarti, Supriya

    2016-01-01

    We test the utility of the OII 83.4 nm emission feature as a measure of ionospheric parameters. Observed with the Remote Atmospheric and Ionospheric Detection System (RAIDS) Extreme Ultraviolet Spectrograph on the International Space Station (ISS), limb profiles of 83.4 nm emissions are compared to predicted dayglow emission profiles from a theoretical model incorporating ground-based electron density profiles measured by the Millstone Hill radar and parameterized by a best-fit Chapman-{\\alpha} function. Observations and models are compared for periods of conjunction between Millstone Hill and the RAIDS fields-of-view. These RAIDS observations show distinct differences in topside morphology between two days, 15 January and 10 March 2010, closely matching the forward model morphology and demonstrating that 83.4 nm emission is sensitive to changes in the ionospheric density profile from the 340 km altitude of the ISS during solar minimum. We find no significant difference between 83.4 nm emission profiles model...

  1. MEx/SPICAM Dayside Exospheric Temperatures Derived from Airglow Emissions and Comparisons with Global Model Simulations: Do We Understand the Variations?

    Science.gov (United States)

    Bougher, S. W.; Stiepen, A.; Gerard, J. M.; Pawlowski, D. J.; Montmessin, F.

    2013-12-01

    For ten years now, the SPectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (SPICAM) instrument on board Mars Express has collected tangential limb dayglow observations of the CO Cameron bands (170-270 nm) and the CO2+ doublet emission lines (289 nm). The CO2+ emission arises from the relaxation of the CO2+* molecule in the B2Σ+ state to the X2Π state. The CO Cameron emissions arise from the forbidden transition between CO in the exited a3 Π triplet state to the ground (X1Σ+) state. CO2+*and CO* molecules are mainly produced in the Martian dayside through photoionization and photoelectron impact. The temperature of the neutral thermosphere-exosphere region of the Martian atmosphere (above 150 km) has been derived from the top scale height of these emission vertical profiles. The database contains temperatures obtained from observations that cover all latitudes, seasons, dayside solar zenith angles, etc. for solar minimum to moderate conditions. A search for the key factors that influence the temperature in this region of the Martian atmosphere is presented. In addition, 3-D global model simulations are conducted appropriate to these SPICAM sampling conditions. Comparisons among Mars Thermosphere General Circulation Model (MTGCM), Mars Global Ionosphere Thermosphere Model (MGITM), and SPICAM derived temperatures are made. The capability of these solar EUV controlled 3-D models to reproduce observed dayside temperatures is discussed.

  2. Extensive MRO CRISM Observations of 1.27 micron O2 Airglow in Mars Polar Night and Their Comparison to MRO MCS Temperature Profiles and LMD GCM Simulations

    Science.gov (United States)

    Clancy, R. Todd; Sandor, Brad J.; Wolff, Michael J.; Smith, Michael Doyle; Lefevre, Franck; Madeleine, Jean-Baptiste; Forget, Francois; Murchie, Scott L.; Seelos, Frank P.; Seelos, Kim D.; Nair, Hari A.; Toigo, Anthony D.; Humm, David; Kass, David M.; Kleinbahl, Armin; Heavens, Nicholas

    2012-01-01

    The Martian polar night distribution of 1.27 micron (0-0) band emission from O2 singlet delta [O2(1Delta(sub g))] is determined from an extensive set of Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectral Mapping (CRISM) limb scans observed over a wide range of Mars seasons, high latitudes, local times, and longitudes between 2009 and 2011. This polar nightglow reflects meridional transport and winter polar descent of atomic oxygen produced from CO2 photodissociation. A distinct peak in 1.27 micron nightglow appears prominently over 70-90NS latitudes at 40-60 km altitudes, as retrieved for over 100 vertical profiles of O2(1Delta(sub g)) 1.27 micron volume emission rates (VER). We also present the first detection of much (x80+/-20) weaker 1.58 micron (0-1) band emission from Mars O2(1Delta(sub g)). Co-located polar night CRISM O2(1Delta(sub g)) and Mars Climate Sounder (MCS) (McCleese et al., 2008) temperature profiles are compared to the same profiles as simulated by the Laboratoire de Météorologie Dynamique (LMD) general circulation/photochemical model (e.g., Lefèvre et al., 2004). Both standard and interactive aerosol LMD simulations (Madeleine et al., 2011a) underproduce CRISM O2(1Delta(sub g)) total emission rates by 40%, due to inadequate transport of atomic oxygen to the winter polar emission regions. Incorporation of interactive cloud radiative forcing on the global circulation leads to distinct but insufficient improvements in modeled polar O2(1Delta(sub g)) and temperatures. The observed and modeled anti-correlations between temperatures and 1.27 mm band VER reflect the temperature dependence of the rate coefficient for O2(1Delta(sub g)) formation, as provided in Roble (1995).

  3. Degradation of near infrared and shortwave infrared imager performance due to atmospheric scattering of diffuse night illumination.

    Science.gov (United States)

    Vollmerhausen, Richard

    2013-07-20

    On moonless nights, airglow is the primary source of natural ground illumination in the near infrared and shortwave infrared spectral bands. Therefore, night vision imagers operating in these spectral bands view targets that are diffusely illuminated. Aerosol scattering of diffuse airglow illumination causes atmospheric path radiance and that radiance causes increased imager noise. These phenomena and their quantification are described in this paper.

  4. Atmospheric gravity waves due to the Tohoku-Oki tsunami observed in the thermosphere by GOCE

    NARCIS (Netherlands)

    Garcia, R.F.; Doornbos, E.N.; Bruinsma, S.; Hebert, H.

    2014-01-01

    Oceanic tsunami waves couple with atmospheric gravity waves, as previously observed through ionospheric and airglow perturbations. Aerodynamic velocities and density variations are computed from Gravity Field and Steady-State Ocean Circulation Explorer (GOCE) accelerometer and thruster data during T

  5. Chapman Solar Zenith Angle variations at Titan

    Science.gov (United States)

    Royer, Emilie M.; Ajello, Joseph; Holsclaw, Gregory; West, Robert; Esposito, Larry W.; Bradley, Eric Todd

    2016-10-01

    Solar XUV photons and magnetospheric particles are the two main sources contributing to the airglow in the Titan's upper atmosphere. We are focusing here on the solar XUV photons and how they influence the airglow intensity. The Cassini-UVIS observations analyzed in this study consist each in a partial scan of Titan, while the center of the detector stays approximately at the same location on Titan's disk. We used observations from 2008 to 2012, which allow for a wide range of Solar Zenith Angle (SZA). Spectra from 800 km to 1200 km of altitude have been corrected from the solar spectrum using TIMED/SEE data. We observe that the airglow intensity varies as a function of the SZA and follows a Chapman curve. Three SZA regions are identified: the sunlit region ranging from 0 to 50 degrees. In this region, the intensity of the airglow increases, while the SZA decreases. Between SZA 50 and 100 degrees, the airglow intensity decreases from it maximum to its minimum. In this transition region the upper atmosphere of Titan changes from being totally sunlit to being in the shadow of the moon. For SZA 100 to 180 degrees, we observe a constant airglow intensity close to zero. The behavior of the airglow is also similar to the behavior of the electron density as a function of the SZA as observed by Ågren at al (2009). Both variables exhibit a decrease intensity with increasing SZA. The goal of this study is to understand such correlation. We demonstrate the importance of the solar XUV photons contribution to the Titan airglow and prove that the strongest contribution to the Titan dayglow occurs by solar fluorescence rather than the particle impact that predominates at night.

  6. The Auroral Station in Adventdalen, Svalbard

    Institute of Scientific and Technical Information of China (English)

    2002-01-01

    This paper describes the Auroral Station in Adventdalen near Longyearbyen, Svalbard (78°N, 15°E). The main instruments at the site are for optical observation of aurora and airglow, but magnetic and radar observations are also carried out. Emission spectra show the difference between the dayside and nightside optical aurora. A newly compiled mesospheric temperature series from the station is also presented, derived through 20 years of spectral measurements of the hydroxyl airglow layer.

  7. Plan to develop predictive capability for equatorial scintillation storms. Semi-annual report, 1 July-31 December 1996

    Energy Technology Data Exchange (ETDEWEB)

    Mendillo, M.; Aarons, J.

    1997-01-27

    To begin the assembly of a coordinated, multiparameter data base suitable for testing various approaches to prediction the team went to Tucuman, Argentina and set up an airglow imaging system to record the 6300 A airglow depletions that mark the boundaries of low latitude irregularity patterns. A successful series of measurements were made during the campaign. Optical observations at Arequipa, Peru were made. The data are being reduced as of this time with interesting comparisons of phase and amplitude scintillation with optical and radar data. Localized differences are considerable so that on some days the occurrence of scintillation was different for stations 500 km apart.

  8. Inter-hemispheric Comparison of Mesospheric Short-period Gravity Wave Propagation

    Science.gov (United States)

    Nielsen, K.; Taylor, M. J.; Collins, R. L.; Irving, B. K.; Negale, M.; Siskind, D. E.; Eckermann, S. D.; Hoppel, K.; Harvey, V.; Russell, J. M.

    2011-12-01

    Mesospheric short-period (≤1-hr) gravity waves are of great importance for dynamics in the mesosphere-lower thermosphere (MLT) region, and are typically measured by instruments capable of high temporal and/or spatial resolutions such as lidars and airglow imagers. These waves have been studied extensively at low- and mid-latitudes where known wave sources are well established. The results show strong dependence on the background wind and temperature fields, which can act as a barrier prohibiting vertical propagation of the waves, as well as providing a ducted environment in which the waves can travel large horizontal distances. In fact, results show that up to 75% of these waves may exhibit ducted wave motion. Recent airglow imaging measurements over Antarctica have revealed a large number of short-period gravity waves in absence of the prominent wave sources present at lower latitudes. In contrast to results at lower latitudes, very few waves (˜5%) observed over Halley (76°S) exhibited Doppler ducted motion. In this work, we utilize airglow imagery, SABER temperature measurements, together with the Navy's high-altitude numerical weather prediction system, NOGAPS-ALPHA, to investigate propagation conditions (particularly, the role of thermal ducting) over Rothera (68°S). Data acquired from a newly installed airglow imager operating at Poker Flat, Alaska (65°N) and the co-located lidar provide an opportunity to perform an inter-hemispheric comparison of propagation conditions over two polar sites at similar latitudes.

  9. Solar and chemical reaction-induced heating in the terrestrial mesosphere and lower thermosphere

    Science.gov (United States)

    Mlynczak, Martin G.

    1992-01-01

    Airglow and chemical processes in the terrestrial mesosphere and lower thermosphere are reviewed, and initial parameterizations of the processes applicable to multidimensional models are presented. The basic processes by which absorbed solar energy participates in middle atmosphere energetics for absorption events in which photolysis occurs are illustrated. An approach that permits the heating processes to be incorporated in numerical models is presented.

  10. Skycorr: A general tool for spectroscopic sky subtraction

    CERN Document Server

    Noll, S; Kimeswenger, S; Barden, M; Jones, A M; Modigliani, A; Szyszka, C; Taylor, J

    2014-01-01

    Airglow emission lines, which dominate the optical-to-near-IR sky radiation, show strong, line-dependent variability on various time scales. Therefore, the subtraction of the sky background in the affected wavelength regime becomes a problem if plain sky spectra have to be taken at a different time as the astronomical data. A solution of this issue is the physically motivated scaling of the airglow lines in the plain sky data to fit the sky lines in the object spectrum. We have developed a corresponding instrument-independent approach based on one-dimensional spectra. Our code skycorr separates sky lines and sky/object continuum by an iterative approach involving a line finder and airglow line data. The sky lines are grouped according to their expected variability. The line groups in the sky data are then scaled to fit the sky in the science data. Required pixel-specific weights for overlapping groups are taken from a comprehensive airglow model. Deviations in the wavelength calibration are corrected by fitti...

  11. Study of mid-latitude 5577A CI dayglow emissions. Doctoral thesis

    Energy Technology Data Exchange (ETDEWEB)

    Hume, E.E.

    1992-01-01

    Summary of thesis: The green line (5577angstroms) is a bright, persistent component of the visible airglow. It is produced by an electric quadruple transition from the metastable second excited state (1So) to the first excited state (1D2) of atomic oxygen. These two excited states all lie in the same electron shell of the atom and have the same electron configuration as the ground state of 1s22s22p4, which is the 3P2,1,0. This emission is present in both the daytime and night airglow and in the aurora, and despite a long history of study it is still not fully understood. The emission in the dayglow and the nightglow is relatively homogeneous spatially and global in coverage. In the aurora, the emission is much brighter than the airglow, high structured and very localized being restricted to higher latitudes. The structure of the 5577angstroms emission with altitude and the chemistry responsible for the production of the emission are complex. The vertical structure for the emission has two distinct layers in the airglow each with its own set of production and loss mechanisms. the chemistry for either of these layers is not completely known. The auroral emission is not understood either since it overlaps the upper and lower layer altitudes and it tends to contain some parts of the chemistry of both layers as sources and losses.

  12. Fabrication and performance of intrinsic germanium photodiodes. [for atmospheric IR spectroscopy

    Science.gov (United States)

    Beiting, E. J., III; Feldman, P. D.

    1977-01-01

    The paper presents fabrication details for an intrinsic germanium photodiode developed for study of atmospheric constituents, the airglow and auroras in the 1-2 micron spectral range. Attention is given to cutting of the single crystal, spreading of the lithium dispersion, sputtering of a gold coating, and surface passivation. A wavelength response curve is presented.

  13. Orbital Sunrise

    Science.gov (United States)

    1994-01-01

    The STS-68 crew aboard the Space Shuttle Endeavour told a post-flight audience at JSC that this sunrise was one of the most scenic sunrises/ sunsets witnessed during the week and a half long Space Radar Laboratory (SRL-2) mission. Jutting clouds, back-lit by the dawn colors, are sandwiched between the blue airglow and the silhouetted horizon of Earth.

  14. A Multi-Instrument Measurement of a Mesospheric Bore at the Equator

    Science.gov (United States)

    Shiokawa, K.; Suzuki, S.; Otsuka, Y.; Ogawa, T.; Nakamura, T.; Mlynczak, M. G.; Russell, J. M., III

    2005-01-01

    We have made a comprehensive measurement of mesospheric bore phenomenon at the equator at Kototabang, Indonesia (0.2 deg S, 100.3 deg E), using an airglow imager, an airglow temperature photometer, a meteor radar, and the SABER instrument on board the TIMED satellite. The bore was detected in airglow images of both OH-band (peak emission altitude: 87 km) and 557.7-nm (96 km) emissions, as east-west front-like structure propagating northward with a velocity of 52-58 m/s. Wave trains with a horizontal wavelength of 30-70 km are observed behind the bore front. The airglow intensity decreases for all the mesospheric emissions of OI (557.7 nm), OH-band, O2-band (altitude: 94 km), and Na (589.3 nm) (90 km) after the bore passage. The rotational temperatures of both OH-band and O2-band also decrease approximately 10 K after the bore passage. An intense shear in northward wind velocity of 80m/s was observed at altitudes of 84-90 km by the meteor radar. Kinetic temperature profile at altitudes of 20-120 km was observed near Kototabang by TIMED/SABER. On the basis of these observations, we discuss generation and ducting of the observed mesospheric bore.

  15. Transparency of the Atmosphere to Short Horizontal Wavelength Gravity Waves

    Science.gov (United States)

    2008-12-16

    Suzuki, S., K. Shiokawa , Y. Otsuka, T. Ogawa, K. Nakamura, and T. Nakamura (2007a), A concentric gravity wave structure in the meso- spheric airglow images...J. Geophys. Res., 112, D02102, doi:10.1029/ 2005JD006558. Suzuki, S., K. Shiokawa , Y. Otsuka, T. Ogawa, M. Kubota, M. Tsutsumi, T. Nakamura, and D

  16. On the backscatter of solar He II, 304 A radiation from interplanetary He/+/.

    Science.gov (United States)

    Paresce, F.; Bowyer, S.

    1973-01-01

    Backscatter of solar He II, 304 A radiation by interplanetary positive helium ions is shown to be insufficient to account for recent observations of this airglow radiation in the night sky at rocket altitudes. In fact, for most viewing directions, the expected intensities probably fall well below the sensitivity threshold of existing extreme ultraviolet instrumentation.

  17. WAMDII: The Wide Angle Michelson Doppler Imaging Interferometer

    Science.gov (United States)

    1992-01-01

    As part of an effort to learn more about the upper atmosphere and how it is linked to the weather experienced each day, NASA and NRCC are jointly sponsoring the Wide Angle Michelson Doppler Imaging Interferometer (WAMDII) Mission. WAMDII will measure atmospheric temperature and wind speed in the upper atmosphere. In addition to providing data on the upper atmosphere, the wind speed and temperature readings WAMDII takes will also be highly useful in developing and updating computer simulated models of the upper atmosphere. These models are used in the design and testing of equipment and software for Shuttles, satellites, and reentry vehicles. In making its wind speed and temperature measurements, WAMDII examines the Earth's airglow, a faint photochemical luminescence caused by the influx of solar ultraviolet energy into the upper atmosphere. During periods of high solar flare activity, the amount of this UV energy entering the upper atmosphere increases, and this increase may effect airglow emissions.

  18. Observation of mesospheric gravity waves at Comandante Ferraz Antarctica Station (62° S

    Directory of Open Access Journals (Sweden)

    P. B. Souza

    2009-06-01

    Full Text Available An airglow all-sky imager was operated at Comandante Ferraz Antarctica Station (62.1° S, 58.4° W, between April and October of 2007. Mesospheric gravity waves were observed using the OH airglow layer during 43 nights with good weather conditions. The waves presented horizontal wavelengths between 10 and 60 km and observed periods mainly distributed between 5 and 20 min. The observed phase speeds range between 5 m/s and 115 m/s; the majority of the wave velocities were between 10 and 60 m/s. The waves showed a preferential propagation direction towards the southwest in winter (May to July, while during spring (August to October there was an anisotropy with a preferential propagation direction towards the northwest. Unusual mesospheric fronts were also observed. The most probable wave source could be associated to orographic forcing, cold fronts or strong cyclonic activity in the Antarctica Peninsula.

  19. Aeronomy of the current Martian atmosphere

    Science.gov (United States)

    Barth, C. A.; Stewart, A. I. F.; Bougher, S. W.; Hunten, D. M.; Bauer, S. J.; Nagy, A. F.

    1992-01-01

    The thermal structure of the Martian atmosphere, which varies diurnally, seasonally and episodically, is discussed. The atomic oxygen airglow at 1304 A is used to determine the density of atomic oxygen, and the 1216-A Lyman-alpha line is used to calculate the density of atomic hydrogen and, when coupled with the temperature measurement, the escape flux of atomic hydrogen. The most intense airglow is the IR atmospheric band of O2 at 1.27 micron that results from the photodissociation of ozone. The escape mechanism for atomic hydrogen is thermal, or Jeans, escape, while the atomic oxygen escape is caused by a nonthermal process, namely, the dissociative recombination of O2(+). The ratio of deuterium to hydrogen is enriched by a factor of 6. Three-dimensional models of the Mars thermospheric circulation show that planetary rotation has a significant effect on the wind, composition, and temperature structure.

  20. Characterization of VHF radar observations associated with equatorial Spread F by narrow-band optical measurements

    Directory of Open Access Journals (Sweden)

    R. Sekar

    2004-09-01

    Full Text Available The VHF radars have been extensively used to investigate the structures and dynamics of equatorial Spread F (ESF irregularities. However, unambiguous identification of the nature of the structures in terms of plasma depletion or enhancement requires another technique, as the return echo measured by VHF radar is proportional to the square of the electron density fluctuations. In order to address this issue, co-ordinated radar backscatter and thermospheric airglow intensity measurements were carried out during March 2003 from the MST radar site at Gadanki. Temporal variations of 630.0-nm and 777.4-nm emission intensities reveal small-scale ("micro" and large-scale ("macro" variations during the period of observation. The micro variations are absent on non-ESF nights while the macro variations are present on both ESF and non-ESF nights. In addition to the well-known anti-correlation between the base height of the F-region and the nocturnal variation of thermospheric airglow intensities, the variation of the base height of the F-layer, on occasion, is found to manifest as a bottomside wave-like structure, as seen by VHF radar on an ESF night. The micro variations in the airglow intensities are associated with large-scale irregular plasma structures and found to be in correspondence with the "plume" structures obtained by VHF radar. In addition to the commonly observed depletions with upward movement, the observation unequivocally reveals the presence of plasma enhancements which move downwards. The observation of enhancement in 777.4-nm airglow intensity, which is characterized as plasma enhancement, provides an experimental verification of the earlier prediction based on numerical modeling studies.

  1. Color enhancement of ten-minute far ultraviolet exposure of Earth

    Science.gov (United States)

    1972-01-01

    An artifically reproduced color enhancement of a ten-minute far-ultraviolet exposure of the Earth, taken with a filter which blocks the glow cause by atomic hydrogen but which transmits the glow caused by atomic oxygen and molecular nitrogen. Note that airglow emission bands are visible on the night side of the Earth, one roughly centered between the two polar auroral zones and one at an angle to this extending northward toward the sunlit side of the Earth.

  2. Optical aeronomy

    Science.gov (United States)

    Solomon, Stanley C.

    1991-01-01

    Optical measurements of thermospheric and ionospheric processes and their interpretation are reviewed and the chemical reactions and their effects on emissions are discussed. Also included are the phenomena which excite the airglow and aurora, i.e., the solar UV/EUV flux and auroral particle precipitation. Consideration is given to solar flux, atomic emissions, molecular emissions, hydrogen geocorona, and molecular oxygen and the green line nightglow.

  3. Measurement of the Characteristics of TIDs Using Small and Regional Networks of GPS Receivers during the Campaign of 17-30 July of 2008

    Science.gov (United States)

    2012-01-01

    M. Sato, Y. Otsuka , T. Takami, and T. Tsuda, “Middle and upper atmosphere radar observations of the dispersion relation for ionospheric gravity waves...vol. 108, no. 21, pp. 1–12, 2003. [17] S. Suzuki, K. Shiokawa, Y. Otsuka , T. Ogawa, and P.Wilkinson, “Statistical characteristics of gravity waves...Ihara, Y. Otsuka , and T. Ogawa, “Statisti- cal study of nighttime medium-scale traveling ionospheric disturbances using midlatitude airglow images

  4. Characteristics of Small-scale Gravity Wave Propagation in the Mesopause Region over Alaska

    Science.gov (United States)

    Kubota, M.; Yamaguchi, Y.; Kawamura, S.; Murayama, Y.; Kita, K.

    2014-12-01

    We investigated characteristics of the atmospheric gravity waves (AGWs) propagation using sodium airglow images obtained by an all-sky imager installed at Poker Flat Research Range (65.1N, 147.4W, MLAT 65.6) in Alaska. In this study, we developed data analysis programs which automatically derive the unambiguous 2-D power spectrum from the sodium airglow images, using a method by Coble et al. (1998). The power spectrums of the AGWs which have horizontal wavelengths between 2 - 400 km and periods up to 8 hours were obtained by these programs. Statistical study of the AGW data and mesospheric wind data by an MF radar during two winter seasons from October 2000 to April 2002 indicates the following characteristics. - During these periods, the AGW dominantly propagated westward in the zonal direction. - The meridional propagation direction frequently changed. This change seems to be explained by filtering effect by the mesospheric wind. - Total power of the AGW increased in December and January. In this paper, we discuss the relationship between these characteristics of the AGW propagation and unique phenomena in high-latitude region such as auroral precipitation. Acknowledgements This work is conducted as a part of "Alaska Project", the cooperative research project between NICT and Geophysical Institute of University of Alaska. Reference Coble, M. R., G. C. Papen, and C. S. Gardner, Computing two-dimensional unambiguous horizontal wavenumber spectra from OH airglow images, IEEE Trans. Geosci. and Remote Sens., 36, 368--382, 1998.

  5. Horizontal structure and propagation characteristics of mesospheric gravity waves observed by Antarctic Gravity Wave Imaging/Instrument Network (ANGWIN), using a 3-D spectral analysis technique

    Science.gov (United States)

    Matsuda, Takashi S.; Nakamura, Takuji; Murphy, Damian; Tsutsumi, Masaki; Moffat-Griffin, Tracy; Zhao, Yucheng; Pautet, Pierre-Dominique; Ejiri, Mitsumu K.; Taylor, Michael

    2016-07-01

    ANGWIN (Antarctic Gravity Wave Imaging/Instrument Network) is an international airglow imager/instrument network in the Antarctic, which commenced observations in 2011. It seeks to reveal characteristics of mesospheric gravity waves, and to study sources, propagation, breaking of the gravity waves over the Antarctic and the effects on general circulation and upper atmosphere. In this study, we compared distributions of horizontal phase velocity of the gravity waves at around 90 km altitude observed in the mesospheric airglow imaging over different locations using our new statistical analysis method of 3-D Fourier transform, developed by Matsuda et al. (2014). Results from the airglow imagers at four stations at Syowa (69S, 40E), Halley (76S, 27W), Davis (69S, 78E) and McMurdo (78S, 156E) out of the ANGWIN imagers have been compared, for the observation period between April 6 and May 21 in 2013. In addition to the horizontal distribution of propagation and phase speed, gravity wave energies have been quantitatively compared, indicating a smaller GW activity in higher latitude stations. We further investigated frequency dependence of gravity wave propagation direction, as well as nightly variation of the gravity wave direction and correlation with the background wind variations. We found that variation of propagation direction is partly due to the effect of background wind in the middle atmosphere, but variation of wave sources could play important role as well. Secondary wave generation is also needed to explain the observed results.

  6. Nonlinear regression method for estimating neutral wind and temperature from Fabry-Perot interferometer data.

    Science.gov (United States)

    Harding, Brian J; Gehrels, Thomas W; Makela, Jonathan J

    2014-02-01

    The Earth's thermosphere plays a critical role in driving electrodynamic processes in the ionosphere and in transferring solar energy to the atmosphere, yet measurements of thermospheric state parameters, such as wind and temperature, are sparse. One of the most popular techniques for measuring these parameters is to use a Fabry-Perot interferometer to monitor the Doppler width and breadth of naturally occurring airglow emissions in the thermosphere. In this work, we present a technique for estimating upper-atmospheric winds and temperatures from images of Fabry-Perot fringes captured by a CCD detector. We estimate instrument parameters from fringe patterns of a frequency-stabilized laser, and we use these parameters to estimate winds and temperatures from airglow fringe patterns. A unique feature of this technique is the model used for the laser and airglow fringe patterns, which fits all fringes simultaneously and attempts to model the effects of optical defects. This technique yields accurate estimates for winds, temperatures, and the associated uncertainties in these parameters, as we show with a Monte Carlo simulation.

  7. Post midnight spread-F occurrence over Waltair (17.7° N, 83.3° E during low and ascending phases of solar activity

    Directory of Open Access Journals (Sweden)

    K. Niranjan

    Full Text Available A study carried out on the occurrence of post midnight spread-F events at a low-latitude station, Waltair (17.7° N, 83.3° E, India revealed that its occurrence is maximum in the summer solstice months of the low solar activity period and decreases with an increase in the sunspot activity. The F-region virtual height variations show that 80% of these spread-F cases are associated with an increase in the F-region altitude. It is suggested with the support of the night airglow 6300 A zenith intensity data obtained with co-located ground-based night airglow photometer and electron temperature data from the Indian SROSS C2 satellite that the seasonal variation of the occurrence and probable onset times of the post midnight spread-F depend on the characteristics of the highly variable semipermanent equatorial Midnight Temperature Maximum (MTM.

    Key words. Ionosphere (ionospheric irregularities; ionosphere atmosphere interactions Atmospheric composition and structure (airglow and Aurora

  8. Statistical analysis of mesospheric gravity waves over King Sejong Station, Antarctica (62.2°S, 58.8°W)

    Science.gov (United States)

    Kam, Hosik; Jee, Geonhwa; Kim, Yong; Ham, Young-bae; Song, In-Sun

    2017-03-01

    We have investigated the characteristics of mesospheric short period (<1 h) gravity waves which were observed with all-sky images of OH Meinel band and OI 557 nm airglows over King Sejong Station (KSS) (62.22°S, 58.78°W) during a period of 2008-2015. By applying 2-dimensional FFT to time differenced images, we derived horizontal wavelengths, phase speeds, and propagating directions (188 and 173 quasi-monochromatic waves from OH and OI airglow images, respectively). The majority of the observed waves propagated predominantly westward, implying that eastward waves were filtered out by strong eastward stratospheric winds. In order to obtain the intrinsic properties of the observed waves, we utilized winds simultaneously measured by KSS Meteor Radar and temperatures from Aura Microwave Limb Sounder (MLS). More than half the waves propagated horizontally, as waves were in Doppler duct or evanescent in the vertical direction. This might be due to strong eastward background wind field in the mesosphere over KSS. For freely propagating waves, the vertical wavelengths were in the interquartile range of 9-33 km with a median value of 15 km. The vertical wavelengths are shorter than those observed at Halley station (76°S, 27°W) where the majority of the observed waves were freely propagating. The difference in the wave propagating characteristics between KSS and Halley station suggests that gravity waves may affect mesospheric dynamics in this part of the Antarctic Peninsula more strongly than over the Antarctic continent. Furthermore, strong wind shear over KSS played an important role in changing the vertical wavenumbers as the waves propagated upward between two airglow layers (87 and 96 km).

  9. What can we do with an atmospheric seismometer moving at 8 km/s?

    Science.gov (United States)

    Garcia, R.; Brissaud, Q.; Martin, R.; Komatitsch, D.; Doornbos, E.; Bruinsma, S.

    2014-12-01

    The solid/ocean/atmosphere coupling of terrestrial planets has been widely investigated through detection and imaging of electron density perturbations in the ionosphere.Recently, two new observations methods have proven their efficiency: perturbations of airglow emissions and variations of the drag of very low Earth orbit satellites.The perturbations of these observables are mainly due to air density variations induced by post-seismic infrasounds or atmospheric gravity waves generated by tsunamis.Even if the airglow emissions present the great advantage of providing an imaging capability, the weakness of the airglow signal induces long integration time, and does not allow to infer high frequency infrasound signals.Moreover, restrictions on observation conditions and line of sight integration reduce the capability of detailed imaging of atmospheric wavefronts.On the other hand, variations of the satellite drag provide only one measurement point along the satellite orbit.However, the unprecedented quality of the data of GOCE mission allows a precise estimate of air density perturbations, but also vertical and cross track winds estimates.Consequently, this capability to measure the vibrations induced by atmospheric waves along 3 axes is very similar to the one of a ground seismometer.We first present some polarisation analysis using these data in order to discriminate between infrasonic waves, gravity waves and perturbations induced by thermosphere dynamics.Then, we summarize some recent developments in numerical modeling of atmospheric and acoustic and gravity wave propagation with SPECFEM software.Finally, we present how this numerical tool will allow to perform studies comparable to what was done in solid seismology.We conclude by a prospect on the application of these observables and numerical tools to other terrestrial planets.

  10. Response of the upper atmosphere to variations in the solar soft x-ray irradiance. Ph.D. Thesis

    Science.gov (United States)

    Bailey, Scott Martin

    1995-01-01

    Terrestrial far ultraviolet (FUV) airglow emissions have been suggested as a means for remote sensing the structure of the upper atmosphere. The energy which leads to the excitation of FUV airglow emissions is solar irradiance at extreme ultraviolet (EUV) and soft x-ray wavelengths. Solar irradiance at these wavelengths is known to be highly variable; studies of nitric oxide (NO) in the lower thermosphere have suggested a variability of more than an order of magnitude in the solar soft x-ray irradiance. To properly interpret the FUV airflow, the magnitude of the solar energy deposition must be known. Previous analyses have used the electron impact excited Lyman-Birge-Hopfield (LBH) bands of N2 to infer the flux of photoelectrons in the atmosphere and thus to infer the magnitude of the solar irradiance. This dissertation presents the first simultaneous measurements of the FUV airglow, the major atmospheric constituent densities, and the solar EUV and soft x-ray irradiances. The measurements were made on three flights of an identical sounding rocket payload at different levels of solar activity. The linear response in brightness of the LBH bands to variations in solar irradiance is demonstrated. In addition to the N2 LBH bands, atomic oxygen lines at 135.6 and 130.4 nm are also studied. Unlike the LBH bands, these emissions undergo radiative transfer effects in the atmosphere. The OI emission at 135.6 nm is found to be well modeled using a radiative transfer calculation and the known excitation processes. Unfortunately, the assumed processes leading to OI 130.4 nm excitation are found to be insufficient to reproduce the observed variability of this emission. Production of NO in the atmosphere is examined; it is shown that a lower than previously reported variability in the solar soft x-ray irradiance is required to explain the variability of NO.

  11. Wave Driven Exothermic Heating in the Mesopause Region

    Science.gov (United States)

    Hickey, Michael P.

    1997-01-01

    A full-wave propagation model was developed that describes the propagation of gravity waves from the Earth's surface to the upper boundary, which can be placed anywhere between 150 and 500 km altitude. The model includes a realistic background atmosphere, and includes the effects of mean horizontal winds and their vertical shears, mean vertical temperature gradients, the eddy and molecular diffusion of heat and momentum, and the effects of ion-drag. This model solves five coupled second-order differential equations (continuity, momentum, and energy) in the vertical coordinate to derive the perturbation variables u', v', w' (horizontal and vertical velocity components), T' (temperature) and p' (pressure). The upper boundary can be automatically selected based on tests using the radiation condition at the upper boundary, wherein the height is increased until the wave is experiencing severe dissipation at the upper boundary, ensuring that substantial absorption occurs for any waves reflected from the upper boundary. The determination of wave amplitude is a key requirement of wave energetics. Therefore, the fullwave model has been applied to airglow observations in order to determine wave amplitudes as a function of altitude. This was accomplished by using the full-wave model output to drive a chemistry perturbation module that describes minor species perturbations and the resulting airglow perturbations. The full-wave output was multiplied by an altitude-independent factor such that the modeled and observed relative airglow intensity perturbations were equal. The effects of mean winds were included in these studies, and found to be the most important model input affecting the calculations (being more important than the choice of eddy diffusion profiles and chemical kinetic coefficients). In one study (Hickey et al., 1997a) these winds could not be well estimated from the measurements, whereas in the second study (Hickey et al.,1997b) the mean were well defined with a

  12. Multi-instrument investigation of troposphere-ionosphere coupling through gravity waves and the role of gravity waves in the formation of equatorial plasma bubbles (EPBs)

    Science.gov (United States)

    Sivakandan, Mani; Patra, Amit; Sripathi, Samireddipelle; Thokuluwa, Ramkumar; Paulino, Igo; Taori, Alok; Kandula, Niranjan

    2016-07-01

    Equatorial plasma bubble (EPB) occurs in the equatorial ionosphere in pre-mid night (most of the time) as well as post-midnight (rarely) hours. The generation of EPBs by Rayleigh-Taylor Instability (RTI) due to seeding of gravity wave perturbation (polarization electric field) have well been explained theoretically by several authors but experimental evidence supporting this hypothesis is very limited. Using co-located observations from Gadanki (13.5oN, 79.2o E) using an all sky airglow imager and Gadanki Ionospheric Radar Interferometer (GIRI) and Ionosonde observations from Tirunelveli (8.7o N, 77.8o E), we investigate the role of gravity waves in the generation EPB during geomagnetic quiet conditions. To avoid any changes occurring in the background ionosphere owing to the large scale features (e.g., seasonal variation), we use four consecutive nights (03-06, February, 2014). Out of these four nights on two nights we have noted very strong plasma depletions in the OI 630 nm airglow emission and radar plumes. We analyse data to identify cases where, 1) EPBs occurred with large amplitudes of mesospheric gravity waves, 2) Occurrence of EPBs without large amplitudes of mesospheric gravity waves, and 3) identifiable mesospheric gravity waves without occurrence of EPBs. In order to calculate the mesospheric gravity wave parameter we used mesospheric OH airglow emission imager data, to identify their propagation to the E-region, we used E-region observations made using the MST radar which resembled the gravity wave signatures. Together with these, by using ray tracing techniques, we have identified the source region of the noted gravity wave events also. These results are discussed in detail in the present study.

  13. Letter to the EditorOn the use of the sunspot number for the estimation of past solar and upper atmosphere conditions from historical and modern auroral observations

    Directory of Open Access Journals (Sweden)

    J. M Vaquero

    2005-07-01

    Full Text Available In this short contribution the use of different sunspot numbers for the estimation of past solar and upper atmosphere conditions from historical and modern auroral observations realised by Schröder et al. (2004 is analysed. Moreover, some comments are made on the relationships between mean annual visual observations of the auroras at middle latitudes of Europe and the mean annual sunspot number during 1780–1829. Keywords. Atmospheric composition and structure (Airglow and aurora – Magnetospheric physics (Auroral phenomena, solar wind-magnetosphere interactions – History of geophysics (Solar-planetary relationship

  14. Dominant winter-time mesospheric wave signatures over a low latitude station, Hawaii (20.8°N): An investigation

    Indian Academy of Sciences (India)

    A Taori; M Taylor

    2010-06-01

    We utilize mesospheric O2 airglow emission intensity and temperature data collected during January–February 2003 on 17 consecutive nights from Maui, Hawaii (20.8°N, 156.2°W) to study the dominant and long period wave features at mesospheric altitudes. Apart from large day-to-day variability, it is found that nocturnal data for the period under consideration was dominated by a terdiurnal tide-like wave. Together, a quasi 5-day wave is also noticed with significant amplitude.

  15. Use of a personal computer for the real-time reception and analysis of data from a sounding rocket experiment

    Science.gov (United States)

    Herrick, W. D.; Penegor, G. T.; Cotton, D. M.; Kaplan, G. C.; Chakrabarti, S.

    1990-01-01

    In September 1988 the Earth and Planetary Atmospheres Group of the Space Sciences Laboratory of the University of California at Berkeley flew an experiment on a high-altitude sounding rocket launched from the NASA Wallops Flight Facility in Virginia. The experiment, BEARS (Berkeley EUV Airglow Rocket Spectrometer), was designed to obtain spectroscopic data on the composition and structure of the earth's upper atmosphere. Consideration is given to the objectives of the BEARS experiment; the computer interface and software; the use of remote data transmission; and calibration, integration, and flight operations.

  16. Layered phenomena in the mesopause region

    Science.gov (United States)

    Plane, J. M. C.; Bailey, S. M.; Baumgarten, G.; Rapp, M.

    2015-05-01

    This special issue of the Journal of Atmospheric and Solar-Terrestrial Physics comprises a collection of papers which were mostly presented at the 11th Layered Phenomena in the Mesopause Region (LPMR) Workshop, held at the University of Leeds between 29th July 2013 and 1st August 2013. The topics covered at the workshop included atmospheric dynamics, mesospheric ice clouds, meteoric metal layers, meteoric smoke particles, and airglow layers. There was also a session on the potential of planned sub-orbital spacecraft for making measurements in the mesosphere and lower thermosphere (MLT).

  17. Determination of Ionospheric Electron Density Profiles from Satellite UV (Ultraviolet) Emission Measurements.

    Science.gov (United States)

    1984-05-17

    events , but the mid- and low- [titude requirements of D.ISP and AWS were also satisfied by this instrument. In fact, even the actual instrument...ledge in the E region. Figure 5 from Takacs and Feldman 1 2 shows the type of airglow spectrum in the far UV (FUV) that can be detected in the daytime...Planck theory, Planet. Space. Sci. 25:743. 16. Anderson, D. N. (1973) A theoretical study of the ionospheric F region. equatorial anamoly , 1, Theory

  18. The effects of magnetic storm phases on F-layer irregularities from auroral to equatorial latitudes

    Science.gov (United States)

    Aarons, Jules; Mendillo, Michael

    1990-12-01

    Some topics of discussion in this journal include the following: The effects of electric field and ring current energy increases on F-layer irregularities at auroral and sub-auroral latitudes; The role of the ring current in generating or inhibiting equatorial F-layer irregularities during magnetic storms; Auroral and sub-auroral F-layer irregularities and high plasma convection during the magnetically active periods of September 17-24, 1984; and Simultaneous All-Sky Optical Airglow Imaging Observations and San Marco Satellite Measurements in the Pacific Sector.

  19. Auroral spectrograph data annals of the international geophysical year, v.25

    CERN Document Server

    Carrigan, Anne; Norman, S J

    1964-01-01

    Annals of the International Geophysical Year, Volume 25: Auroral Spectrograph Data is a five-chapter text that contains tabulations of auroral spectrograph data. The patrol spectrograph built by the Perkin-Elmer Corporation for the Aurora and Airglow Program of the IGY is a high-speed, low-dispersion, automatic instrument designed to photograph spectra of aurora occurring along a given magnetic meridian of the sky. Data from each spectral frame were recorded on an IBM punched card. The data recorded on the cards are printed onto the tabulations in this volume. These tabulations are available

  20. A tenuous carbon dioxide atmosphere on Jupiter's moon Callisto

    Science.gov (United States)

    Carlson, R. W.

    1999-01-01

    An off-limb scan of Callisto was conducted by the Galileo near-infrared mapping spectrometer to search for a carbon dioxide atmosphere. Airglow in the carbon dioxide nu3 band was observed up to 100 kilometers above the surface and indicates the presence of a tenuous carbon dioxide atmosphere with surface pressure of 7.5 x 10(-12) bar and a temperature of about 150 kelvin, close to the surface temperature. A lifetime on the order of 4 years is suggested, based on photoionization and magnetospheric sweeping. Either the atmosphere is transient and was formed recently or some process is currently supplying carbon dioxide to the atmosphere.

  1. Experiment S001: Zodiacal Light Photography

    Science.gov (United States)

    Ney, E. P.; Huch, W. F.

    1971-01-01

    Observations made during the Gemini 5, 9, and 10 missions in the context of their relation to ground-based and balloon-based experiments on dim-light phenomena are reported. Zodiacal light is the visible manifestation of dust grains in orbit around the sun. The negatives that were exposed on the Gemini 9 mission were studied by the use of an isodensitracer to produce intensity isophotes. Data on the following factors were obtained: (1) intensity distribution of the zodiacal light, both morning and evening; (2) the height and intensity of the airglow at various geographic positions; and (3) intensity distribution of the Milky Way in the region of the sky near Cygnus. Also, a previously unreported phenomenon was discovered. This phenomenon appeared as an upward extension of the normal 90-kilometer airglow layer. The extension was in the form of wisps or plumes approximately 5 deg wide and extending upward approximately 5 deg. The results obtained from pictures exposed on the Gemini 10 mission were of qualitative or geometrical value only.

  2. Transition of GAIM from Research to Operations

    Science.gov (United States)

    Nicholas, A. C.; Thonnard, S. E.; Budzien, S. A.; Dandenault, P. B.

    2004-12-01

    In July 2004, Utah State University delivered the Global Assimilation of Ionospheric Measurements (GAIM) for transition to operations at the Air Force Weather Agency (AFWA) by 2006. This system was designed to assimilated measurements from a variety of sources and provide ionospheric specification and forecasting satisfying DoD needs. Coordinated by AFWA, the transition of GAIM to operations at AFWA is a multi-organizational effort and includes data source evaluation, environment porting, validation and integration. The Naval Research Laboratory is responsible for the configuration management of GAIM between the USU and AFWA during this transition process. As such, NRL has installed GAIM to provide daily ionospheric specification and 24 hour forecast on a routine basis. Additionally, NRL has begun new research effort to investigate the assimilation of ultraviolet airglow observations into GAIM. This poster describes the configuration of GAIM at NRL and ionospheric specification capabilities that are currently available. The information will include a background of the assimilation process and data inputs used at NRL. An overview of ongoing GAIM research including plans at NRL to assimilate ultraviolet airglow emission observations will be provided. Additionally, a brief description of the graphical tools to operate the GAIM model and visualize the output will be provided.

  3. The study of equatorial plasma bubble during January to April 2012 over Kolhapur (India

    Directory of Open Access Journals (Sweden)

    Parashram T. Patil

    2016-05-01

    Full Text Available Over 53 nights of all sky airglow imager data collected during January-April 2012 from the low latitude station Kolhapur (16.68°N, 74.26°E; 10.6°N dip latitude have been analyzed to study the F-region dynamics through the imaging of OI 630 nm emission line. The observed night airglow data were supported by the ionosonde measurements from Tirunelveli (8.7°N, 77.8°E; 0.51°N dip latitude. Well defined magnetic field aligned depletions were observed during the observation period. Out of 53 nights, 40 nights exhibited the occurrence of north-south aligned equatorial plasma bubbles. These plasma bubbles were found moving towards east with drift speed in range between 70 to 200 m s-1. We have analyzed the zonal drift velocity variation and relation of bubble occurrence with the base height of the ionosphere together with the effects of the geomagnetic Ap and solar flux F10.7 cm index in its first appearance.

  4. Lines and continuum sky emission in the near infrared: observational constraints from deep high spectral resolution spectra with GIANO-TNG

    CERN Document Server

    Oliva, E; Scuderi, S; Benatti, S; Carleo, I; Lapenna, E; Mucciarelli, A; Baffa, C; Biliotti, V; Carbonaro, L; Falcini, G; Giani, E; Iuzzolino, M; Massi, F; Sanna, N; Sozzi, M; Tozzi, A; Ghedina, A; Ghinassi, F; Lodi, M; Harutyunyan, A; Pedani, M

    2015-01-01

    Aims Determining the intensity of lines and continuum airglow emission in the H-band is important for the design of faint-object infrared spectrographs. Existing spectra at low/medium resolution cannot disentangle the true sky-continuum from instrumental effects (e.g. diffuse light in the wings of strong lines). We aim to obtain, for the first time, a high resolution infrared spectrum deep enough to set significant constraints on the continuum emission between the lines in the H-band. Methods During the second commissioning run of the GIANO high-resolution infrared spectrograph at La Palma Observatory, we pointed the instrument directly to the sky and obtained a deep spectrum that extends from 0.97 to 2.4 micron. Results The spectrum shows about 1500 emission lines, a factor of two more than in previous works. Of these, 80% are identified as OH transitions; half of these are from highly excited molecules (hot-OH component) that are not included in the OH airglow emission models normally used for astronomical ...

  5. Can Ground-based Telescopes Detect The Oxygen 1.27 Micron Absorption Feature as a Biomarker in Exoplanets ?

    CERN Document Server

    Kawahara, Hajime; Takami, Michihiro; Fujii, Yuka; Kotani, Takayuki; Murakami, Naoshi; Tamura, Motohide; Guyon, Olivier

    2012-01-01

    The oxygen absorption line imprinted in the scattered light from the Earth-like planets has been considered as the most promising metabolic biomarker of the exo-life. We examine the feasibility of the detection of the oxygen 1.27 micron band from habitable exoplanets, in particular, around late-type stars with a 30 m class ground-based telescope with a future instrument. We analyzed the night airglow around 1.27 micron with IRCS/echelle spectrometer on Subaru and found that the strong telluric emission from atmospheric oxygen molecules declines by an order of magnitude by the midnight. With compilation of nearby star catalogues combined with the sky background model, we estimate the detectability of the oxygen absorption band from an Earth twin, if exists, around nearby stars. We find that the most dominant photon noise of the oxygen 1.27 micron detection comes from the night airglow if the leakage is suppressed enough to detect the planet. We conclude that the future detectors for which the detection contras...

  6. First ground-based observations of mesopause temperatures above the Eastern-Mediterranean Part I: Multi-day oscillations and tides

    Science.gov (United States)

    Silber, Israel; Price, Colin; Schmidt, Carsten; Wüst, Sabine; Bittner, Michael; Pecora, Emilio

    2017-03-01

    The mesopause region ( 90 km altitude) is the coldest region of our atmosphere, and is found at the boundary between the upper mesosphere and lower thermosphere. Ground-based spectrometers, which are sensitive to the emissions from the hydroxyl (OH*) airglow layer (lying at 87 km altitude), are used to monitor the temperature variability within the mesosphere-lower-thermosphere (MLT), at high temporal resolution. The variability of the MLT region of the atmosphere is driven by momentum deposition from gravity waves, atmospheric tides and planetary waves. The displacement of air caused by these waves can produce strong temperature, wind and species concentration perturbations. In this study we present an analysis of 4-years of OH* rotational temperature data, acquired with the German Aerospace Center (DLR) GRIPS-10 (Ground Based Infrared P-branch Spectrometer) instrument, which was installed in Israel in November 2011. This instrument provided the first long-term ground-based observations of airglow emissions in the Eastern Mediterranean. We show the nocturnal mean temperature analysis, which includes time series as well as spectral analysis of the data. In addition, we obtain (migrating) tidal oscillation estimates from the high resolution (1 min) data, by using harmonic fitting, and we analyze the variability of planetary wave signatures in the residual temperature data, which are retrieved after the removal of the tidal harmonic fits from the data. In this analysis of the residual data we find a dominant quasi-5-7 day planetary wave influence on the mesopause temperatures above the Eastern Mediterranean.

  7. Gravity wave vertical energy flux at 95 km

    Science.gov (United States)

    Jacob, P. G.; Jacka, F.

    1985-01-01

    A three-field photometer (3FP) located at Mt. Torrens near Adelaide, is capable of monitoring different airglow emissions from three spaced fields in the sky. A wheel containing up to six different narrow bandpass interference filters can be rotated, allowing each of the filters to be sequentially placed into each of the three fields. The airglow emission of interest is the 557.7 nm line which has an intensity maximum at 95 km. Each circular field of view is located at the apexes of an equilateral triangle centered on zenith with diameters of 5 km and field separations of 13 km when projected to the 95-km level. The sampling period was 30 seconds and typical data lengths were between 7 and 8 hours. The analysis and results from the interaction of gravity waves on the 557.7 nm emission layer are derived using an atmospheric model similar to that proposed by Hines (1960) where the atmosphere is assumed isothermal and perturbations caused by gravity waves are small and adiabatic, therefore, resulting in linearized equations of motion. In the absence of waves, the atmosphere is also considered stationary. Thirteen nights of quality data from January 1983 to October 1984, covering all seasons, are used in this analysis.

  8. Measurement of two-dimensional Doppler wind fields using a field widened Michelson interferometer.

    Science.gov (United States)

    Langille, Jeffery A; Ward, William E; Scott, Alan; Arsenault, Dennis L

    2013-03-10

    An implementation of the field widened Michelson concept has been applied to obtain high resolution two-dimensional (2D) images of low velocity (<50 m/s) Doppler wind fields in the lab. Procedures and techniques have been developed that allow Doppler wind and irradiance measurements to be determined on a bin by bin basis with an accuracy of less than 2.5 m/s from CCD images over the observed field of view. The interferometer scanning mirror position is controlled to subangstrom precision with subnanometer repeatability using the multi-application low-voltage piezoelectric instrument control electronics developed by COM DEV Ltd.; it is the first implementation of this system as a phase stepping Michelson. In this paper the calibration and characterization of the Doppler imaging system is described and the planned implementation of this new technique for imaging 2D wind and irradiance fields using the earth's airglow is introduced. Observations of Doppler winds produced by a rotating wheel are reported and shown to be of sufficient precision for buoyancy wave observations in airglow in the mesopause region of the terrestrial atmosphere.

  9. Mesospheric temperatures from observations of the hydroxyl (6–2 emission above Davis, Antarctica: A comparison of rotational and Doppler measurements

    Directory of Open Access Journals (Sweden)

    J. L. Innis

    Full Text Available We present observations of the hydroxyl (6–2 airglow lines from ~ 87 km altitude obtained at Davis station, Antarctica, in the austral winter of 1999. Nine nights of observations were made of the P-branch near λ840 nm with a Czerny-Turner scanning spectrometer (CTS; at the same time, high-resolution Fabry-Perot Spectrometer (FPS spectra were collected of the Q1(1 doublet at λ834 nm. Rotational temperatures were determined from the CTS observations, while Doppler temperatures were derived from the line-widths of the FPS Q1(1 spectra. Absolute temperatures determined by these methods are uncertain by ~ 2 and ~ 20 K, respectively. For the comparison we set the value of the reflective finesse of the FPS at λ834 nm so the mean FPS temperature from one night of simultaneous data was equal to that from the CTS, and then looked at the measured variations in each data set for the other eight nights. Both instruments show the upper mesosphere temperature to vary in a similar manner to within the observational errors of the measurements, implying an equivalence of the rotational and Doppler temperatures. We believe that this is the first published simultaneous, same-site, comparison of rotational and Doppler temperatures from the OH emission.

    Key words. Atmospheric composition and structure (airglow and aurora; pressure density and temperature; instruments and techniques

  10. Modelling UV sky for future UV missions

    Science.gov (United States)

    Sreejith, A. G.; Safanova, M.; Mohan, R.; Murthy, Jayant

    Software simulators are now widely used in all areas of science, especially in application to astronomical missions: from instrument design to mission planning, and to data interpretation. We present a simulator to model the diffuse ultraviolet sky, where the different contributors are separately calculated and added together to produce a sky image of the size specified by the instrument requirements. Each of the contributors to the background, instrumental dark current, airglow, zodiacal light and diffuse galactic light, is dependent on various factors. Airglow is dependent on the time of day, zodiacal light on the time of year, angle from the Sun and from the ecliptic, and diffuse UV emission depends on the look direction. To provide a full description of any line of sight, we have also added stars. The diffuse UV background light can dominate in many areas of the sky and severely impact space telescopes viewing directions due to over brightness. The simulator, available as a downloadable package and as a simple web-based tool, can be applied to separate missions and instruments. For demonstration, we present the example used for two UV missions: the UVIT instrument on the Indian ASTROSAT mission to be launched in the next year and a prospective wide-field mission to search for transients in the UV.

  11. Predicting UV sky for future UV missions

    Science.gov (United States)

    Safonova, M.; Mohan, R.; Sreejith, A. G.; Murthy, Jayant

    2013-02-01

    Software simulators are now widely used in all areas of science, especially in application to astronomical missions: from instrument design to mission planning, and to data interpretation. We present a simulator to model the diffuse ultraviolet sky, where the different contributors are separately calculated and added together to produce a sky image of the size specified by the instrument requirements. Each of the contributors to the background, instrumental dark current, airglow, zodiacal light and diffuse Galactic light, depends on different factors. Airglow is dependent on the time of day; zodiacal light depends on the time of year, angle from the Sun and from the ecliptic; diffuse UV emission depends on the line of sight. To provide a full description of the sky along any line of sight, we have also added stars. The UV background light can dominate in many areas of the sky and severely limit viewing directions due to overbrightness. The simulator, available as a downloadable package and as a web-based tool, can be applied to preparation of real space missions and instruments. For demonstration, we present the example use for the two near-future UV missions: UVIT instrument on the Indian Astrosat mission and a new proposed wide-field (∼1000 square degrees) transient explorer satellite.

  12. Ground observation and AMIE-TIEGCM modeling of a large-scale traveling ionospheric disturbance

    Science.gov (United States)

    Shiokawa, K.; Lu, G.; Nishitani, N.; Sato, N.

    We show comparison of ground observation and modeling of a prominent large-scale traveling ionospheric disturbance (LSTID) observed in Japan during the major magnetic storm of March 31, 2001 (Shiokawa et al., JGR, 2003). The LSTID was detected as an enhancement of the 630-nm airglow intensity, an enhancement of GPS-TEC, a decrease of F-layer virtual height, and an increase of foF2. They moved equatorward with a velocity of 400-500 m/s. These results suggest that an enhancement of poleward neutral wind (propagating equatorward as a traveling atmospheric wave) caused the observed ionospheric features of the LSTID. The ion drift measurement by the MU radar and Doppler wind measurement by a Fabry-Perot interferometer (630-nm and 558-nm airglow) at Shigaraki actually showed poleward wind enhancement during the LSTID event. To model this LSTID event, we used the assimilative mapping of ionospheric electrodynamics (AMIE) technique as inputs to the thermosphere-ionosphere-electrodynamics general circulation model (TIEGCM). The model shows fine structures of the poleward wind enhancement both propagated from the auroral zone and generated directly at midlatitudes.

  13. S-NPP VIIRS DNB Dark Offset and Detector Dark Current Trending Study

    Science.gov (United States)

    Sun, Z.; Chen, W.; DeLuccia, F.; Moy, G.

    2015-12-01

    The Visible Infrared Imaging Radiometer Suite (VIIRS) Day-Night Band (DNB) is a panchromatic band in the VisNIR spectral range from 0.5 to 0.9 μm with a dynamic range from 3x10-9 to about 0.02 W cm-2 sr-1. DNB achieves this large dynamic range by having three gain stages: low gain (LGS), mid gain (MGS), and high gain (HGS). HGS is the average of two redundant detector arrays, HGA and HGB. The HGS offset determination is critically important to improve the imagery capability and calibration accuracy and stability at novel low radiances. Currently, the dark offset is determined on a monthly basis by observing new moon data in the dark regions in the Pacific Ocean. The data is mainly comprised of detector dark current, electronic/clock offsets, artificial illumination sources, and nighttime airglow contamination. The first two are instrument phenomena/characterizations and the last two are scene contaminations.In this presentation, we discuss the long-term growth in offset with short-term fluctuations we have captured since the beginning of the mission. We associate the long-term growth with dark current increase. We show that the offset rate of change over time is proportional to the number of Charge Coupled Device (CCD) elements aggregated to comprise a DNB pixel. We compare offset growth rate from new moon data in the dark ocean and that from calibration sector data at the same time; which contain very limited scene contaminations. We associate the short-term variability in offset growth with airglow effects that survive the filtering process used to derive the offsets from dark ocean data. These spurious offset fluctuations are removed from the offset LUTs via long time scale smoothing of the offsets. The remaining persistent time average contribution due to airglow can be estimated by comparison of the pitch maneuver propagated offsets determined from deep space scans early in the mission and the offsets determined from the dark regions in the Pacific Ocean.

  14. CISCO: Cooled Infrared Spectrograph and Camera for OHS on the Subaru Telescope

    Science.gov (United States)

    Motohara, Kentaro; Iwamuro, Fumihide; Maihara, Toshinori; Oya, Shin; Tsukamoto, Hiroyuki; Imanishi, Masatoshi; Terada, Hiroshi; Goto, Miwa; Iwai, Jun'ichi; Tanabe, Hirohisa; Hata, Ryuji; Taguchi, Tomoyuki; Harashima, Takashi

    2002-04-01

    This paper describes a Cooled Infrared Spectrograph and Camera for OHS (CISCO), mounted on the Nasmyth focus of the Subaru telescope. It is primarily designed as a back-end camera of the OH-Airglow Suppressor (OHS), and is also used as an independent, general-purpose near-infrared camera/spectrograph. CISCO is based on a single 1024 × 1024 format HgCdTe HAWAII array detector, and is capable of either wide-field imaging of 1'.8 × 1'.8 field-of-view or low-resolution spectroscopy from 0.9 to 2.4 μm. The limiting magnitudes measured during test observations were found to be J=23.5 mag and K' = 22.4 mag (imaging, 1" aperture, S/N = 5, 1hr exposure).

  15. Near-infrared thermal emissivity from ground based atmospheric dust measurements at ORM

    CERN Document Server

    Lombardi, G; Ortolani, S; Melnick, J; Ghedina, A; Garcia, A; Molinari, E; Gatica, C

    2011-01-01

    We present an analysis of the atmospheric content of aerosols measured at Observatorio del Roque de los Muchachos (ORM; Canary Islands). Using a laser diode particle counter located at the Telescopio Nazionale Galileo (TNG) we have detected particles of 0.3, 0.5, 1.0, 3.0, 5.0 and 10.0 um size. The seasonal behavior of the dust content in the atmosphere is calculated. The Spring has been found to be dustier than the Summer, but dusty conditions may also occur in Winter. A method to estimate the contribution of the aerosols emissivity to the sky brightness in the near-infrared (NIR) is presented. The contribution of dust emission to the sky background in the NIR has been found to be negligible comparable to the airglow, with a maximum contribution of about 8-10% in the Ks band in the dusty days.

  16. STS-39 AFP-675 and STP-1 MPESS in OV-103's payload bay (PLB)

    Science.gov (United States)

    1991-01-01

    An overview of Discovery's, Orbiter Vehicle (OV) 103's, aft payload bay (PLB) documents a variety of STS-39's payloads. In the foreground is the Space Test Payload 1 (STP-1) multipurpose experiment support structure (MPESS) with the Spacecraft Kinetic Infrared Test (SKIRT) (left), ascent particle monitor (APM) (center), and advanced liquid feed experiment (ALFE) (two canisters) visible. Behind the STP-1 is the Air Force Program 675 (AFP-675) experiment support structure (ESS) with ESS tape recorders (left), Uniformly Redundant Array (URA) (front),and Cryogenic Infrared Radiance Instrumentation for Shuttle 1A (CIRRIS-1A) (center back) visible. The ESS pallet power distribution system thermal covering (gold-colored) is visible at the bottom. AFP-675 is a Department of Defense (DOD)-sponsored collection of experiments whose objective is to gather data on the Earth's atmosphere (aurora, Earth limb, and airglow), celestial objects, and the environment in and around the PLB. In the backgroun

  17. STS-39 AFP-675 CIRRIS-1A in OV-103's payload bay (PLB)

    Science.gov (United States)

    1991-01-01

    STS-39's Air Force Program 675 (AFP-675) Uniformly Redundant Array (URA) and Cryogenic Infrared Radiance Instrumentation for Shuttle 1A (CIRRIS-1A) mounted on the experiment support system (ESS) pallet are documented in Discovery's, Orbiter Vehicle (OV) 103's, payload bay (PLB). Part of the ESS pallet power distribution system thermal covering is visible at the bottom of the frame. AFP-675 is a Department of Defense (DOD)-sponsored collection of experiments whose objective is to gather data on the Earth's atmosphere (aurora, Earth limb, and airglow), celestial objects, and the environment in and around the PLB. In the background are the aft PLB bulkhead, the vertical tail, and the orbital maneuvering system (OMS) pods.

  18. On the temperature dependence of the reaction O+NO-NO2(asterisk). [in earth atmosphere

    Science.gov (United States)

    Sharp, W. E.

    1984-01-01

    The published data on the temperature dependence of the radiative combination of atomic oxygen with nitric oxide at pressures near 1 torr is examined. Arguments are advanced to suggest that radiation near the cut-off wavelength (about 3875A) is coming from the unstabilized activated complex, NO2(asterisk). At 4000A a positive activation energy of 1 kcal/mole is deduced. Application of this temperature dependence with the rate coefficient at 5200A is made to airglow measurements in aurora. The deduced NO concentration is about 10 to the 9th per cu cm, in general agreement with that deduced from the measured NO(+)/O2(+) ratio as well as an auroral model prediction.

  19. Wide angle Michelson Doppler imaging interferometer. [measuring atmospheric emissions

    Science.gov (United States)

    Shepherd, G. G.

    1980-01-01

    The optical system, stepping control, phase and modulation depth, array detector, and directions sensor are described for a specialized type of Michelson interferometer which works at sufficiently high resolution to measure the line widths and Doppler shifts of naturally occurring atmospheric emissions. With its imaging capability, the instrument can potentially supply this data independently for each element of the 100 x 100 detector array. The experiment seeks: (1) to obtain vertical profiles of atmospheric winds and temperatures as functions of latitude by observing near the limb; (2) to acquire exploratory wind and temperature data on smaller scale structures in airglow irregularities and in auroral forms; and (3) to collaborate with other Spacelab experiments, such as barium cloud releases, in providing wind and temperature data.

  20. Leonid storm research

    CERN Document Server

    Rietmeijer, Frans; Brosch, Noah; Fonda, Mark

    2000-01-01

    This book will appeal to all researchers that have an interest in the current Leonid showers It contains over forty research papers that present some of the first observational results of the November 1999 Leonid meteor storm, the first storm observed by modern observing techniques The book is a first glimpse of the large amount of information obtained during NASA's Leonid Multi-Instrument Aircraft Campaign and groundbased campaigns throughout the world It provides an excellent overview on the state of meteor shower research for any professional researcher or amateur meteor observer interested in studies of meteors and meteoroids and their relation to comets, the origin of life on Earth, the satellite impact hazard issue, and upper atmosphere studies of neutral atom chemistry, the formation of meteoric debris, persistent trains, airglow, noctilucent clouds, sprites and elves

  1. 2D analytical modeling of distortion and sky background in multi-fiber spectrographs the case of the Norris spectrograph at Palomar Mountain

    CERN Document Server

    Viton, M; Viton, Maurice; Milliard, Bruno

    2002-01-01

    A method for optimal reduction of data taken with multi-fiber spectrographs is described, based on global correction of their geometrical distortion. Though it was specifically developed for reducing observations performed at Palomar Mountain using the Norris fiber spectrograph, this method can be adapted to other types of multi-object spectrographs such as the multi-slit ones. Combined with a 2D analytical interpolation of sky-background that accounts for non-uniform spectral resolution, the Norris software package achieves very high accuracy in airglow subtraction, even in the near infrared (7000-9000A) where molecular band-emissions commonly induce strong artefacts that preclude clean sky subtraction whenever standard image processing techniques are used. Correlatively, an improvement by a factor of 2 on the precision of radial velocities is achievable. Throughout the paper possible improvements to the method are suggested for those devising similar packages for other instruments.

  2. On the dissociation of nitrogen by electron impact and by EUV photo-absorption. [in aurorqs

    Science.gov (United States)

    Zipf, E. C.; Mclaughlin, R. W.

    1978-01-01

    The dissociation of N2 by electron impact and by absorption of EUV photons was studied experimentally. It was shown that most of the N2 molecules excited to singlet states in the 12.5-14.86 eV range are depopulated by predissociation and not by the emission of EUV photons and that this is the principal mechanism by which N2 is dissociated by solar EUV absorption and by electron impact. The experiments provide a physical explanation for the near absence of N2 band radiation in airglow and auroral EUV spectra, and rule out the excitation of EUV radiation as a major factor in the overall energy economy of an auroral substorm.

  3. CISCO Cooled Infrared Spectrograph and Camera for OHS on the Subaru Telescope

    CERN Document Server

    Motohara, K; Maihara, T; Oya, S; Tsukamoto, H; Imanishi, M; Terada, H; Goto, M; Iwai, J; Tanabe, H; Hata, R; Taguchi, T; Harashima, T

    2002-01-01

    This paper describes a Cooled Infrared Spectrograph and Camera for OHS (CISCO), mounted on the Nasmyth focus of the Subaru telescope. It is primarily designed as a back-end camera of the OH-Airglow Suppressor (OHS), and is also used as an independent, general-purpose near-infrared camera/spectrograph. CISCO is based on a single 1024x1024 format HgCdTe HAWAII array detector, and is capable of either wide-field imaging of 1.8'x1.8' field-of-view or low-resolution spectroscopy from 0.9 to 2.4 um. The limiting magnitudes measured during test observations were found to be J=23.5mag and K'=22.4mag (imaging, 1" aperture, S/N=5, 1 hr exposure).

  4. Galmatheia A Galactic Plasma Explorer

    CERN Document Server

    Edelstein, J D; Korpela, E J

    1998-01-01

    Galmatheia is a broad bandpass (900-1800 Angstrom), far-ultraviolet (FUV) nebular spectrograph (lambda /delta lambda ~ 650) for the study of the evolution of galactic plasma with a temperature of 10^4.5 - 10^6 K. Galmatheia will survey the FUV sky with 5' imaging and conduct hundreds of deep 8 degree x 5' field pointings during its proposed two-year mission. Unprecedented sensitivity is achieved by careful exclusion of FUV-bright stars and airglow background. The emission-line sensitivity for a single-day exposure and for a one-year sky survey 3 degree x 3 degree bin yields 50 sigma and 10-15 sigma detections, respectively, of both the predicted radiation from hot Galactic gas and previously-observed diffuse FUV emission. The continuum sensitivity provides 15-25 sigma detections of the predicted flux from unresolved extra-galactic sources.

  5. Evidence of meso-scale structure in the high-latitude thermosphere

    Directory of Open Access Journals (Sweden)

    A. L. Aruliah

    Full Text Available There is a widely held assumption that the thermospheric neutral gas is slow to respond to magnetospheric forcing owing to its large inertia and therefore, may be treated as a steady state background medium for the more dynamic ionosphere. This is shown to be over simplistic. The data presented here compare direct measurements of the thermospheric neutral winds made in Northern Scandinavia by Fabry-Perot Interferometers (FPIs with direct measurements of the ionosphere made by the EISCAT radar and with model simulations. These comparisons will show that the neutral atmosphere is capable of responding to ionospheric changes on mesoscale levels, i.e., spatial and temporal scale sizes of less than a few hundred kilometres and tens of minutes, respectively.

    Key words. Atmospheric composition and structure (air-glow and aurora; instruments and techniques – Ionosphere (ionosphere-atmosphere interactions

  6. Determination of SATI Instrument Filter Parameters by Processing Interference Images

    CERN Document Server

    Atanassov, Atanas Marinov

    2010-01-01

    This paper presents a method for determination of interference filter parameters such as the effective refraction index and the maximal transmittance wavelength on the basis of image processing of a spectrogram produced by Spectrometer Airglow Temperature Imager instrument by means of data processing. The method employs the radial sections for determination of points from the crests and valleys in the spectrograms. These points are involved in the least square method for determination of the centres and radii of the crests and valleys. The use of the image radial sections allows to determine the maximal number of crests and valleys in the spectrogram. The application of the least square fitting leads to determination of the image centers and radii of the crests and valleys with precision higher than one pixel. The nocturnal course of the filter parameters produced by this method is presented and compared with that of the known ones. The values of the filter parameters thus obtained are closer to the laborator...

  7. Joint observations of a traveling ionospheric disturbance with the Paratunka OMTI camera and the Hokkaido HF radar

    Directory of Open Access Journals (Sweden)

    A. Koustov

    2009-06-01

    Full Text Available On 10 September 2007 between 10:00 and 14:00 UT, the OMTI all-sky imager at Paratunka (Kamchatka, Russia, GLAT~52° observed the onset and south-western progression of a localized depletion region in the airglow intensity. The perturbation, while being stretched in the NW-SE direction, crossed the entire field of view of the camera. During the event, the Hokkaido SuperDARN HF radar was monitoring echoes in the Paratunka longitudinal sector. It was detecting a localized band of ground scatter echoes progressing equatorward synchronously with the motion of the optical perturbation. It is suggested that both features resulted from the onset and south-western progression of a localized region with enhanced electric field that influenced the distribution of the plasma density in the ionosphere. Modeling of the HF ground scatter dynamics based on numerical ray tracing demonstrated qualitative consistency with the observations.

  8. Time evolution of high-altitude plasma bubbles imaged at geomagnetic conjugate points

    Directory of Open Access Journals (Sweden)

    K. Shiokawa

    2004-09-01

    Full Text Available Temporal and spatial evolution of two high-altitude plasma bubbles (evening and midnight was observed on 4 April 2002, at geomagnetic conjugate points at Sata, Japan (magnetic latitude 24° N, and Darwin, Australia (magnetic latitude 22° S, using two 630-nm airglow imagers. The apex height of the bubbles reached ~1500km. The upward velocity of the evolution was faster in the evening (~170m/s at 20:00-21:00 LT than around midnight (~28m/s at 23:00-00:00 LT. Bifurcating features of the bubbles into a smaller scale size of ~50km were clearly seen for both the evening and midnight bubbles, showing fairly good conjugacy between the Northern and Southern Hemispheres.

  9. Electron-impact excitation of the Cameron system (a(3)pi yields x(1) Sigma) transition of CO

    Science.gov (United States)

    Erdman, P. W.; Zipf, E. C.

    1983-01-01

    The results of experimental observations of the Cameron bands of CO produced by electron impacts with CO and CO2 are presented, noting that the bands have been detected in the atmospheres of both Mars and Venus. The study was initiated to account for Conway's (1981) data that the Martian airglow displayed cross-sectional dissociative excitation of the Cameron bands seven time larger than laboratory measurements by Ajello (1971). Spectrometer measurements were obtained of processes occurring in a chamber filled with CO or CO2 gas being bombarded by an electron beam. A value three times higher than the previous lab oratory estimate was obtained. Reasons for the discrepancy are discussed, including a present factor of two error in laboratory estimates.

  10. WDC Activities in Japan, 2008

    Directory of Open Access Journals (Sweden)

    Takashi Watanabe

    2009-06-01

    Full Text Available This paper briefly reviews the activities of the International Council for Science (ICSU World Data Centers (WDCs in Japan at a time of great change in the data and information structures of the ICSU ? the creation of the World Data System (WDS in 2009. Seven WDCs are currently operating in Japan: the WDC for Airglow, the WDC for Cosmic Rays, the WDC for Geomagnetism, Kyoto, the WDC for Ionosphere, the WDC for Solar Radio Emission, and the WDC for Space Science Satellites. Although these WDCs are highly active, along-term support system must be established to ensure the stewardship and provision of quality-assessed data and data services to the international science community.

  11. Mesospheric minor species determinations from rocket and ground-based i.r. measurements

    Science.gov (United States)

    Ulwick, J. C.; Baker, K. D.; Baker, D. J.; Steed, A. J.; Pendleton, W. R.; Grossmann, K.; Brückelmann, H. G.

    As part of the MAP/WINE campaign the infrared hydroxyl airglow layer was investigated at Kiruna, Sweden, by simultaneous measurements with rocket probes of OH ≠ and O2( a1Δg) infrared emissions and concentrations of odd oxygen species (O and O 3). Coordinated measurements of OH ≠ and O2( a1Δg) zenith radiance and emission spectra and their time histories were made from the ground. The rocket-borne Λ = 1.55 μm radiometer ( ΔΛ ≊ 0.23 μm) provided volume emission rates for OH for both rocket ascent and descent, showing a peak near 87 km with a maximum of nearly 10 6 photons sec -1 cm -3. The atomic oxygen distribution showed a concentration of about 10 11 cm -3 between 88 and 100 km, dropping off sharply below 85 km. The ground-based radiometer at Λ = 1.56 μm, which had a similar filter bandpass to the rocket-borne instrument, yielded an equivalent of 130 kR for the total OH Δv = 2 sequence, which is consistent with the zenith-corrected rocket-based sequence radiance value of ≌ 110 kR. The rotational temperature of the OH night airglow obtained from the rotational structure of the OH M (3,1) band observed by the ground-based interferometer was about 195K at the time of the rocket measurement. Atomic oxygen concentrations were calculated from the OH profile and show agreement with the directly measured values. Atomic hydrogen concentrations of a few times 10 7 cm -3 near 85 km were inferred from the data set.

  12. Reply to comment by Kil et al. on "The night when the auroral and equatorial ionospheres converged"

    Science.gov (United States)

    Martinis, Carlos; Baumgardner, Jeffrey; Mendillo, Michael; Wroten, Joei; Coster, Anthea J.; Paxton, Larry J.

    2016-10-01

    One of the goals of the Martinis et al. (2015) (M15) paper was to stimulate interest in the topic of "severe events during moderate geomagnetic storms"—and we succeeded. We welcome the Comment by Kil et al. (2016) (K16) who identified weak signatures related to medium-scale traveling ionospheric disturbances (MSTIDs) and tried to argue that airglow depletion signatures of equatorial spread F (ESF) were not present. We agree with K16 in that MSTIDs were present to the north of the all-sky imager, but only during the early observations. They are easily distinguished from the ESF-related dark structures observed at the same time to the south of the imager. We stress some observational facts that K16 overlooked or erroneously used to support their case. M15 offered evidence and discussion evidence and discussion of a dynamical pattern—both in space and time domains—and the counter arguments by K16 should have dealt with the same places and same times. We also point out that the GPS data shown by K16 do not provide any information below 30° geographic latitude in the longitude sector covered by the all-sky imager. This is the region where the ESF structures appeared first and grew to reach higher latitudes. We believe that the issues addressed by K16 do not provide conclusive evidence to rule out the interpretation given by M15 on the nature of the airglow depletions observed at McDonald Observatory.

  13. Space-borne imaging observation of the terrestrial upper atmosphere by ISS-IMAP

    Science.gov (United States)

    Saito, Akinori; Otsuka, Yuichi; Yamamoto, Mamoru; Yamazaki, Atsushi; Yoshikawa, Ichiro; Sakanoi, Takeshi

    ISS-IMAP (Ionosphere, Mesosphere, upper Atmosphere, and Plasmasphere mapping) mission is a space-borne mission on the international space station (ISS) to elucidate the mesoscale structures in the ionosphere, the mesosphere, and the plasmasphere by imaging observations. ISS-IMAP measures the following three parameters: (1) distribution of the atmospheric gravity wave in the mesopause (87km), the ionospheric E-region (95km), and the ionospheric F-region (250km) (2) distribution of the ionized atmosphere in the ionospheric F-region (3) distribution of O+ and He+ ions in the ionosphere and plasmasphere. After the initial check outs, its observation was started in October 2012. ISS-IMAP consists of two imaging instruments on the Exposed Facility of Japanese Experiment Module of the International Space Station, EF of ISS-JEM. Visible-light and infrared spectrum imager (VISI) observes the Mesosphere and the Ionosphere. Extra ultraviolet imager (EUVI) observes the Ionosphere and the Plasmasphere. VISI observes the airglow of 730nm (OH, Alt. 85km), 762nm (O2, Alt. 95km), and 630nm (O, Alt. 250km) in the Nadir direction. The global distributions of the airglow structures whose scale size is 50-500km in the nightside of the Mesosphere and the Ionosphere have been obtained by the VISI observation. EUVI measures the resonant scattering of 30.4nm [He+] and 83.4nm [O+]. Its field- of-view is 15 degrees, and points the limb of the Earth to observe the vertical distribution of the ions. The continuous observation of ISS-IMAP started in October 2012. The coordinated observation between ISS-IMAP and the several ground-based instruments have been carried out to elucidate the coupling process between the lower atmosphere and the upper atmosphere by the wave structures in this scale.

  14. MOOSE: A Multi-Spectral Observatory Of Sensitive EMCCDs for innovative research in space physics and aeronomy

    Science.gov (United States)

    Samara, M.; Michell, R. G.; Hampton, D. L.; Trondsen, T.

    2012-12-01

    The Multi-Spectral Observatory Of Sensitive EMCCDs (MOOSE) consists of 5 imaging systems and is the result of an NSF-funded Major Research Instrumentation project. The main objective of MOOSE is to provide a resource to all members of the scientific community that have interests in imaging low-light-level phenomena, such as aurora, airglow, and meteors. Each imager consists of an Andor DU-888 Electron Multiplying CCD (EMCCD), combined with a telecentric optics section, made by Keo Scientific Ltd., with a selection of available angular fields of view. During the northern hemisphere winter the system is typically based and operated at Poker Flat Research Range in Alaska, but any or all imagers can be shipped anywhere in individual stand-alone cases. We will discuss the main components of the MOOSE project, including the imagers, optics, lenses and filters, as well as the Linux-based control software that enables remote operation. We will also discuss the calibration of the imagers along with the initial deployments and testing done. We are requesting community input regarding operational modes, such as filter and field of view combinations, frame rates, and potentially moving some imagers to other locations, either for tomography or for larger spatial coverage. In addition, given the large volume of auroral image data already available, we are encouraging collaborations for which we will freely distribute the data and any analysis tools already developed. Most significantly, initial science highlights relating to aurora, airglow and meteors will be discussed in the context of the creative and innovative ways that the MOOSE observatory can be used in order to address a new realm of science topics, previously unachievable with traditional single imager systems.

  15. Regional variations of mesospheric gravity-wave momentum flux over Antarctica

    Directory of Open Access Journals (Sweden)

    P. J. Espy

    2006-03-01

    Full Text Available Images of mesospheric airglow and radar-wind measurements have been combined to estimate the difference in the vertical flux of horizontal momentum carried by high-frequency gravity waves over two dissimilar Antarctic stations. Rothera (67° S, 68° W is situated in the mountains of the Peninsula near the edge of the wintertime polar vortex. In contrast, Halley (76° S, 27° W, some 1658 km to the southeast, is located on an ice sheet at the edge of the Antarctic Plateau and deep within the polar vortex during winter. The cross-correlation coefficients between the vertical and horizontal wind perturbations were calculated from sodium (Na airglow imager data collected during the austral winter seasons of 2002 and 2003 at Rothera for comparison with the 2000 and 2001 results from Halley reported previously (Espy et al., 2004. These cross-correlation coefficients were combined with wind-velocity variances from coincident radar measurements to estimate the daily averaged upper-limit of the vertical flux of horizontal momentum due to gravity waves near the peak emission altitude of the Na nightglow layer, 90km. The resulting momentum flux at both stations displayed a large day-to-day variability and showed a marked seasonal rotation from the northwest to the southwest throughout the winter. However, the magnitude of the flux at Rothera was about 4 times larger than that at Halley, suggesting that the differences in the gravity-wave source functions and filtering by the underlying winds at the two stations create significant regional differences in wave forcing on the scale of the station separation.

  16. Case study of a mesospheric wall event over Ferraz station, Antarctica (62° S

    Directory of Open Access Journals (Sweden)

    C. M. Denardini

    2011-01-01

    Full Text Available On 16–17 July 2007 during an observational campaign at Comandante Ferraz Antarctic Station (62° S, 58° W, a mesospheric wall was observed with an airglow all-sky imager. The wave appeared like an extensive dark region in the all-sky airglow images, with a large depletion in the OH emission. Simultaneous mesospheric winds measured with a MF radar at Rothera station and temperature profiles from SABER instrument, on board of TIMED satellite, were used to obtain the propagation condition of the wave. Wind measurements during four days, around the time of observation of the wave, are presented in order to discuss the type and consistence of the duct in which this wave was propagating. By using wavelet analysis and tidal amplitude components we found that 12 and 8 h components were the most important periodicities around the time interval of the wave observation. A collocated imaging spectrometer, for mesospheric temperature measurements, has been operated simultaneously with the all-sky imager. Direct effects of the mesospheric front have been seen in the spectrometric measurements, showing an abrupt decrease in both OH intensity and rotational temperature when the wave front passes overhead. The main contribution of the present work is the investigation of the type of duct in which the wall event was propagating. We found evidences for a thermal duct structure to support the mesospheric wall propagation. This result was obtained by two types of analysis: (a the tidal components analysis and winds filtering (harmonic analysis, and (b comparison between the terms of the m2 dispersion relation.

  17. Ionospheric and Thermospheric Imaging from Geosynchronous Orbit

    Science.gov (United States)

    McCoy, R. P.; Wood, K.; Dymond, K. F.; Thonnard, S. E.; Cannon, K.; Makela, J.

    2001-12-01

    The Office of Naval Research is sponsoring the development of an ultraviolet imaging system to test the concept of real-time synoptic observations of the ionosphere and thermosphere from geosynchronous orbit. The observational hardware consists of two ultraviolet telescopes mounted to a two-axis gimbal to measure airglow radiances on the disk and limb of the Earth. A far-ultraviolet telescope will use a filter wheel with filters to image atomic oxygen emission at 130.4 nm, 135.6 nm, and molecular nitrogen emission at 143.0 nm. An extreme-ultraviolet telescope will image the oxygen ion airglow at 83.4 nm. The oxygen emission measurements will be used to infer nightside ionospheric total electron content (TEC) on the disk and electron density profiles on the limb. On the dayside the oxygen ion measurements will be used to determine electron density profiles, and the oxygen and nitrogen measurements will be used to infer thermospheric neutral density profiles on the limb and O/N2 ratios on the disk. The telescope fields of view cover a 1000 km x 1000 km region with 10 km x 10 km resolution. A goal for nightside TEC measurements is to obtain images with 100 second integrations and to be able to track ionospheric irregularities in real time as "weather systems". Ratios of oxygen nightglow measurements will be used to explore the possibility of providing three dimensional measurements of the ionosphere. These telescopes will be mounted aboard an Air Force Space Test Program satellite which will be launched into geosynchronous orbit over the continental U. S. for about year and then moved over the Indian Ocean for an additional seven years.

  18. Polar ionospheric responses to solar wind IMF changes

    Directory of Open Access Journals (Sweden)

    Y. Zhang

    Full Text Available Auroral and airglow emissions over Eureka (89° CGM during the 1997-98 winter show striking variations in relation to solar wind IMF changes. The period January 19 to 22, 1998, was chosen for detailed study, as the IMF was particularly strong and variable. During most of the period, Bz was northward and polar arcs were observed. Several overpasses by DMSP satellites during the four day period provided a clear picture of the particle precipitation producing the polar arcs. The spectral character of these events indicated excitation by electrons of average energy 300 to 500 eV. Only occasionally were electrons of average energy up to ~1 keV observed and these appeared transitory from the ground optical data. It is noted that polar arcs appear after sudden changes in IMF By, suggesting IMF control over arc initiation. When By is positive there is arc motion from dawn to dusk, while By is negative the motion is consistently dusk to dawn. F-region (anti-sunward convections were monitored through the period from 630.0 nm emissions. The convection speed was low (100-150 m/s when Bz was northward but increased to 500 m/s after Bz turned southward on January 20.

    Key words: Atmospheric composition and structure (airglow and aurora - Ionosphere (particle precipitation - Magnetospheric Physics (polar cap phenomena

  19. Oxygen Atom Recombination in Carbon Dioxide Atmospheres

    Science.gov (United States)

    Jamieson, Corey; Garcia, R. M.; Pejakovic, D. A.; Kalogerakis, K. S.

    2009-09-01

    Understanding processes involving atomic oxygen is crucial for the study and modeling of composition, energy transfer, airglow, and transport dynamics in planetary atmospheres. Significant gaps and uncertainties exist in our understanding of the above processes, and often the relevant input from laboratory measurements is missing or outdated. We are conducting experiments to measure the rate coefficients for O + O + CO2 and O + O2 + CO2 recombination and investigate the O2 excited states produced following O-atom recombination. These laboratory measurements are key input for a quantitative understanding and reliable modeling of the atmospheres of the CO2 planets and their airglow. An ArF excimer laser with 193-nm pulsed output radiation is employed to partially photodissociate carbon dioxide. In an ambient-pressure (760 Torr) background of CO2, the O atoms produced recombine in a time scale of a few milliseconds. Detection of laser-induced fluorescence at 845 nm following two-photon excitation near 226 nm monitors the decay of the oxygen atom population. From the temporal evolution of the signal we can extract the rate coefficients for recombination of O + O and O + O2 in the presence of CO2. We also use fluorescence and resonance-enhanced multi-photon ionization techniques to detect the products of the O-atom recombination and subsequent relaxation in CO2. This work is supported by the US National Science Foundation's (NSF) Planetary Astronomy Program. Rosanne Garcia's participation was funded by the NSF Research Experiences for Undergraduates (REU) Program.

  20. Mesopause temperature perturbations caused by infrasonic waves as a potential indicator for the detection of tsunamis and other geo-hazards

    Directory of Open Access Journals (Sweden)

    M. Bittner

    2010-07-01

    Full Text Available Many geo-hazards such as earthquakes, tsunamis, volcanic eruptions, severe weather, etc., produce acoustic waves with sub-audible frequency, so called infrasound. This sound propagates from the surface to the middle and upper atmosphere causing pressure and temperature perturbations. Temperature fluctuations connected with the above mentioned events usually are very weak at the surface, but the amplitude increases with height because of the exponential decrease of atmospheric pressure with increasing altitude. At the mesopause region (80–100 km height signal amplitudes are about two to three orders of magnitude larger than on the ground.

    The GRIPS (GRound-based Infrared P-branch Spectrometer measurement system operated by the German Remote Sensing Data Center of the German Aerospace Center (DLR-DFD derives temperatures of the mesopause region by observing hydroxyl (OH airglow emissions in the near infrared atmospheric emission spectrum originating from a thin layer at approximately 87 km height.

    The GRIPS instrument is in principle suited for the detection of infrasonic signals generated by e.g. tsunamis and other geo-hazards. This is due to the fact that the infrasound caused by such events should induce observable short-period fluctuations in the OH airglow temperatures. First results obtained during a field campaign performed at the Environmental Research Station "Schneefernerhaus", Zugspitze (47.4° N, 11.0° E from October to December 2008 are presented regarding potential sources of meteorological and orographical origin.

    An adequate distinction of the overlapping infrasonic signatures caused by different infrasound sources in the OH temperature record is needed for the ascription to the proper source. The approach presented here could form a contribution to a hazard monitoring and early warning system.

  1. All Sky Imager Network for Science and Education

    Science.gov (United States)

    Bhatt, A.; Kendall, E. A.; Zalles, D. R.; Baumgardner, J. L.; Marshall, R. A.; Kaltenbacher, E.

    2012-12-01

    A new all sky imager network for space weather monitoring and education outreach has been developed by SRI International. The goal of this program is to install sensitive, low-light all-sky imagers across the continental United States to observe upper atmospheric airglow and aurora in near real time. While aurora borealis is often associated with the high latitudes, during intense geomagnetic storms it can extend well into the continental United States latitudes. Observing auroral processes is instrumental in understanding the space weather, especially in the times of increasing societal dependence on space-based technologies. Under the THEMIS satellite program, Canada has installed a network of all-sky imagers across their country to monitor aurora in real-time. However, no comparable effort exists in the United States. Knowledge of the aurora and airglow across the entire United States in near real time would allow scientists to quickly assess the impact of a geomagnetic storm in concert with data from GPS networks, ionosondes, radars, and magnetometers. What makes this effort unique is that we intend to deploy these imagers at high schools across the country. Selected high-schools will necessarily be in rural areas as the instrument requires dark night skies. At the commencement of the school year, we plan to give an introductory seminar on space weather at each of these schools. Science nuggets developed by SRI International in collaboration with the Center for GeoSpace Studies and the Center for Technology in Learning will be available for high school teachers to use during their science classes. Teachers can use these nuggets as desired within their own curricula. We intend to develop a comprehensive web-based interface that will be available for students and scientific community alike to observe data across the network in near real time and also to guide students towards complementary space weather data sets. This interface will show the real time extent of

  2. Extreme ultraviolet spectral irradiance measurements since 1946

    Science.gov (United States)

    Schmidtke, G.

    2015-03-01

    In the physics of the upper atmosphere the solar extreme ultraviolet (EUV) radiation plays a dominant role controlling most of the thermospheric/ionospheric (T/I) processes. Since this part of the solar spectrum is absorbed in the thermosphere, platforms to measure the EUV fluxes became only available with the development of rockets reaching altitude levels exceeding 80 km. With the availability of V2 rockets used in space research, recording of EUV spectra started in 1946 using photographic films. The development of pointing devices to accurately orient the spectrographs toward the sun initiated intense activities in solar-terrestrial research. The application of photoelectric recording technology enabled the scientists placing EUV spectrometers aboard satellites observing qualitatively strong variability of the solar EUV irradiance on short-, medium-, and long-term scales. However, as more measurements were performed more radiometric EUV data diverged due to the inherent degradation of the EUV instruments with time. Also, continuous recording of the EUV energy input to the T/I system was not achieved. It is only at the end of the last century that there was progress made in solving the serious problem of degradation enabling to monitore solar EUV fluxes with sufficient radiometric accuracy. The data sets available allow composing the data available to the first set of EUV data covering a period of 11 years for the first time. Based on the sophisticated instrumentation verified in space, future EUV measurements of the solar spectral irradiance (SSI) are promising accuracy levels of about 5% and less. With added low-cost equipment, real-time measurements will allow providing data needed in ionospheric modeling, e.g., for correcting propagation delays of navigation signals from space to earth. Adding EUV airglow and auroral emission monitoring by airglow cameras, the impact of space weather on the terrestrial T/I system can be studied with a spectral terrestrial

  3. Mesospheric imaging Michelson interferometer instrument development and observations

    Science.gov (United States)

    Babcock, David D.

    This dissertation demonstrated the capability of the Mesospheric Imaging Michelson Interferometer (MIMI) instrument to passively measure wind velocities from Doppler-shifted atmospheric airglow emissions. The work consisted of two parts, (i) laboratory work focused on the measurement of simulated atmospheric winds with both Doppler-shifted visible and near-IR wavelengths and (ii) the development of a field instrument based on a lab prototype to investigate the potential of measuring Mesospheric winds from the ground. The primary component of the MIMI instrument was a custom built Michelson interferometer which was field widened, chromatically compensated, thermally compensated, and monolithic with no moving parts. The Michelson interferometer, used together with a novel four-point wind retrieval algorithm, provides simultaneous emission rate and wind velocity data over a single integration time. Simultaneously measuring the emission rate over the FOV and measuring wind velocity relative to the observer, of an air parcel containing an emitting chemical species, is a unique feature of the MIMI instrument. Eliminating sequential scanning of the Michelson to measure wind velocities (or being able to take a 'snapshot' of the atmosphere) and provide data on the emission rates and wind velocities, renders the instrument insensitive to scene changes over the integration time, which is an advantage over traditional scanning Michelson interferometers. Spectral lines from visible and near-IR sources were Doppler shifted in a controllable procedure to provide known velocities which were compared to the velocities measured by the interferometer. Wind simulations completed in the visible wavelength region retrieved velocities to within a standard deviation of +/-1ms-1. Wind simulations in the near-IR retrieved wind velocities to within a standard deviation of +/-2ms -1. These standard deviations are acceptable when compared to typical Mesospheric winds of 10 to 100ms-1 and when

  4. Atmospheric Sciences Meet Astronomy: Mutual Benefits from two Different Approaches

    Science.gov (United States)

    Kausch, Wolfgang; Noll, Stefan; Kimeswenger, Stefan; Kondrak, Matthias; Unterguggenberger, Stefanie; Przybilla, Norbert; Lakićević, Maša; Zeilinger, Werner

    2016-04-01

    Light from astronomical targets has to pass the Earth's atmosphere when being observed by ground-based telescope facilities. The signal detected by modern astronomical spectrographs is significantly influenced by molecular absorption and airglow emission. The first mainly arises from various species in the lower, thus denser atmosphere, whereas the latter is caused by chemiluminescence in the mesopause region and above. As ground-based astronomical spectrographs are optimised from the near-UV to the mid-infrared regime (0.3....25μm), a number of absorption features from numerous species are directly visible (e.g. H2O, CO2, CH4, O2, O3,...). The same is true for the airglow emission arising e.g. from the hydroxyl radical and oxygen. The high resolution provided by some spectrographs and their frequent usage allows a detailed investigation of atmospheric lines. Usually being a source of noise for astronomers, which needs to be corrected for, this influence can be used to precisely analyse the composition and the state of the Earth's atmosphere above an observatory. On the other hand, a good knowledge of this allows astronomers to better correct for this influence. Thus, both, atmospheric and astronomical sciences highly benefit from a good understanding of the atmospheric state above an observatory. During the past years we conducted several studies to link astronomical and atmospheric data. For this purpose we use data taken with the Very Large Telescope (VLT) operated by the European Southern Observatory, and the Cerro Armazones Observatory (OCA, University of Bochum, Germany; Universidad Católica del Norte, Chile), both located in the Chilean Atacama desert. The three spectrographs used in our studies are X-Shooter@VLT (resolving power R˜3300...18000, wavelength range λ=0.3...2.5μm), UVES@VLT (R˜20.000....110.000, λ=0.3....1.1μm), and BESO@OCA (R=50000@Hα=0.656μm, λ=0.38 - 0.84μm). In addition, we use atmospheric data obtained with the satellites

  5. The Ultraviolet Spectrograph on the Europa Mission (Europa-UVS)

    Science.gov (United States)

    Retherford, K. D.; Gladstone, R.; Greathouse, T. K.; Steffl, A.; Davis, M. W.; Feldman, P. D.; McGrath, M. A.; Roth, L.; Saur, J.; Spencer, J. R.; Stern, S. A.; Pope, S.; Freeman, M. A.; Persyn, S. C.; Araujo, M. F.; Cortinas, S. C.; Monreal, R. M.; Persson, K. B.; Trantham, B. J.; Versteeg, M. H.; Walther, B. C.

    2015-12-01

    NASA's Europa multi-flyby mission is designed to provide a diversity of measurements suited to enrich our understanding of the potential habitability of this intriguing ocean world. The Europa mission's Ultraviolet Spectrograph, Europa-UVS, is the sixth in a series of successful ultraviolet imaging spectrographs (Rosetta-Alice, New Horizons Pluto-Alice, LRO-LAMP) and, like JUICE-UVS (now under Phase B development), is largely based on the most recent of these to fly, Juno-UVS. Europa-UVS observes photons in the 55-210 nm wavelength range, at moderate spectral and spatial resolution along a 7.5° slit. Three distinct apertures send light to the off-axis telescope mirror feeding the long-slit spectrograph: i) a main entrance airglow port is used for most observations (e.g., airglow, aurora, surface mapping, and stellar occultations); ii) a high-spatial-resolution port consists of a small hole in an additional aperture door, and is used for detailed observations of bright targets; and iii) a separate solar port allows for solar occultations, viewing at a 60° offset from the nominal payload boresight. Photon event time-tagging (pixel list mode) and programmable spectral imaging (histogram mode) allow for observational flexibility and optimal science data management. As on Juno-UVS, the effects of penetrating electron radiation on electronic parts and data quality are mitigated through contiguous shielding, filtering of pulse height amplitudes, management of high-voltage settings, and careful use of radiation-hard parts. The science goals of Europa-UVS are to: 1) Determine the composition & chemistry, source & sinks, and structure & variability of Europa's atmosphere, from equator to pole; 2) Search for and characterize active plumes in terms of global distribution, structure, composition, and variability; 3) Explore the surface composition & microphysics and their relation to endogenic & exogenic processes; and 4) Investigate how energy and mass flow in the Europa

  6. Observation of a mesospheric front in a dual duct over King George Island, Antarctica

    Directory of Open Access Journals (Sweden)

    J. V. Bageston

    2011-05-01

    Full Text Available A mesospheric bore was observed with an all-sky airglow imager on the night of 9–10 July 2007 at Ferraz Station (62° S, 58° W, located on King George island on the Antarctic Peninsula. The observed bore propagated from southwest to northeast with a well defined wave front and a series of crests behind the main front. There was no evidence of dissipation during its propagation within the field of view. The wave parameters were obtained via a 2-D Fourier transform of the imager data providing a horizontal wavelength of 33 km, an observed period of 6 min, and a horizontal phase speed of 92 m s−1. Simultaneous mesospheric winds were measured with a medium frequency (MF radar at Rothera Station (68° S, 68° W and temperature profiles were obtained from the SABER instrument on the TIMED satellite. These wind and temperature profiles were used to estimate the propagation environment of the bore. A wavelet technique was applied to the wind in the plane of bore propagation at the OH emission height spanning three days centered on the bore event to define the dominant periodicities. Results revealed a dominance of near-inertial periods, and semi-diurnal and terdiurnal tides suggesting that the ducting structure enabling bore propagation occurred on large spatial scales. The observed tidal motions were used to reconstruct the winds employing a least-squares method, which were then compared to the observed ducting environment. Results suggest an important contribution of large-scale winds to the ducting structure, but with buoyancy frequency variations in the vertical also expected to be important. These results allow us to conclude that the bore was supported by a duct including contributions from both winds and temperature (or stability. A co-located airglow temperature imager operated simultaneously with the all-sky imager confirmed that the bore event was the dominant small-scale wave event during the analysis interval.

  7. Characterizing Near-Infrared Sky Brightness in the Canadian High Arctic

    CERN Document Server

    Sivanandam, Suresh; Abraham, Roberto; Tekatch, Anthony; Steinbring, Eric; Ngan, Wayne; Welch, Doug L; Law, Nicholas M

    2012-01-01

    We present the first measurements of the near-infrared (NIR), specifically the J-band, sky background in the Canadian High Arctic. There has been considerable recent interest in the development of an astronomical observatory in Ellesmere Island; initial site testing has shown promise for a world-class site. Encouragement for our study came from sky background measurements on the high Antarctic glacial plateau in winter that showed markedly lower NIR emission when compared to good mid-latitude astronomical sites due to reduced emission from OH airglow lines. This is possibly a Polar effect and may also be present in the High Arctic. To test this hypothesis, we carried out an experiment which measured the the J-band sky brightness in the High Arctic during winter. We constructed a zenith-pointing, J-band photometer, and installed it at the Polar Environment Atmospheric Research Laboratory (PEARL) near Eureka, Nunavut (latitude: 80 degrees N). We present the design of our photometer and our results from our shor...

  8. The Climatology of Neutral Winds in the MLT Region as Observed From Orbit

    Science.gov (United States)

    Niciejewski, R.; Skinner, W.; Gell, D.; Cooper, M.; Marsh, A.; Killeen, T.; Wu, Q.; Solomon, S.; Ortland, D.; Drob, D.; Emmert, J.

    2005-12-01

    Unique observations of the horizontal neutral winds in the altitude range 70 to 115 km have been performed from satellite platforms by HRDI and WINDII (UARS) and by TIDI (TIMED), the former since September 1991 and the latter since January 2002. All three experiments observed airglow on the terrestrial limb and derived vertical wind profiles of geophysical quantities by inverting altitude scans of Doppler shifted emission spectra. As a result, the global mesosphere / lower thermosphere region has been sampled for 14 years by a common technique resulting in an unparalleled neutral wind database. This database will be one of the key contributions to an improved Horizontal Wind Model (HWM). This paper will describe results from the first long term climatological study of the MLT region based on satellite wind measurements. The basic dynamic structure in the MLT is a tide, which also has long-term variation that has similar periods to the 27-month QBO (quasi-biennial oscillation) and the SAO (semi-annual oscillation). Signatures of ultra-long variability require analysis of the full wind database.

  9. Indirect methods of retrieval of important mesospheric gas constituents from available measurements data

    Science.gov (United States)

    Kulikov, Mikhail; Nechaev, Anton; Belikovich, Mikhail; Ermakova, Tatiana; Feigin, Alexander

    2016-04-01

    Observation of minor gas constituents is traditionally considered as one of the fundamental problems in investigations of the Earth's mesosphere and mesopause region. Since direct and regular measurements are still rather scanty, indirect methods are a useful tool. Based on a priori assumptions about possible relationships between measured and retrieved characteristics (for example, photochemical models), they allow one to obtain additional information about the important constituents from available experimental data. In this presentation we discuss, firstly, the restrictions on the use of the ozone steady state equilibrium condition for the retrieval of atomic oxygen and hydrogen concentrations from O2 and OH airglow emissions ratios and O3 concentration measurements. Secondly, we present a statistical Bayesian procedure of retrieving the concentrations of important constituents in mesosphere from available satellite and ground based experimental data. The technique is based on the application of the so-called basic dynamic model of mesospheric photochemistry, which is simplified mathematically correctly in a special manner and describes the most significant reactions between components of the families of odd hydrogen and oxygen. The work was supported by the Russian Science Foundation (Contract No. 15-17-10024).

  10. The Puzzling Detection of X-rays From Pluto by Chandra

    CERN Document Server

    Lisse, C M; Wolk, S J; Bagenal, F; Stern, S A; Gladstone, G R; Cravens, T E; Hill, M E; Kollmann, P; Weaver, H A; Strobel, D F; Elliott, H A; McComas, D J; Binzel, R P; Snios, B T; Bhardwaj, A; Chutjian, A; Young, L A; Olkin, C B; Ennico, K A

    2016-01-01

    Using Chandra ACIS-S, we have obtained imaging Xray spectrophotometry of the Pluto system in support of the New Horizons flyby on 14 July 2015. 174 ksec of observations were obtained on 4 visits in Feb 2014 to Aug 2015. We measured a net signal of 6.8 counts and a noise level of 1.2 counts in a comoving 11 x 11 pixel box (100 x 100 R_Pluto) in the 0.31 to 0.60 keV passband for a detection at > 99.95 C.L. The Pluto photons do not match the background spectrum, are coincident with a 90% flux aperture comoving with Pluto, and are not sky source confused. The mean 0.31 to 0.60 keV Xray power from Pluto is 200 MW, in the midrange of Xray power levels seen for known solar system emission sources: auroral precipitation, solar Xray scattering, and charge exchange (CXE) between solar wind (SW) ions & atmospheric neutrals. We eliminate auroral effects as a source, as Pluto has no known magnetic field & the New Horizons Alice UV spectrometer detected no airglow from Pluto during the flyby. Nano-scale atmospheric...

  11. Detection of small scale fluctuations in the near-IR cosmic infrared background from long exposure 2MASS fields

    CERN Document Server

    Kashlinsky, A; Mather, J; Skrutskie, M F; Cutri, R M

    2002-01-01

    We report first results for the cosmic infrared background (CIB) fluctuations at 1.25, 1.65 and 2.17 micron obtained from long exposures constructed from 2MASS standard star fields. We have co-added and analyzed scans from one such field with a total exposure time > 1 hour, and removed sources and other artifacts. The stars and galaxies were clipped out to K_s~19^m leaving only high-z galaxies (or possibly local low-surface-brightness systems). The residual component of the diffuse emission on scales from a few arc-sec to a few arc-min has a power-law slope consistent with emission produced by clustered galaxies. The noise (and residual artifacts) contribution to the signal is small and the colors of the signal are very different from Galactic stars or air-glow. We therefore identify the signal as CIB fluctuations from the faint unresolved galaxies. We show that the present-day galaxies with no evolution would produce a significant deficit in the observed CIB fluctuations. Thus the dominant contribution to th...

  12. Study on Planetary Wave Propagation in the Lower Thermosphere using wind Measurements from Fabry-Perot Interferometers

    Science.gov (United States)

    Otoo Lomotey, Solomon; Meriwether, John; Buriti, Ricardo; Medeiros, Amauri; Paulino, Igo; Barros Silva, Diego

    2016-07-01

    This research is focused on the study of planetary wave propagation in the lower thermosphere. The Fabry-Perot Interferometer (FPI) is a passive optical sensing instrument used to estimate thermospheric winds and temperature. The data used in this paper were captured by the FPIs which are located at São João do Carirri (7.4°S, 36.5°W) and Cajazeiras (6.9ºS, 38.5ºW). The main objective of this research is looking for periodicities in the wind measurements with periods longer than few days in both component of the wind. This was done by using airglow emission of Atomic Oxygen OI630nm in the red line during the nighttime, i.e., from 20:00 to 03:00 local time (LT). Lomb-Scargle analysis was used to process the thermospheric winds and temperature. Phases (time of maximum) and amplitudes of these oscillations were estimated by using Least Square fitting method (LSF), almost all of periodicities propagation of planetary waves was above 2 days for the Zonal and Meriodional winds. A strong oscillation of quasi eight days were observed from September to December 2003

  13. Correlations of mesospheric winds with subtle motion of the Arctic polar vortex

    Directory of Open Access Journals (Sweden)

    Y. Bhattacharya

    2009-08-01

    Full Text Available This paper investigates the relationship between high latitude upper mesospheric winds and the state of the stratospheric polar vortex in the absence of major sudden stratospheric warmings. A ground based Michelson Interferometer stationed at Resolute Bay (74°43´ N, 94°58´ W in the Canadian High Arctic is used to measure mesopause region neutral winds using the hydroxyl (OH Meinel-band airglow emission (central altitude of ~85 km. These observed winds are compared to analysis winds in the upper stratosphere during November and December of 1995 and 1996; years characterized as cold, stable polar vortex periods. Correlation of mesopause wind speeds with those from the upper stratosphere is found to be significant for the 1996 season when the polar vortex is subtly displaced off its initial location by a strong Aleutian High. These mesopause winds are observed to lead stratospheric winds by approximately two days with increasing (decreasing mesospheric winds predictive of decreasing (increasing stratospheric winds. No statistically significant correlations are found for the 1995 season when there is no such displacement of the polar vortex.

  14. Propagation of short-period gravity waves at high-latitudes during the MaCWAVE winter campaign

    Directory of Open Access Journals (Sweden)

    K. Nielsen

    2006-07-01

    Full Text Available As part of the MaCWAVE (Mountain and Convective Waves Ascending Vertically winter campaign an all-sky monochromatic CCD imager has been used to investigate the properties of short-period mesospheric gravity waves at high northern latitudes. Sequential measurements of several nightglow emissions were made from Esrange, Sweden, during a limited period from 27–31 January 2003. Coincident wind measurements over the altitude range (~80–100 km using two meteor radar systems located at Esrange and Andenes have been used to perform a novel investigation of the intrinsic properties of five distinct wave events observed during this period. Additional lidar and MSIS model temperature data have been used to investigate their nature (i.e. freely propagating or ducted. Four of these extensive wave events were found to be freely propagating with potential source regions to the north of Scandinavia. No evidence was found for strong orographic forcing by short-period waves in the airglow emission layers. The fifth event was most unusual exhibiting an extensive, but much smaller and variable wavelength pattern that appeared to be embedded in the background wind field. Coincident wind measurements indicated the presence of a strong shear suggesting this event was probably due to a large-scale Kelvin-Helmholtz instability.

  15. Correlations of mesospheric winds with subtle motion of the Arctic polar vortex

    Directory of Open Access Journals (Sweden)

    Y. Bhattacharya

    2010-01-01

    Full Text Available This paper investigates the relationship between high latitude upper mesospheric winds and the state of the stratospheric polar vortex in the absence of major sudden stratospheric warmings. A ground based Michelson Interferometer stationed at Resolute Bay (74°43' N, 94°58' W in the Canadian High Arctic is used to measure mesopause region neutral winds using the hydroxyl (OH Meinel-band airglow emission (central altitude of ~85 km. These observed winds are compared to analysis winds in the upper stratosphere during November and December of 1995 and 1996; years characterized as cold, stable polar vortex periods. Correlation of mesopause wind speeds with those from the upper stratosphere is found to be significant for the 1996 season when the polar vortex is subtly displaced off its initial location by a strong Aleutian High. These mesopause winds are observed to lead stratospheric winds by approximately two days with increasing (decreasing mesospheric winds predictive of decreasing (increasing stratospheric winds. No statistically significant correlations are found for the 1995 season when there is no such displacement of the polar vortex.

  16. Spectroscopy of the extreme ultraviolet dayglow at 6.5A resolution - Atomic and ionic emissions between 530 and 1240A

    Science.gov (United States)

    Gentieu, E. P.; Feldman, P. D.; Meier, R. R.

    1979-01-01

    EUV spectra (530-1500A) of the day airglow in up, down and horizontal aspect orientations have been obtained with 6.5A resolution and a limiting sensitivity of 5R from a rocket experiment. Below 834A the spectrum is rich in previously unobserved OII transitions connecting with 4S(0), 2D(0), and 2P(0) states. Recent broad-band photometric observations of geocoronal HeI 584A emission in terms of the newly observed OII emissions are shown. The OI 989A and OI 1304A emissions exhibit similar dependence on altitude and viewing geometry with the OI 989A brightness 1/15 that of OI 1340. Emission at 1026A is identified as geocoronal HI Lyman beta rather than OI multiplet emission and observed intensities agree well with model estimates. An unexpectedly high NI 1200/NI 1134A brightness ratio is evidence of a significant contribution from photodissociative excitation of N2 to the NI 1200A source function.

  17. Sky Background Variability Measured on Maunakea at Gemini North Observatory

    Science.gov (United States)

    Smith, Adam B.; Roth, Katherine; Stephens, Andrew W.

    2016-01-01

    Gemini North has recently implemented a Quality Assessment Pipeline (QAP) that automatically reduces images in realtime to determine sky condition quantities, including background sky brightness from the optical to near-infrared. Processing archived images through the QAP and mining the results allows us to look for trends and systematic issues with the instruments and optics during the first decade of Gemini.Here we present the results of using the QAP calculated values to quantify how airglow affects the background sky brightness of images taken with Gemini's imaging instruments, GMOS and NIRI, as well as searching for other factors that may cause changes in the sky brightness. By investigating the dependence of measured sky brightness as a function of a variety of variables, including time after twilight, airmass, season, distance from the moon, air temperature, etc., we quantify the effect of sky brightness and its impact on the sensitivity of Gemini optical and near-infrared imaging data. These measurements will be used to determine new sky background relationships for Maunakea, and to improve the Gemini Integration Time Calculators (ITCs).

  18. Investigation of a mesospheric bore event over northern China

    Directory of Open Access Journals (Sweden)

    Q. Li

    2013-03-01

    Full Text Available A mesospheric bore event was observed using an OH all-sky airglow imager (ASAI at Xinglong (40.2° N, 117.4° E, in northern China, on the night of 8–9 January 2011. Simultaneous observations by a Doppler meteor radar, a broadband sodium lidar, and TIMED/SABER OH intensity and temperature measurements are used to investigate the characteristics and environment of the bore propagation and the possible relations with the Na density perturbations. The bore propagated from northeast to southwest and divided the sky into bright and dark halves. The calculations show that the bore has an average phase velocity of 68 m s−1. The crests following the bore have a horizontal wavelength of ~ 22 km. These parameters are consistent with the hydraulic jump theory proposed by Dewan and Picard, as well as the previous bore reports. Simultaneous wind measurements from the Doppler meteor radar at Shisanling (40.3° N, 116.2° E and temperature data from SABER on board the TIMED satellite are used to characterize the propagating environment of the bore. The result shows that a thermal-Doppler duct exists near the OH layer that supports the horizontal propagation of the bore. Simultaneous Na lidar observations at Yanqing (40.4° N, 116.0° E suggest that there is a downward displacement of Na density during the passage of the mesospheric bore event.

  19. New Horizons Constraints on Charon's Present Day Atmosphere

    CERN Document Server

    Stern, S A; Gladstone, G R; Steffl, A J; Cheng, A F; Young, L A; Weaver, H A; Olkin, C B; Ennico, K; Parker, J W; Parker, A H; Lauer, T R; Zangari, A; Summers, M

    2016-01-01

    We report on a variety of standard techniques used by New Horizons including a solar ultraviolet occultation, ultraviolet airglow observations, and high-phase look-back particulate search imaging to search for an atmosphere around Pluto's large moon Charon during its flyby in July 2015. Analyzing these datasets, no evidence for a present day atmosphere has been found for 14 potential atomic and molecular species, all of which are now constrained to have pressures below 0.3 nanobar, as we describe below, these are much more stringent upper limits than the previously available 15-110 nanobar constraints (e.g., Sicardy et al. 2006); for example, we find a 3$\\sigma$ upper limit for an N$_2$ atmosphere on Charon is 4.2 picobars and a 3$\\sigma$ upper limit for the brightness of any atmospheric haze on Charon of I/F=2.6x10$^{-5}$. A radio occultation search for an atmosphere around Charon was also conducted by New Horizons but will be published separately by other authors.

  20. Ionospheric effects of rocket exhaust products (HEAO-C, Skylab and SPS-HLLV)

    Energy Technology Data Exchange (ETDEWEB)

    Zinn, J; Sutherland, D; Stone, S N; Duncan, L M; Behnke, R

    1980-10-01

    This paper reviews the current state of our understanding of the problem of ionospheric F-layer depletions produced by chemical effects of the exhaust gases from large rockets, with particular emphasis on the Heavy Lift Launch Vehicles (HLLV) proposed for use in the construction of solar power satellites. The currently planned HLLV flight profile calls for main second-stage propulsion confined to altitudes below 124 km, and a brief orbit-circularization maneuver at apogee. The second-stage engines deposit 9 x 10/sup 31/ H/sub 2/O and H/sub 2/ molecules between 56 and 124 km. Model computations show that they diffuse gradually into the ionospheric F region, where they lead to weak but widespread and persistent depletions of ionization and continuous production of H atoms. The orbit-circularization burn deposits 9 x 10/sup 29/ exhaust molecules at about 480-km altitude. These react rapidly with the F2 region 0/sup +/ ions, leading to a substantial (factor-of-three) reduction in plasma density, which extends over a 1000- by 2000-km region and persists for four to five hours. Also described are experimental airglow and incoherent-scatter radar measurements performed in conjunction with the 1979 launch of satellite HEAO-C, together with prelaunch and post-launch computations of the ionospheric effects. Several improvements in the model have been driven by the experimental observations. The computer model is described in some detail.

  1. Voyager Ultraviolet Spectrometers calibration and the heliosphere neutrals composition: reassessment

    CERN Document Server

    Ben-Jaffel, Lotfi

    2016-01-01

    The Voyagers (V) 1 and 2 Ultraviolet Spectrometers (UVS) data harvest covers outer planets encounters, heliosphere sky-background measurements, and stellar spectrophotometry. Because their operation period overlaps with many ultraviolet missions, the V1 and V2 UVS calibration with other spectrometers are invaluable. Here we revisit the UVS calibration to assess the intriguing 243 % (V1) and 156 % (V2) sensitivity enhancements recently proposed. Using the Saturn Lyman-$\\alpha$ airglow, observed in-situ by both Voyagers, and remotely by IUE, we match the Voyager values to IUE, taking into account the shape of the Saturn Lyman-$\\alpha$ line observed with the Goddard High Resolution Spectrograph onboard the Hubble Space Telescope. For all known ranges of the interplanetary hydrogen density, we show that the V1 and V2 UVS sensitivities cannot be enhanced by the amounts thus far proposed. The same diagnostic holds for distinct channels covering the diffuse HeI 58.4 nm emission. Our prescription is to keep the origi...

  2. Status of development of lightning detector for PLANET-C mission

    Science.gov (United States)

    Takahashi, Y.; Hoshino, N.; Sato, M.; Teraguchi, T.

    2008-12-01

    Magnetometer onboard Venus Express detected whistler mode waves whose source can be considered to be lightning discharge occurring well below the spacecraft orbit. However, there still remain some uncertainties to conclude finally such waves are originated by lightning discharge in the atmosphere. In order to identify the discharge phenomena in the atmosphere of Venus without any doubt, we plan to observe the lightning activity with high-speed optical detector onboard Planet-C, the Japanese Venus Climate Orbiter mission which will be launched in 2010 by JAXA. We are developing a new type of lightning detector, LAC (Lightning and Airglow Camera). Main difference from other equipments which have provided evidences of lightning existence in Venus is the high-speed sampling rate at 50kHz for each pixel, enabling us to distinguish the optical lightning flash from other pulsing noises. On the other hand, spatial resolution is not first priority as the first detector of Venus lightning. New type of APD (avalanche photo diode) array with a format of 8 x 8 is used and a narrow band interference filter at wavelength of 777.4 nm (OI) is selected for lightning measurement. The development is now at the stage for designing and manufacturing the flight model, based on the performance and environmental tolerance of the proto model. Especially, the algorithm for self- triggering is carefully improved in order to exclude false-trigger by other pulse-like noise.

  3. Lightning Detection by LAC Onboard the Japanese Venus Climate Orbiter, Planet-C

    Science.gov (United States)

    Takahashi, Y.; Yoshida, J.; Yair, Y.; Imamura, T.; Nakamura, M.

    2008-06-01

    Lightning activity in Venus has been a mystery for a long period, although many studies based on observations both by spacecraft and by ground-based telescope have been carried out. This situation may be attributed to the ambiguity of these evidential measurements. In order to conclude this controversial subject, we are developing a new type of lightning detector, LAC (Lightning and Airglow Camera), which will be onboard Planet-C (Venus Climate Orbiter: VCO). Planet-C will be launched in 2010 by JAXA. To distinguish an optical lightning flash from other pulsing noises, high-speed sampling at 50 kHz for each pixel, that enables us to investigate the time variation of each lightning flash phenomenon, is adopted. On the other hand, spatial resolution is not the first priority. For this purpose we developed a new type of APD (avalanche photo diode) array with a format of 8×8. A narrow band interference filter at wavelength of 777.4 nm (OI), which is the expected lightning color based on laboratory discharge experiment, is chosen for lightning measurement. LAC detects lightning flash with an optical intensity of average of Earth’s lightning or less at a distance of 3 Rv. In this paper, firstly we describe the background of the Venus lightning study to locate our spacecraft project, and then introduce the mission details.

  4. Imaging Sunlit Aurora from Balloon

    Science.gov (United States)

    Lummerzheim, D.; Zhou, X.

    2012-12-01

    Since 1892 when aurora was first imaged by Martin Brendel, useful auroral images have been obtained only when the aurora is in darkness. While UV imagers onboard satellite provide global auroral dynamics, the sunlit aurora in the UV band is overwhelmed by the UV airglow that has the same wavelengths with the UV auroral emissions. The visible band imaging is feasible only when the aurora is in darkness to avoid the sunlight contamination. However, sunlit aurora (such as dayside aurora) is closely related to the solar wind - magnetosphere - ionosphere coupling. In addition, limited land area has badly restricted the capability of imaging dayside aurora from the northern hemisphere and nightside aurora from the southern hemisphere. We have confirmed that sunlit aurora can be imaged using a near-infrared (NIR) camera on board the balloon platform flying in Antarctica or Arctic. This method provides a unique capability for dayside and conjugate auroral investigations. Scientific questions that can be addressed by such observations include how does the dayside aurora respond to solar wind transient variations? Are auroras hemispherically symmetric? Are auroral forms and their variations under sunlight the same as those in darkness? etc. The new method is also cost effective comparing to space-borne imagers, and offers capabilities not obtainable from space and the ground. With the accomplishment of identifying auroral dynamics in sunlight and darkness, in the south and north simultaneously, our knowledge and understanding of auroral phenomenon and its causes will be expanded.

  5. Concurrent observations at the magnetic equator of small-scale irregularities and large-scale depletions associated with equatorial spread F

    CERN Document Server

    Hickey, D A; Rodrigues, F S; Varney, R H; Milla, M A; Nicolls, M J; Strømme, Anja; Arratia, J F

    2015-01-01

    In 2014 an all-sky imager (ASI) and an Advanced Modular Incoherent Scatter Radar consisting of 14 panels (AMISR-14) system were installed at the Jicamarca Radio Observatory. The ASI measures airglow depletions associated with large-scale equatorial spread F irregularities (10s-100s km), while AMISR-14 detects small-scale irregularities (0.34 m). This study presents simultaneous observations of equatorial spread F (ESF) irregularities at 10-100 km scales using the all sky-imager, at 3 m scales using the JULIA (Jicamarca Unattended Long-term Investigations of the Ionosphere and Atmosphere) radar, and at 0.34 m scales using the AMISR-14 radar. We compare data from the three instruments on the night of 20-21 August, 2014 by locating the radar scattering volume in the optical images. During this night no topside plumes were observed, and we only compare with bottomside ESF. AMISR-14 had five beams perpendicular to the magnetic field covering ~200 km in the east-west direction at 250 km altitude. Comparing the rada...

  6. Magnetospheric effects of ion and atom injections by the satellite power system

    Energy Technology Data Exchange (ETDEWEB)

    Chiu, Y.T.; Luhmann, J.G.; Schulz, M.; Cornwall, J.M.

    1980-07-01

    This is the final report of a two-year assessment of magnetospheric effects of the construction and operation of a satellite power system. This assessment effort is based on application of present scientific knowledge rather than on original scientific research. As such, it appears that mass and energy injections of the system are sufficient to modify the magnetosphere substantially, to the extent of possibly requiring mitigation measures for space systems but not to the extent of causing major redirection of efforts and concepts. The scale of the SPS is so unprecedentedly large, however, that these impressions require verification (or rejection) by in-depth assessment based on original scientific treatment of the principal issues. Indeed, it is perhaps appropriate to state that present ignorance far exceeds present knowledge in regard to SPS magnetospheric effects, even though we only seek to define the approximate limits of magnetospheric modifications here. Modifications of the space radiation environment, of the atmospheric airglow background, of the auroral response to solar activity and of the fluctuations in space plasma density are identified to be the principal impacts.

  7. Global Observations of the 630-nm Nightglow and Patterns of Brightness Measured by ISUAL

    Directory of Open Access Journals (Sweden)

    Chih-Yu Chiang

    2013-01-01

    Full Text Available This study investigates the distributions and occurrence mechanisms of the global local-midnight airglow brightness through FORMOSAT-2/ISUAL satellite imaging observations. We focus on the OI 630.0 nm nightglow emission at altitudes of ~250 km along equatorial space. The database used in this study included data from 2007 to 2008 under solar minimum conditions. The data were classified into four specified types in the statistical study. We found that the occurrence of equatorial brightness was often in the vicinity of the geographic equator and mostly at equinoxes with a tendency to move toward the summer hemisphere as the season changes. Conjugate brightness occurring simultaneously on both sides of the geomagnetic equator was observed predominantly in the northern winter. Furthermore, midnight brightness appeared to have lower luminosity from May to July. We suggest that the global midnight brightness associated with the locations and seasons was the result of several effects which include the influence of the thermospheric midnight temperature maximum (MTM, summer-to-winter neutral wind, and ionospheric anomalies.

  8. Spectroscopy of diffuse light in dust clouds. Scattered light and the solar neighbourhood radiation field

    CERN Document Server

    Lehtinen, K

    2012-01-01

    The optical surface brightness of dark nebulae is mainly due to scattering of integrated starlight by classical dust grains. It contains information on the impinging interstellar radiation field, cloud structure, and grain scattering properties. We have obtained spectra of the scattered light from 3500 to 9000 Angstrom in two globules, the Thumbprint Nebula and DC303.8-14.2. We use observations of the scattered light to study the impinging integrated starlight spectrum as well as the scattered H-alpha and other line emissions from all over the sky. We search also for the presence of other than scattered light in the two globules. We obtained long-slit spectra encompassing the whole globule plus adjacent sky in a one-slit setting, thus enabling efficient elimination of airglow and other foreground sky components. We calculated synthetic integrated starlight spectra for the solar neighbourhood using HIPPARCOS-based stellar distributions and the spectral library of Pickles. Spectra are presented separately for t...

  9. WINDII on UARS in the context of SCISAT and Odin

    Science.gov (United States)

    Shepherd, Gordon G.

    2017-01-01

    The fundamental elements of the atmosphere are its energy input, composition, temperature and dynamics. Of these the dynamics have had the least observational investigation because of the difficulty of the measurement of winds through optical remote sensing. This article reviews one approach to this topic, the application of the Doppler Michelson Interferometer, focusing on one particular instrument, the Wind Imaging Interferometer (WINDII) flown on NASA's Upper Atmosphere Research Satellite (UARS) from 1991 to 2003. With this concept, the wind is measured through the phase shifts of a single fringe from a Michelson interferometer set to an appropriately large optical path difference, determined by phase stepping over that fringe. This configuration allows the implementation of field-widening, allowing the measurements to be made over a wide field, providing wind images extending from roughly 80 km to 300 km altitude. The Doppler target is the day and night airglow of the upper atmosphere, whose emission rates provide valuable information about the composition of the atmosphere and whose wavelength shifts provide the Doppler information. The primary result, not fully predicted, was the observation of the influence of the dynamics on the composition of the atmosphere. This review provides a minimal instrumentation description, but adequate references, and concentrates on the larger picture of how these data contribute to understanding the interactions of composition, temperature and dynamics, in the context of the SCISAT and Odin measurements. Some new results presented indicate future directions, yet to be explored in full.

  10. Directional Filtering Due to Mesospheric Wind Shear on the Propagation of Acoustic-gravity Waves

    Institute of Scientific and Technical Information of China (English)

    YU Yonghui; CHEN Wei; WANG Yachong

    2013-01-01

    Gravity waves with periods close to the Brunt-V(a)is(a)l(a) period of the upper troposphere are often observed at mesopause altitudes as short period,quasi-monochromatic waves.The assumption that these short period waves originate in the troposphere may be problematic because their upward propagation to the mesosphere and lower thermosphere region could be significantly impeded due to an extended region of strong evanescence above the stratopause.To reconcile this apparent paradox,an alternative explanation is proposed in this paper.The inclusion of mean winds and their vertical shears is sufficient to allow certain short period waves to remain internal above the stratopause and to propagate efficiently to higher altitudes.A time-dependent numerical model is used to demonstrate the feasibility of this and to determine the circumstances under which the mesospheric wind shears play a role in the removal and directional filtering of short period gravity waves.Finally this paper concludes that the combination of the height-dependent mean winds and the mean temperature structure probably explains the existence of short period,quasi-monochromatic structures observed in airglow images of mesopause region.

  11. Observation and modeling of gravity wave propagation through reflection and critical layers above Andes Lidar Observatory at Cerro Pachón, Chile

    Science.gov (United States)

    Cao, Bing; Heale, Christopher J.; Guo, Yafang; Liu, Alan Z.; Snively, Jonathan B.

    2016-11-01

    A complex gravity wave event was observed from 04:30 to 08:10 UTC on 16 January 2015 by a narrow-band sodium lidar and an all-sky airglow imager located at Andes Lidar Observatory (ALO) in Cerro Pachón (30.25°S, 70.73°W), Chile. The gravity wave packet had a period of 18-35 min and a horizontal wavelength of about 40-50 km. Strong enhancements of the vertical wind perturbation, exceeding 10 m s-1, were found at ˜90 km and ˜103 km, consistent with nearly evanescent wave behavior near a reflection layer. A reduction in vertical wavelength was found as the phase speed approached the background wind speed near ˜93 km. A distinct three-layered structure was observed in the lidar data due to refraction of the wave packet. A fully nonlinear model was used to simulate this event, which successfully reproduced the amplitudes and layered structure seen in observations. The model results provide dynamical insight, suggesting that a double reflection occurring at two separate heights caused the large vertical wind amplitudes, while the three-layered structure in the temperature perturbation was a result of relatively stable regions at those altitudes. The event provides a clear perspective on the filtering processes to which short-period, small-scale gravity waves are subject in mesosphere and lower thermosphere.

  12. Mesospheric gravity waves observed near equatorial and low–middle latitude stations: wave characteristics and reverse ray tracing results

    Directory of Open Access Journals (Sweden)

    E. Achmad

    2006-12-01

    Full Text Available Gravity wave signatures were extracted from OH airglow observations using all-sky CCD imagers at four different stations: Cachoeira Paulista (CP (22.7° S, 45° W and São João do Cariri (7.4° S, 36.5° W, Brazil; Tanjungsari (TJS (6.9° S, 107.9° E, Indonesia and Shigaraki (34.9° N, 136° E, Japan. The gravity wave parameters are used as an input in a reverse ray tracing model to study the gravity wave vertical propagation trajectory and to estimate the wave source region. Gravity waves observed near the equator showed a shorter period and a larger phase velocity than those waves observed at low-middle latitudes. The waves ray traced down into the troposphere showed the largest horizontal wavelength and phase speed. The ray tracing results also showed that at CP, Cariri and Shigaraki the majority of the ray paths stopped in the mesosphere due to the condition of m2m2m|→∞, which suggests the presence of ducting waves and/or waves generated in-situ. In the troposphere, the possible gravity wave sources are related to meteorological front activities and cloud convections at CP, while at Cariri and TJS tropical cloud convections near the equator are the most probable gravity wave sources. The tropospheric jet stream and the orography are thought to be the major responsible sources for the waves observed at Shigaraki.

  13. Multi-instrument investigation of a mesospheric gravity wave event absorbed into background

    Science.gov (United States)

    Sivakandan, M.; Taori, A.; Sathishkumar, S.; Jayaraman, A.

    2015-04-01

    We investigate a gravity wave event exhibiting dissipation noted in the mesospheric O(1S) airglow emission image measurements, over Gadanki (13.5°N, 79.2°E), on 16 March 2012 (during 16:20-16:45 UT). These gravity waves were found to propagate from south-west to north-east directions at ~65° azimuth in OH as well as in O(1S) images. These waves had horizontal wavelength ~21.5 km with apparent horizontal phase speed ~49 m s-1 and period ~7.3 min. These waves were noted to fizzle out in turbulent patches within 15 min. To identify the causative mechanism of this event, we analyze the background wind and temperature data using the medium-frequency radar wind from Tirunelveli (8.7°N, 77.8°E), ground-based Rayleigh lidar temperature data with improved capability over Gadanki, and spaceborne Sounding of the Atmosphere using Broadband Emission Radiometry/Thermosphere Ionosphere Mesosphere Energetics and Dynamics temperature data (20:30 UT) for a latitude-longitude grid of 3-23°N, 60-100°E. Our analysis reveals that convective instability was responsible for the observed event.

  14. Quality studies of the data taking conditions for the Auger fluorescence detector

    Energy Technology Data Exchange (ETDEWEB)

    Caruso, R.; Fonte, R.; Insolia, A.; Petrera, S.; Rodriquez Martino, J.; /Rome U.,Tor Vergata

    2005-07-01

    As more than half of the Fluorescence Detector (FD) of the Auger Observatory is completed, data taking is becoming a routine job. It is then necessary to follow strict procedures to assure the quality of the data. An overview of the data taking methods is given. The nature of the FD background signal is due to the night sky brightness (stars and planet faint light, moonlight, twilight, airglow, zodiacal and artificial light) and to the electronic background (photomultiplier and electronic noise). The analysis of the fluctuations in the FADC signal (variance analysis), directly proportional to the background mean light level, performed for each night of data taking is used to monitor the FD background signal. The data quality is analyzed using different techniques, described in detail. Examples of trigger rates, number of stereo events, dead time due to moonlight, weather or hardware problems are given. The analysis comprises several months of data taking, giving an overview of the FD capabilities, performance and allowing a systematic study of data and their correlation with the environment.

  15. An Overview of High-Altitude Balloon Experiments at the Indian Institute of Astrophysics

    CERN Document Server

    Safonova, Margarita; Sreejith, A G; Mathew, Joice; Sarpotdar, Mayuresh; Ambily, S; Nirmal, K; Talnikar, Sameer; Hadigal, Shripathy; Prakash, Ajin; Murthy, Jayant

    2016-01-01

    The High-Altitude Ballooning programme began at Indian Institute of Astrophysics, Bangalore, in the year 2011 with the primary purpose of developing and flying low-cost scientific payloads on a balloon-borne platform. Some of the science goals are studies of the phenomena occurring in the upper atmosphere, of airglow and zodiacal light, and observations of extended astronomical objects such as, for example, comets, from near space (20 to 30 km). A brief summary and results of the tethered flights carried out at CREST campus are given in Ref.~1. Here we present a complete overview of the 9 free-flying balloon experiments conducted from March 2013 to November 2014. We describe the launch procedures, payloads, methods of tracking and recovery of the payloads. Since we fall in the light/medium balloon category, the weight of the payload is limited to less than 5 kg --- we use a 3-D printer to fabricate lightweight boxes and structures for our experiments. We are also developing in-house lightweight sensors and co...

  16. Atmospheric Photochemistry

    Science.gov (United States)

    Massey, Harrie; Potter, A. E.

    1961-01-01

    The upper atmosphere offers a vast photochemical laboratory free from solid surfaces, so all reactions take place in the gaseous phase. At 30 km altitude the pressure has fallen to about one-hundredth of that at ground level, and we shall, rather arbitrarily, regard the upper atmosphere as beginning at that height. By a little less than 100 km the pressure has fallen to 10(exp -3) mm Hg and is decreasing by a power of ten for every 15 km increase in altitude. Essentially we are concerned then with the photochemistry of a nitrogen-oxygen mixture under low-pressure conditions in which photo-ionization, as well as photodissociation, plays an important part. Account must also be taken of the presence of rare constituents, such as water vapour and its decomposition products, including particularly hydroxyl, oxides of carbon, methane and, strangely enough, sodium, lithium and calcium. Many curious and unfamiliar reactions occur in the upper atmosphere. Some of them are luminescent, causing the atmosphere to emit a dim light called the airglow. Others, between gaseous ions and neutral molecules, are almost a complete mystery at this time. Similar interesting phenomena must occur in other planetary atmospheres, and they might be predicted if sufficient chemical information were available.

  17. Vertical Distribution of Vibrationally Excited Hydroxyl

    Science.gov (United States)

    Grygalashvyly, Mykhaylo; Becker, Erich; Sonnemann, Gerd

    2016-04-01

    Knowledge about the vertical distribution of the vibrationally excited states of hydroxyl (OH*) is important for the interpretation of airglow measurements with respect to dynamical processes in the mesopause region. We derive an approximate analytical expression for the distribution of OH* that highlights the dependence on atomic oxygen and temperature. In addition, we use an advanced numerical model for the formation and relaxation of OH* and investigate the distributions of the different vibrationally exited states of OH*. For the production of OH*, the model includes the reaction of atomic hydrogen with ozone, as well as the reaction of atomic oxygen with hydroperoxy radicals. As loss processes we include 1) deactivation by atomic oxygen, molecular oxygen, and molecular nitrogen, 2) spontaneous emission, and 3) loss due to chemical reaction with atomic oxygen. All these processes take the dependence on the vibrational number into account. The quenching by molecular and atomic oxygen is parameterized by a multi-quantum relaxation scheme. This diagnostic model for OH* has been implemented as part of a chemistry-transport model that is driven by the dynamics simulated with the KMCM (Kühlungsborn Mechanistic general Circulation Model). Numerical results confirm that emission from excited states with higher vibrational number is weaker and emanates from higher altitudes. In addition we find that the OH*-peak altitudes depend significantly on season and latitude. This behavior is mainly controlled by the corresponding variations of atomic oxygen and temperature, as is also confirmed by the aforementioned approximate theory.

  18. Obituary: Joseph Wyan Chamberlain, 1928-2004

    Science.gov (United States)

    Hunten, Donald M.

    2004-12-01

    are glad that his last nineteen active years were spent in that role. In the 1960's the AAS had no Division for Planetary Sciences (DPS), and the group organized an annual series of five Arizona Conferences on Planetary Atmospheres. By 1967 several members of the community felt that a DPS was needed; the AAS Council asked Joe to serve as chair of the organizing committee, and when the Division was formed he became the first Chairman. In 1971, he became Director of the NASA Lunar Science Institute and a few years later Professor of Space Physics and Astronomy at Rice University (Houston). After retirement as Professor Emeritus in 1992, he returned to Tucson where he continued an active interest in golf, opera, chess and satirical humor. Joe's program at Yerkes began with observations of aurora and airglow, making use of the wonderful spectrographs designed and built by Meinel. Among his many contributions was the identification and analysis of a band system in the airglow that now bears his name. His interests shifted toward the theoretical; for example, he applied the radiative-transfer theory of his colleague Chandrasekhar to the sodium twilight airglow. In 1961 he published Theory of the Aurora and Airglow, a book so influential that it was reprinted a few years ago by the American Geophysical Union. In the same period his interest in interplanetary hydrogen led to a low-velocity model that was at odds with Eugene N. Parker's model of the solar wind, and a debate ensued until observations showed Parker to be essentially correct. But the Chamberlain ideas were applied to the structure of the Earth's hydrogen exosphere, and for 40 years this work has been accepted as definitive. Later he studied the reduction of the hydrogen escape rate by the "cooling" that results from the loss of the energy carried by the escaping atoms. Joe was selected to deliver the 1961 Helen Warner lecture and chose the topic "The upper atmospheres of the planets." This paper clearly expounds

  19. Simultaneous Observations of Mesoscale Gravity Waves Over the Central US with CRRL Na Doppler Lidars and USU Temperature Mapper

    Science.gov (United States)

    Lu, Xian; Chen, Cao; Huang, Wentao; Smith, John A.; Zhao, Jian; Chu, Xinzhao; Yuan, Tao; Pautet, Pierre-Dominique; Taylor, Mike J.

    2016-06-01

    We present the first coordinated study of a 1-h mesoscale gravity wave event detected simultaneously by a Na Doppler lidar at Boulder, CO (40.1°N, 105.2°W), and a Na Doppler lidar and an airglow temperature mapper (AMTM) at Logan, UT (41.7°N, 111.8°W) in the mesopause region on 27 Nov. 2013. The vertical and horizontal wavelengths are ~16.0±0.3 and 342.0±10.4 km, corresponding to vertical and horizontal phase speeds of ~4.4±0.1 and 95.0±3.0 m/s, respectively. The wave propagates from Logan to Boulder with an azimuth angle of ~138.1±1.7° clockwise from North. A uniqueness of this study is that the 1-h wave amplitudes on vertical winds have been quantified for the first time by the STAR Na lidar at Boulder. The GW polarization relation between vertical wind and temperature is evaluated. The intrinsic period of the wave is Doppler shifted to ~100 min by a background wind of 40 m/s, which is confirmed by USU lidar wind observations. This study illustrates a great potential of combining multiple instruments to fully characterize mesoscale gravity waves and inspect their intrinsic properties

  20. Direct Numerical Simulations of Small-Scale Gravity Wave Instability Dynamics in Variable Stratification and Shear

    Science.gov (United States)

    Mixa, T.; Fritts, D. C.; Laughman, B.; Wang, L.; Kantha, L. H.

    2015-12-01

    Multiple observations provide compelling evidence that gravity wave dissipation events often occur in multi-scale environments having highly-structured wind and stability profiles extending from the stable boundary layer into the mesosphere and lower thermosphere. Such events tend to be highly localized and thus yield local energy and momentum deposition and efficient secondary gravity wave generation expected to have strong influences at higher altitudes [e.g., Fritts et al., 2013; Baumgarten and Fritts, 2014]. Lidars, radars, and airglow imagers typically cannot achieve the spatial resolution needed to fully quantify these small-scale instability dynamics. Hence, we employ high-resolution modeling to explore these dynamics in representative environments. Specifically, we describe numerical studies of gravity wave packets impinging on a sheet of high stratification and shear and the resulting instabilities and impacts on the gravity wave amplitude and momentum flux for various flow and gravity wave parameters. References: Baumgarten, Gerd, and David C. Fritts (2014). Quantifying Kelvin-Helmholtz instability dynamics observed in noctilucent clouds: 1. Methods and observations. Journal of Geophysical Research: Atmospheres, 119.15, 9324-9337. Fritts, D. C., Wang, L., & Werne, J. A. (2013). Gravity wave-fine structure interactions. Part I: Influences of fine structure form and orientation on flow evolution and instability. Journal of the Atmospheric Sciences, 70(12), 3710-3734.

  1. Excitation of the CO fourth positive system by the dissociative recombination of CO2/+/ ions.

    Science.gov (United States)

    Gutcheck, R. A.; Zipf, E. C.

    1973-01-01

    The fourth positive system of CO has been excited in a static afterglow experiment by the dissociative recombination of CO2(+) ions. From combined absolute optical and microwave measurements the specific recombination coefficient for exciting the CO system was found to be (2 plus 1 or minus 0.5) x 10 to the minus 8th cu cm/sec. This value represents approximately 5% of the total recombination coefficient (4.0 plus or minus 0.5) x 10 to the minus 7th cu cm/sec measured in this experiment, implying that CO2(+) dissociative recombination will contribute significantly to the excitation of the CO fourth positive system in the Martian airglow. Corroborative electron heating experiments showed that the magnitude of the specific recombination coefficient decreased as the electron temperature was increased. Evidence was also found for the presence of vibrationally excited ions in the CO2(+) plasma, a result which indicates that analogous laboratory studies on the dissociative recombination of O2(+), N2(+), and NO(+) ions may have also involved vibrationally hot plasmas.

  2. Experimentally investigate ionospheric depletion chemicals in artificially created ionosphere

    Energy Technology Data Exchange (ETDEWEB)

    Liu Yu; Cao Jinxiang; Wang Jian; Zheng Zhe; Xu Liang; Du Yinchang [CAS Key Laboratory of Basic Plasma Physics, Department of Modern Physics, University of Science and Technology of China, Hefei, Anhui 230026 (China)

    2012-09-15

    A new approach for investigating ionosphere chemical depletion in the laboratory is introduced. Air glow discharge plasma closely resembling the ionosphere in both composition and chemical reactions is used as the artificially created ionosphere. The ionospheric depletion experiment is accomplished by releasing chemicals such as SF{sub 6}, CCl{sub 2}F{sub 2}, and CO{sub 2} into the model discharge. The evolution of the electron density is investigated by varying the plasma pressure and input power. It is found that the negative ion (SF{sub 6}{sup -}, CCl{sub 2}F{sub 2}{sup -}) intermediary species provide larger reduction of the electron density than the positive ion (CO{sub 2}{sup +}) intermediary species. The negative ion intermediary species are also more efficient in producing ionospheric holes because of their fast reaction rates. Airglow enhancement attributed to SF{sub 6} and CO{sub 2} releases agrees well with the published data. Compared to the traditional methods, the new scheme is simpler to use, both in the release of chemicals and in the electron density measurements. It is therefore more efficient for investigating the release of chemicals in the ionosphere.

  3. First experiment of spectrometric observation of hydroxyl emission and rotational temperature in the mesopause in China

    Institute of Scientific and Technical Information of China (English)

    ZHU YaJun; XU JiYao; YUAN Wei; LIU Xiao

    2012-01-01

    A SpectroMeter of Atmospheric RadiaTion (SMART) was developed and installed at the Xinglong station of the National Astronomical Observatories in Hebei province,China,which was supported by the Meridian Project [ 1].The experimental tests of spectrometric observation of the hydroxyl emission and rotational temperature in China were conducted for the first time on the night of February 23,2011 and the night of April 27,2011,respectively.OH 6-2 band and OH 8-3 band spectra were measured and the rotational temperature was retrieved.Hourly average temperatures (186.82+-6.40) K of OH 8-3 band and (178.07±6.73) K of OH 6-2 band were derived from the spectra observed on the night of February 23,2011.Intensities and rotational temperature against local time were determined by the spectra measured in the whole night of April 27,2011.The rotational temperature was consistent with the spatial average temperature of NRLMSISE00 empirical model at height 83-91 km and the average temperature of TIMED/SABER from April to May of seven years at height 83-91 km,with some discrepancies.The results showed that the new instrument and the retrieval method of the rotational temperature can give reasonable results of the airglow emission of OH and the temperature of mesopause.

  4. GALEX Observations of Diffuse UV Radiation at High Spatial Resolution from the Sandage Nebulosity

    CERN Document Server

    Sujatha, N V; Karnataki, Abhay; Henry, Richard Conn; Bianchi, Luciana

    2008-01-01

    Using the GALEX ultraviolet imagers we have observed a region of nebulosity first identified as starlight scattered by interstellar dust by Sandage (1976). Apart from airglow and zodiacal emission, we have found a diffuse UV background of between 500 and 800 \\phunit in both the \\galex FUV (1350 -- 1750 \\AA) and NUV (1750 -- 2850 \\AA). Of this emission, up to 250 \\phunit is due to \\htwo fluorescent emission in the FUV band; the remainder is consistent with scattering from interstellar dust. We have estimated the optical constants to be $a = 0.3; g = 0.7$ in the FUV and $a = 0.5; g = 0.7$ in the NUV, implying highly forward scattering grains, plus an extragalactic contribution of as much as 150 \\phunit. These are the highest spatial resolution observations of the diffuse UV background to date and show an intrinsic scatter beyond that expected from instrumental noise alone. Further modeling is required to understand the nature of this scatter and its implications for the ISM.

  5. Characteristics of Mesospheric Gravity Waves Observed in the Central Region of Brazil

    Science.gov (United States)

    Wrasse, Cristiano Max; Messias Almeida, Lazaro; Abalde Guede, Jose Ricardo; Valentin Bageston, José; Pillat, Valdir G.; Lima, Washington L. C.

    Gravity waves observations were carried out at Palmas (10.16o S, 48.26o W) Brazil, between September 2007 and December 2008, using an all-sky airglow imager to measure the OH emis-sion. The gravity waves were divided in two groups following they morphology as band and ripples type waves. The main characteristics of the band type waves are: horizontal wavelength between 10-35 km; observed period raging from 5 to 25 minutes; observed phase speed between 5-60 m/s. Preferential propagation directions of the bands are northward and southward, show-ing a clear anisotropy. For the ripples the main wave parameters are: horizontal wavelength ranging between 5 and 15 km; observed period mainly distributed between 5 and 15 minutes and horizontal phase velocity from 5 to 30 m/s. The ripples showed the same anisotropy as in the preferential propagation direction as the band type waves. The gravity wave characteristics observed at Palmas were compared with other observations carried out in Brazil, showing simi-lar features. In order to explain the seasonal variation of the wave propagation direction, maps of Outgoing Longwave Radiation (ORL) were used to locate regions with intense deep con-vection (OLR < 220 W.m-2 ) in the lower atmosphere. During summer and autumn the wave sources regions are well correlated with deep convection areas located at west and northwest of Palmas.

  6. Analysis of rocket beacon transmissions for computerized reconstruction of ionospheric densities

    Science.gov (United States)

    Bernhardt, P. A.; Huba, J. D.; Chaturvedi, P. K.; Fulford, J. A.; Forsyth, P. A.; Anderson, D. N.; Zalesak, S. T.

    1993-08-01

    Three methods are described to obtain ionospheric electron densities from transionospheric, rocket-beacon TEC data. First, when the line-of-sight from a ground receiver to the rocket beacon is tangent to the flight trajectory, the electron concentration can be obtained by differentiating the TEC with respect to the distance to the rocket. A similar method may be used to obtain the electron-density profile if the layer is horizontally stratified. Second, TEC data obtained during chemical release experiments may be interpreted with the aid of physical models of the disturbed ionosphere to yield spatial maps of the modified regions. Third, computerized tomography (CT) can be used to analyze TEC data obtained along a chain of ground-based receivers aligned along the plane of the rocket trajectory. CT analysis of TEC data is used to reconstruct a 2D image of a simulated equatorial plume. TEC data is computed for a linear chain of nine receivers with adjacent spacings of either 100 or 200 km. The simulation data are analyzed to provide an F region reconstruction on a grid with 15 x 15 km pixels. Ionospheric rocket tomography may also be applied to rocket-assisted measurements of amplitude and phase scintillations and airglow intensities.

  7. Simulation on volume emission rate at OIRA band based on photochemical model%利用光化学模型的氧红外大气波段体发射率模拟

    Institute of Scientific and Technical Information of China (English)

    汪自军; 陈圣波

    2011-01-01

    基于光化学模型模拟氧红外大气(OIRA)波段1.27μm气辉体发射率(VER),是利用临边OIRA波段卫星数据反演中间层臭氧浓度一个重要的过程.从奇氧族光化学反应出发,基于大气动力学和光化学理论,建立了O2(a1△g)的光化学模型.通过太阳辐射模拟值,解算了光化学反应系数,进而进行了Odin卫星轨道面内气辉VER的模拟.结果表明,白天气辉VER一般数量级达到106,峰值出现在50~55km高度范围,而黑夜VER几乎为0.且随天顶角增大,VER达到峰值的高度增大.与利用Odin OSIRIS IR Levell数据反演的同时间VER剖面相比,VER剖面在数值量级、二维结构特征和衰减变化时间点方面,有很高的一致性.而且高纬地区比低纬地区一致性高,特别是80~100km之间稳合度最高,证明使用建立的光化学模型能够反演高纬度地区中间层臭氧.%Simulation on 1.27 μm airglow volume emission rate (VER) is an indispensable aspect for inversion of mesospheric ozone concentration from satellite measurement in the near oxygen infrared atmospheric (OIRA) band. In this study, the photochemical reactions of odd oxygen family were reviewed.A photochemical model of O2 (a1△g) was established based on the atmospheric kinetics and photochemistry.The photochemical index were solved from the modeled solar fluxes, and then the airglow VER in an orbit plane of Odin was simulated. The results show that the large 106 of VER emerges in the daytime, with a peak near 50-55 km. The VER in the nighttime is nearly zero. The VER peak rises with the increase of solar zenith angle. The comparison between the modeled and retrieved VER from Odin OSIRIS IR Levell data indicates that, there is a good agreement among the scale, photochemical features and decay time at all points along the section. Furthermore, the difference between the modeled and retrieved VER is smaller in high latitudes and the minimum is achieved between 80 and 100 km. It is shown

  8. Equatorial thermospheric measurements of temperatures and winds at Arequipa, Peru

    Science.gov (United States)

    Meriwether, J. W., Jr.; Biondi, M. A.

    1986-01-01

    Enhancement of FPI temperatures above quiet levels was observed a few hours after the start of magnetic activity. Magnitude of this enhancement is about 300 degrees. This is followed by relaxation to prestorm levels. Apparent average offset of RPI temperatures from mass spectrometer incoherent scatter radar by 100 to 200 degrees for relatively quiet times is also observed. There was a definite suggestion of a midnight thermal enhancement for April and August data, with a magnitude of about 100 degrees, seen in both 1983 and 1984 observations. There was a definite enhancement of 6300A surface brightness in the south as compared with other directions, probably connected to the tropical airglow arcs. Meridional winds were small (less than 25 m/s) throughout night. Indication of northward migration of the observed 6300A enhancement in the evening hours as observations approach local winter solstice. This is probably related to the observed poleward (to the south) meridional wind (of magnitude 50 m/s) in this period. Zonal component of winds always eastward, but speed approaches zero sooner near equinox than at summer solstice. Typical magnitude at peak is of order 100 to 150 m/s. Suggestion of zonal wind increase after twilight and recovery of 6300A emission for April data. Origin not clear but may be related to midnight thermal enhancement. Meridional wind virtually zero for equinox in 1983; shows evening flow towards winter hemisphere in early evening for solstice data. Suggestion of post-midnight surge in April 1984 data. No major effects associated with magnetic storm activity, but a suggestion of decrease in zonal component below nominal levels.

  9. First detection of the 63 μm atomic oxygen line in the thermosphere of Mars with GREAT/SOFIA

    Science.gov (United States)

    Rezac, L.; Hartogh, P.; Güsten, R.; Wiesemeyer, H.; Hübers, H.-W.; Jarchow, C.; Richter, H.; Klein, B.; Honingh, N.

    2015-08-01

    Context. The Stratospheric Observatory for Infrared Astronomy (SOFIA) with its 2.5 m telescope provides new science opportunities for spectroscopic observations of planetary atmospheres in the far-infrared wavelength range. Aims: This paper presents first results from the 14 May, 2014 observing campaign of the Martian atmosphere at 4.7 THz using the German REceiver for Astronomy at Terahertz frequencies (GREAT) instrument. Methods: The atomic oxygen 63 μm transition, OI, was detected in absorption against the Mars continuum, with a high signal-to-noise ratio (~35). A beam-averaged atomic oxygen from a global circulation model was used as input to the radiative transfer simulations of the observed line area and to obtain a new estimate on the column density using a grid-search method. Results: Minimizing differences between the calculated and observed line intensities in the least-square sense yields an atomic oxygen column density of (1.1 ± 0.2) × 1017 cm-2. This value is about twice as low as predicted by a modern photochemical model of Mars. The radiative transfer simulations indicate that the line forms in the upper atmospheric region over a rather extended altitude region of 70-120 km. Conclusions: For the first time, a far-infrared transition of the atomic oxygen line was detected in the atmosphere of Mars. The absorption depth provides an estimate on the column density, and this measurement provides additional means to constrain the photochemical models in global circulation models and airglow studies. The lack of other means for monitoring the atomic oxygen in the Martian upper atmosphere makes future observations with the SOFIA observatory highly desirable. Appendix A is available in electronic form at http://www.aanda.org

  10. Data Impact of the DMSP F18 SSULI UV Data on the Operational GAIM Model

    Science.gov (United States)

    Dandenault, P. B.; Metzler, C. A.; Nicholas, A. C.; Coker, C.; Budzien, S. A.; Chua, D. H.; Finne, T. T.; Dymond, K.; Walker, P. W.; Schunk, R. W.; Scherliess, L.; Gardner, L. C.

    2011-12-01

    The Naval Research Laboratory (NRL) has developed five ultraviolet remote sensing instruments for the United States Air Force (USAF) Defense Meteorological Satellite Program (DMSP). The DMSP satellites are launched in a near-polar, sun-synchronous orbit at an altitude of approximately 830 km. Each Special Sensor Ultraviolet Limb Imager (SSULI) instrument measures vertical profiles of the natural airglow radiation from atoms, molecules and ions in the upper atmosphere and ionosphere by viewing the earth's limb within a tangent altitude range of approximately 50 km to 750 km. Limb observations are made from the extreme ultraviolet (EUV) to the far ultraviolet (FUV) over the wavelength range of 80 nm to 170 nm, with 1.8 nm resolution. Data products from SSULI observations include nightglow and dayglow Sensor Data Records (SDRs), as well as Environmental Data Records (EDRs) which contain vertical profiles of electron (Ne) densities, N2, O2, O, O+, and Temperature, hmF2, NmF2 and vertical Total Electron Content (TEC). On October 18, 2009, the third SSULI sensor launched from Vandenberg Air Force Base aboard the DMSP F18 spacecraft. The Calibration and Validation of the F18 instrument has completed and the SSULI program is scheduled to go operational at the Air Force Weather Agency (AFWA) in Fall 2011. The SSULI F18 data are ingested by the Global Assimilation of Ionospheric Measurements (GAIM) space weather model, which was developed by Utah State University and has been used operationally at AFWA since February 2006. A brief overview of the SSULI F18 SDR data assimilation process with GAIM is provided and the impact of the SSULI 1356 Å emission on the GAIM model is examined for spring and summer 2011 nightside data in the low-latitude region.

  11. Quantum yield for O-atom production in the VUV photodissociation of CO2 using the time-sliced velocity-mapped imaging (TS-VMI) method

    Science.gov (United States)

    Jackson, William M.

    2016-10-01

    VUV photodissociation above 10.5 eV is considered the primary region for photochemical destruction of CO2 by solar radiation. There is enough photon energy in this region so that in addition to ground state O(3PJ) and CO(1Σ +) that can be produced during photodissociation excited species such as atomic oxygen O(1D) and O(1S), as well as excited carbon monoxide CO(a3Π, a'3Σ+) also can be formed. Electronic excited oxygen atom and carbon monoxide are the species that are responsible for the airglows in atmospheres of the solar planets and comets. Therefore, detail photodissociation quantum yields for these excited species from CO2 are critical in interpreting the chemistry in these solar system bodies. We have previously shown that the time-sliced velocity-mapped imaging (TS-VMI) technique can provide detailed branching ratio information about photodissociation of diatomic molecules.1, 2 However, to date we have not been able to show how this technique can be use to determine absolute quantum yields for the products produced in the VUV photodissociation of CO2. In this talk we will describe how the known quantum yields for the photodissociation O2 to O(3P2), O(3P1), O(3P0) and O(1D) can be used to determine quantum yields of similar products in the photodissociation of CO2.[1] Yu Song, Hong Gao, Yih Chung Chang, D. Hammouténe, H. Ndome, M. Hochlaf, William M. Jackson, and C. Y. Ng, Ap. J., 819:23 (13pp), 2016; doi:10.3847/0004-637X/819/1/23.[2] Hong Gao, Yu Song, William M. Jackson and C. Y. Ng, J. Chem. Phys, 138, 191102, 2013.

  12. The prediction of the optical contrast of air-borne targets against the night-sky background for Photopic and NVG sensors

    Science.gov (United States)

    Havemann, Stephan; Wong, Gerald

    2016-10-01

    The Havemann-Taylor Fast Radiative Transfer Code (HT-FRTC) represents transmittances, radiances and fluxes by principal components that cover the spectra at very high resolution, allowing fast highly-resolved pseudo line-by-line, hyperspectral and broadband simulations across the electromagnetic spectrum form the microwave to the ultraviolet for satellite-based, airborne and ground-based sensors. HT-FRTC models clear atmospheres and those containing clouds and aerosols, as well as any surface (land/sea/man-made). The HT-FRTC has been used operationally in the NEON Tactical Decision Aid (TDA) since 2008. The TDA combines the HT-FRTC with a thermal contrast model and an NWP model forecast data feed to predict the apparent thermal contrast between different surfaces and ground-based targets in the thermal and short-wave IR. The new objective here is to predict the optical contrast of air-borne targets under realistic night-time scenarios in the Photopic and NVG parts of the spectrum. This requires the inclusion of all the relevant radiation sources, which include twilight, moonlight, starlight, airglow and cultural light. A completely new exact scattering code has been developed which allows the straight-forward addition of any number of direct and diffuse sources anywhere in the atmosphere. The new code solves the radiative transfer equation iteratively and is faster than the previous solution. Simulations of scenarios with different light levels, from situations during a full moon to a moonless night with very low light levels and a situation with cultural light from a town are presented. The impact of surface reflectance and target reflectance is investigated.

  13. The fast development of solar terrestrial sciences in Taiwan

    Science.gov (United States)

    Liu, Jann-Yenq; Chang, Loren Chee-Wei; Chao, Chi-Kuang; Chen, Ming-Quey; Chu, Yen-Hsyang; Hau, Lin-Ni; Huang, Chien-Ming; Kuo, Cheng-Ling; Lee, Lou-Chuang; Lyu, Ling-Hsiao; Lin, Chia-Hsien; Pan, Chen-Jeih; Shue, Jih-Hong; Su, Ching-Lun; Tsai, Lung-Chih; Yang, Ya-Hui; Lin, Chien-Hung; Hsu, Rue-Ron; Su, Han-Tzong

    2016-12-01

    In Taiwan, research and education of solar terrestrial sciences began with a ground-based ionosonde operated by Ministry of Communications in 1952 and courses of ionospheric physics and space physics offered by National Central University (NCU) in 1959, respectively. Since 1990, to enhance both research and education, the Institute of Space Science at NCU has been setting up and operating ground-based observations of micropulsations, very high-frequency radar, low-latitude ionospheric tomography network, high-frequency Doppler sounder, digital ionosondes, and total electron content (TEC) derived from ground-based GPS receivers to study the morphology of the ionosphere for diurnal, seasonal, geophysical, and solar activity variations, as well as the ionosphere response to solar flares, solar wind, solar eclipses, magnetic storms, earthquakes, tsunami, and so on. Meanwhile, to have better understanding on physics and mechanisms, model simulations for the heliosphere, solar wind, magnetosphere, and ionosphere are also introduced and developed. After the 21 September 1999 Mw7.6 Chi-Chi earthquake, seismo-ionospheric precursors and seismo-traveling ionospheric disturbances induced by earthquakes become the most interesting and challenging research topics of the world. The development of solar terrestrial sciences grows even much faster after National Space Origination has been launching a series of FORMOSAT satellites since 1999. ROCSAT-1 (now renamed FORMOSAT-1) measures the ion composition, density, temperature, and drift velocity at the 600-km altitude in the low-latitude ionosphere; FORMOSAT-2 is to investigate lightning-induced transient luminous events, polar aurora, and upper atmospheric airglow, and FORMOSAT-3 probes ionospheric electron density profiles of the globe. In the near future, FORMOSAT-5 and FORMOSAT-7/COSMIC-2 will be employed for studying solar terrestrial sciences. These satellite missions play an important role on the recent development of solar

  14. Ionospheric response to geomagnetic disturbances in the north-eastern region of Asia during the minimum of 23rd cycle of solar activity

    Science.gov (United States)

    Kurkin, V. I.; Pirog, O. M.; Polekh, N. M.; Mikhalev, A. V.; Poddelsky, I. N.; Stepanov, A. E.

    2008-12-01

    We present the results of studies of the subauroral and mid-latitude ionosphere variations in the north-eastern region of Asia. We used the data from network of vertical and oblique-incidence sounding ionosondes and optical measurements. Long-term experiments on the radio paths Magadan-Irkutsk and Norilsk-Irkutsk were carried out within the period 2005-2007. Vertical sounding stations operated in standard regime. Observation of airglow near Irkutsk was provided by the zenith photometer that measured intensities of 557.7 and 630.0 nm atomic oxygen emissions. The results may be summarized as follows. (1) Large daytime negative disturbances are observed during the main and recovery phases mainly at high latitudes, whereas the positive disturbances observed during the main phase at mid latitudes. The disturbances changed their sign between Yakutsk and Irkutsk. (2) During the main and recovery storm phases the fall of foF2 associated with the equatorward wall of the main ionospheric trough is observed in the afternoon and evening. (3) Fluctuations of the electron density more intensive at mid latitudes during the storm main phase are observed during all considered periods. They are classed as traveling ionospheric disturbances (TID). Such sharp gradients of electron density are responsible for the strong changes in the characteristics of the radio wave propagation, particularity MOF. (4) A large-scale ionospheric disturbance is noted at the meridional chain of ionosonds in December 2006 as the sharp increase of foF2. It appears in the evening in the minimum of Dst at high latitude and propagate to equator. (5) A maximum of 630 nm emission above Irkutsk corresponds to the foF2 increase. (6) The obtained experimental data on the net of vertical and oblique-incidence sounding with high time resolution show that such net is the effective facility to study the conditions of the radio wave propagation and can be used for the diagnostic of the ionosphere.

  15. Effects of solar zenith angles on CO Cameron bands emission intensities in the dayside atmosphere of Mars: MEX/SPICAM observations

    Science.gov (United States)

    Pothuraju, Thirupathaiah; Haider, Syed A.

    2016-07-01

    We have developed a model to calculate the photoelectron energy fluxes and emission intensities of the CO Cameron bands in the upper atmosphere of Mars between solar zenith angles 0° to 90°. The production and loss mechanisms of CO (a ^{3}Π) are incorporated in the model. The atmospheric neutral parameters are adopted from the Mars Climate Database (v5.2). The required solar EUV fluxes are taken from the Solar2000 model (v2.37) and scaled to Mars. The photoelectron fluxes are calculated at different solar zenith angles using an analytical yield spectrum approach based on the Monte Carlo method. In this model we have assumed that crustal magnetic fields are horizontal in direction. Thus, photoelectrons are losing their energy at the same height where they are produced. This assumption is valid at mid and high latitudes where magnetic fields are mostly horizontal. We have also developed a coupled chemistry model to calculate the ion and electron density at different solar zenith angles, which are used in the airglow model. The model results are compared with the observations provided by the SPICAM onboard MEX. Our model reproduces the observed intensity profiles quite well. The CO (a ^{3}Π) is produced due to photoelectron excitation/dissociation, photodissociation, and dissociative recombination processes. It is destroyed by CO _{2}, CO and radiative decay. It is found that photon and photoelectron dissociation are dominant production processes of CO (a ^{3}Π), while radiative decay is a major loss mechanism of this state. The estimated photoelectron fluxes, production rates and intensities are decreasing with increasing solar zenith angles.

  16. Electron loss rates from the outer radiation belt caused by the filling of the outer plasmasphere: the calm before the storm

    Energy Technology Data Exchange (ETDEWEB)

    Borovsky, Joseph E [Los Alamos National Laboratory; Denton, Michael H [LANCASTER UNIV

    2009-01-01

    Measurements from 7 spacecraft in geosynchronous orbit are analyzed to determine the decay rate of the number density of the outer electron radiation belt prior to the onset of high-speed-stream-driven geomagnetic storms. Superposed-data analysis is used wan(?) a collection of 124 storms. When there is a calm before the storm, the electron number density decays exponentially before the storm with a 3.4-day e-folding time: beginning about 4 days before storm onset, the density decreases from {approx}4x10{sup -4} cm{sup -3} to {approx}1X 10{sup -4} cm{sup -3}. When there is not a calm before the storm, the number-density decay is very smalL The decay in the number density of radiation-belt electrons is believed to be caused by pitch-angle scattering of electrons into the atmospheric loss cone as the outer plasmasphere fills during the calms. While the radiation-belt electron density decreases, the temperature of the electron radiation belt holds approximately constant, indicating that the electron precipitation occurs equally at all energies. Along with the number density decay, the pressure of the outer electron radiation belt decays and the specific entropy increases. From the measured decay rates, the electron flux to the atmosphere is calculated and that flux is 3 orders of magnitude less than thermal fluxes in the magnetosphere, indicating that the radiation-belt pitch-angle scattering is 3 orders weaker than strong diffusion. Energy fluxes into the atmosphere are calculated and found to be insufficient to produce visible airglow.

  17. MAVEN's Imaging UV Spectrograph: Studying Atmospheric Structure and Escape at Mars

    Science.gov (United States)

    Schneider, Nicholas M.; McClintock, W. E.; IUVS Science Team

    2012-10-01

    MAVEN (Mars Volatile and Atmosphere EvolutioN) is a Mars Scout mission slated for launch in November 2013. The key hardware and management partners are University of Colorado, Goddard Space Flight Center, University of California at Berkeley, Lockheed Martin, and the Jet Propulsion Laboratory. MAVEN carries a powerful suite of fields and particles instruments and a sophisticated Imaging UltraViolet Spectrograph (IUVS). In this presentation we will describe IUVS' science goals, instrument design, operational approach and data analysis strategy. IUVS supports the top-level MAVEN science goals: measure the present state of the atmosphere, observe its response to varying solar stimuli, and use the information to estimate loss from Mars' atmosphere over time. The instrument operates at low spectral resolution spanning the FUV and MUV ranges in separate channels, and at high resolution around the hydrogen Lyman alpha line to measure the D/H ratio in the upper atmosphere. MAVEN carries the instrument on an Articulated Payload Platform which orients the instrument for optimal observations during four segments of its 4.5 hr elliptical orbit. During periapse passage, IUVS uses a scan mirror to obtain vertical profiles of emissions from the atmosphere and ionosphere. Around apoapse, the instrument builds up low-resolution images of the atmosphere at multiple wavelengths. In between, the instrument measures emissions from oxygen, hydrogen and deuterium in the corona. IUVS also undertakes day-long stellar occultation campaigns at 2 month intervals, to measure the state of the atmosphere at altitudes below the airglow layer and in situ sampling. All data will be pipeline-processed from line brightnesses to column abundances, local densities and global 3-D maps and provided to the PDS Atmospheres Node. The combined results from all instruments on ion and neutral escape will bear on the central question of the history of Mars' atmosphere and climate change.

  18. Polarizing Michelson interferometer for measuring thermospheric winds

    Energy Technology Data Exchange (ETDEWEB)

    Bird, J.C.

    1991-01-01

    The Polarizing Atmospheric Michelson Interferometer, PAMI, a new version of the Wide Angle Michelson Interferometer, is used to measure winds in the termosphere. In the polarizing instrument, the optical path difference is changed simply by rotating a polarizing filter external to the interferometer. This allows a very simple scanning mechanism. PAMI is similar to other instruments such as WAMDII that measure thermospheric winds and temperatures, retaining the benefits of high light throughput, while offering advantages including lower cost, simplicity, and portability. The instrument is highly sensitive and thus is designed to be used for field measurements at locations far from city lights. Results are shown from the AIDA observation campaign in Puerto Rico where coordinated observations were made by PAMI along with other optical and radio measurements during April and May 1989. Intensities of the green line layer at 95 km were compared to those observed by several other instruments. For example, MORTI (Mesopause Oxygen Rotational Temperature Imager), a colocated instrument which was looking at the 94 km 867.6 nm molecular oxygen emission. MORTI and PAMI emission rates were found to show the same trends. On the brightest night recorded during April, the zenith emission rate reached over 400 Rayleighs; emission enhancements were sometimes related to auroral events. During the observing period of April 4 to April 11, 1989, most of the observations of the 94 km airglow were after midnight where the winds were found to be generally towards the north east at about 50 to 100 m/s. During auroral activity this wind vector always turned counterclockwise, towards the west. During the nights of May 2 and May 6 these wind vectors follow a wave-like variation in magnitude and direction. It is concluded that auroral activity changes the global circulation in a way that sometimes transports increased amounts of oxygen atoms over Arecibo.

  19. Galileo Ultraviolet Spectrometer experiment

    Science.gov (United States)

    Hord, C. W.; Mcclintock, W. E.; Stewart, A. I. F.; Barth, C. A.; Esposito, L. W.; Thomas, G. E.; Sandel, B. R.; Hunten, D. M.; Broadfoot, A. L.; Shemansky, D. E.

    1992-01-01

    The Galileo ultraviolet spectrometer experiment uses data obtained by the Ultraviolet Spectrometer (UVS) mounted on the pointed orbiter scan platform and from the Extreme Ultraviolet Spectrometer (EUVS) mounted on the spinning part of the orbiter with the field of view perpendicular to the spin axis. The UVS is a Ebert-Fastie design that covers the range 113-432 nm with a wavelength resolution of 0.7 nm below 190 and 1.3 nm at longer wavelengths. The UVS spatial resolution is 0.4 deg x 0.1 deg for illuminated disk observations and 1 deg x 0.1 deg for limb geometries. The EUVS is a Voyager design objective grating spectrometer, modified to cover the wavelength range from 54 to 128 nm with wavelength resolution 3.5 nm for extended sources and 1.5 nm for point sources and spatial resolution of 0.87 deg x 0.17 deg. The EUVS instrument will follow up on the many Voyager UVS discoveries, particularly the sulfur and oxygen ion emissions in the Io torus and molecular and atomic hydrogen auroral and airglow emissions from Jupiter. The UVS will obtain spectra of emission, absorption, and scattering features in the unexplored, by spacecraft, 170-432 nm wavelength region. The UVS and EUVS instruments will provide a powerful instrument complement to investigate volatile escape and surface composition of the Galilean satellites, the Io plasma torus, micro- and macro-properties of the Jupiter clouds, and the composition structure and evolution of the Jupiter upper atmosphere.

  20. Thermospheric zonal temperature gradients observed at low latitudes

    Directory of Open Access Journals (Sweden)

    P. R. Fagundes

    Full Text Available Fabry-Perot interferometer (FPI measurements of thermospheric temperatures from the Doppler widths of the OI 630 nm nightglow emission line have been carried out at Cachoeira Paulista (23° S, 45° W, 16° S dip latitude, Brazil. The east-west components of the thermospheric temperatures obtained on 73 nights during the period from 1988 to 1992, primarily under quiet geomagnetic conditions, were analyzed and are presented in this paper. It was observed that on 67% of these nights, the temperatures in both the east and west sectors presented similar values and nocturnal variations. However, during 33% of the nights, the observed temperatures in the west sector were usually higher than those observed in the east sector, with zonal temperature gradients in the range of 100 K to 600 K, over about an 800 km horizontal distance. Also, in some cases, the observed temperatures in the east and west sectors show different nocturnal variations. One of the possible sources considered for the observed zonal temperature gradients is the influence of gravity wave dissipation effects due to waves that propagate from lower altitudes to thermospheric heights. The observed zonal temperature gradients could also be produced by orographic gravity waves originated away, over the Andes Cordillera in the Pacific Sector, or by dissipation of orographic gravity waves generated over the Mantiqueira Mountains in the Atlantic sector by tropospheric disturbances (fronts and/or subtropical jet streams.

    Key words. Atmospheric composition and structure (air-glow and aurora; thermosphere - composition and chemistry Ionosphere (equatorial ionosphere

  1. Extension of the AURIC Radiative Transfer Model for Mars Atmospheric Research

    Science.gov (United States)

    Evans, J. S.; Lumpe, J. D.; Correira, J.; Stewart, A. I.; Schneider, N. M.; Deighan, J.

    2013-12-01

    We present recent updates to the Atmospheric Ultraviolet Radiance Integrated Code (AURIC) model that allow it to be used as a forward model for Mars atmospheric research. AURIC is a state of the art far ultraviolet (FUV) to near-infrared (NIR) atmospheric radiance model that has been used extensively for analysis and modeling of terrestrial upper atmospheric remote sensing data. We present recent updates to the Atmospheric Ultraviolet Radiance Integrated Code (AURIC) model that allow it to be used as a forward model for Mars atmospheric research. AURIC is a state of the art far ultraviolet (FUV) to near-infrared (NIR) atmospheric radiance model that has been used extensively for analysis and modeling of terrestrial upper atmospheric remote sensing data. The airglow modeling capabilities of AURIC make it a powerful tool that can be used to characterize optical backgrounds, simulate data from both rocket and satellite-borne optical instrumentation, and serve as a forward model driver for geophysical retrieval algorithms. Upgrades made to allow modeling of the Martian atmosphere include 1-D Mars photochemistry and molecular transport and the addition of the following molecular band systems: CO Cameron; CO Fourth Positive Group; CO2+ Fox-Duffendack-Barker; CO2+ UV Doublet; CO Hopfield-Birge (B-X); and CO+ First Negative Group. Furthermore, a prototype AURIC-Titan model has also been developed, allowing comparison of AURIC spectral radiances with Cassini-Huygens/UVIS data [Stevens et al., 2011; Stevens et al., in preparation]. Extension of AURIC to the atmospheres of Pluto and it's largest moon, Charon, is also ongoing in support of NASA's New Horizons mission [Stevens, Evans, and Gladstone, 2012; 2013].

  2. Observation of a mesospheric front in a thermal-doppler duct over King George Island, Antarctica

    Directory of Open Access Journals (Sweden)

    J. V. Bageston

    2011-12-01

    Full Text Available A mesospheric front was observed with an all-sky airglow imager on the night of 9–10 July 2007 at Ferraz Station (62° S, 58° W, located on King George island on the Antarctic Peninsula. The observed wave propagated from southwest to northeast with a well defined wave front and a series of crests behind the main front. The wave parameters were obtained via a 2-D Fourier transform of the imager data providing a horizontal wavelength of 33 km, an observed period of 6 min, and a horizontal phase speed of 92 m s−1. Simultaneous mesospheric winds were measured with a medium frequency (MF radar at Rothera Station (68° S, 68° W and temperature profiles were obtained from the SABER instrument on the TIMED satellite. These wind and temperature profiles were used to estimate the propagation environment of the wave event. A wavelet technique was applied to the wind in the plane of wave propagation at the OH emission height spanning three days centered on the front event to define the dominant periodicities. Results revealed a dominance of near-inertial periods, and semi-diurnal and terdiurnal tides suggesting that the ducting structure enabling mesospheric front propagation occurred on large spatial scales. The observed tidal motions were used to reconstruct the winds employing a least-squares method, which were then compared to the observed ducting environment. Results suggest an important contribution of large-scale winds to the ducting structure, but with buoyancy frequency variations in the vertical also expected to be important. These results allow us to conclude that the wave front event was supported by a duct including contributions from both winds and temperature.

  3. Probing Reionization through Near-Infrared Background Fluctuations with CIBER

    Science.gov (United States)

    Sullivan, Ian S.

    2010-01-01

    The Cosmic Infrared Background Experiment (CIBER) is a NASA sounding rocket payload that was first launched in February 2009. CIBER consists of four co-aligned instruments designed with foreground subtraction and control of systematics in mind. In addition, the platform of a sounding rocket enables observations of the NIRB outside of narrow atmospheric windows that are uncontaminated by airglow. We will present preliminary results from the first flight. CIBER seeks to measure the absolute brightness spectrum of the extragalactic NIRB, and has two spectrometers dedicated to that purpose. One, a high-resolution Fabry-Perot spectometer, is tuned to the 8545 nm Ca II line of the solar spectrum, and is designed to measure the absolute brightness of the Zodiacal Light directly, which is the source of greatest uncertainty in the NIRB spectrum. The second spectrometer measures the NIRB spectrum from 700nm to 1800nm, which spans the wavelength range where a Lyman cutoff feature from Reionization could appear. CIBER also houses two Infrared imaging telescopes, which have identical optics that give 2º x 2º field of views with 7 arcsec pixels, but have different band defining filters. The first imager has a wide band centered at 1600nm, and images the background at the expected peak of the spectrum. The imagers’ wide field of view allows them to measure the distinctive power spectrum peaking at 10 arcminutes. The second imager has a wide band centered at 1000nm that is intended to image at wavelengths shorter than the Lyman cutoff, and provides a powerful systematic test for any detection made at 1600 nm. First-light fluctuations should have a distinctive spatial power spectrum with very red 1600nm / 1000nm color, distinctly redder than the approximately solar color of any residual fluctuations arising from Zodiacal light, Galactic starlight, or low-redshift galaxies.

  4. A coordinated study of 1 h mesoscale gravity waves propagating from Logan to Boulder with CRRL Na Doppler lidars and temperature mapper

    Science.gov (United States)

    Lu, Xian; Chen, Cao; Huang, Wentao; Smith, John A.; Chu, Xinzhao; Yuan, Tao; Pautet, Pierre-Dominique; Taylor, Mike J.; Gong, Jie; Cullens, Chihoko Y.

    2015-10-01

    We present the first coordinated study using two lidars at two separate locations to characterize a 1 h mesoscale gravity wave event in the mesopause region. The simultaneous observations were made with the Student Training and Atmospheric Research (STAR) Na Doppler lidar at Boulder, CO, and the Utah State University Na Doppler lidar and temperature mapper at Logan, UT, on 27 November 2013. The high precision possessed by the STAR lidar enabled these waves to be detected in vertical wind. The mean wave amplitudes are ~0.44 m/s in vertical wind and ~1% in relative temperature at altitudes of 82-107 km. Those in the zonal and meridional winds are 6.1 and 5.2 m/s averaged from 84 to 99 km. The horizontal and vertical wavelengths inferred from the mapper and lidars are ~219 ± 4 and 16.0 ± 0.3 km, respectively. The intrinsic period is ~1.3 h for the airglow layer, Doppler shifted by a mean wind of ~17 m/s. The wave packet propagates from Logan to Boulder with an azimuth angle of ~135° clockwise from north and an elevation angle of ~ 3° from the horizon. The observed phase difference between the two locations can be explained by the traveling time of the 1 h wave from Logan to Boulder, which is about ~2.4 h. The wave polarization relations are examined through the simultaneous quantifications of the three wind components and temperature. This study has developed a systematic methodology for fully characterizing mesoscale gravity waves, inspecting their intrinsic properties and validating the derivation of horizontal wave structures by applying multiple instruments from coordinated stations.

  5. Challenge of lightning detection with LAC on board Akatsuki spacecraft

    Science.gov (United States)

    Takahashi, Yukihiro; Sato, Mitsutero; Imai, Masataka; Yair, Yoav; Fischer, Georg; Aplin, Karen

    2016-04-01

    Even after extensive investigations with spacecraft and ground-based observations, there is still no consensus on the existence of lightning in Venus. It has been reported that the magnetometer on board Venus Express detected whistler mode waves whose source could be lightning discharge occurring well below the spacecraft. On the other hand, with an infrared sensor, VIRTIS of Venus Express, does not show the positive indication of lightning flashes. In order to identify the optical flashes caused by electrical discharge in the atmosphere of Venus, at least, with an optical intensity of 1/10 of the average lightning in the Earth, we built a high-speed optical detector, LAC (Lightning and Airglow Camera), on board Akatsuki spacecraft. The unique performance of the LAC compared to other instruments is the high-speed sampling rate at 32 us interval for all 32 pixels, enabling us to distinguish the optical lightning flash from other pulsing noises. Though, unfortunately, the first attempt of the insertion of Akatsuki into the orbit around Venus failed in December 2010, the second one carried out in December 7 in 2015 was quite successful. We checked out the condition of the LAC on January 5, 2016, and it is healthy as in 2010. Due to some elongated orbit than that planned originally, we have umbra for ~30 min to observe the lightning flash in the night side of Venus every ~10 days, starting on April 2016. Here we would report the instrumental status of LAC and the preliminary results of the first attempt to observe optical lightning emissions.

  6. Analysis of traveling ionospheric disturbances (TIDs) in GPS TEC launched by the 2011 Tohoku earthquake

    Science.gov (United States)

    Crowley, Geoff; Azeem, Irfan; Reynolds, Adam; Duly, Timothy M.; McBride, Patrick; Winkler, Clive; Hunton, Don

    2016-05-01

    Traveling ionospheric disturbances (TIDs) have been detected using various measurement techniques, including HF sounders, incoherent scatter radars, in situ measurements, and optical techniques. However, observations of TIDs have tended to be sparse and there is a need for additional observations to provide new scientific insight into the geophysical source phenomenology and wave propagation physics. The dense network of GPS receivers around the globe offers a relatively new data source to observe and monitor TIDs. In this paper, we use total electron content (TEC) measurements from ~4000 GPS receivers throughout the continental United States to observe TIDs associated with the 11 March 2011 Tohoku tsunami. The tsunami propagated across the Pacific to the U.S. west coast over several hours, and we show that corresponding TIDs were observed in the US. Using this network of GPS receivers we present a 2D imaging of TEC perturbations and calculate various TID parameters, including horizontal wavelength, speed, and period. Well-formed, planar TIDs were detected over the west coast of the U.S. ~10 h after the earthquake. Fast Fourier transform analysis of the observed waveforms revealed that the period of the wave was 15.1 min with a horizontal wavelength of 194.8 km, phase velocity of 233.0 m/s, and an azimuth of 105.2° (propagating nearly due east in the direction of the tsunami wave). These results are consistent with the TID observations in airglow measurements from Hawaii earlier in the day and with other GPS TEC observations.

  7. Observations of Traveling Ionospheric Disturbances (TIDs) Over the United States Associated With the Tsunami Generated by the 2011 Tohoku Earthquake

    Science.gov (United States)

    Duly, T. M.; Azeem, I.; Crowley, G.; Vadas, S.; Makela, J. J.; Reynolds, A.

    2015-12-01

    The March 11, 2011 Tohoku earthquake generated a massive tsunami off the Pacific coast of Japan which in turn forced intense atmospheric gravity waves (AGW) that were seen in GPS Total Electron Content (TEC) data and airglow measurements as traveling ionospheric disturbance (TID) signatures as far away as Hawaii. What is unknown is how far these TIDs traveled after being launched by the tsunami and the role of the underlying neutral atmosphere on their propagation characteristics. For the first time, we show that TIDs associated with the Tohoku tsunami were observed in GPS TEC data for several hours over the west coast of the US and as far inland as Colorado. The results presented here show a range of TIDs generated by gravity wave packets propagating into the ionosphere from below. We present results indicating the presence of TIDs with periods ranging from 15 to 30 minutes, and horizontal wavelengths from 150 km to 400 km. The azimuth of the observed TID wave train was 121.8 ± 1.8° (angle measured in degrees east of north), which matches the azimuth of the tsunami near the Pacific coast of the US. The observed period of the TIDs was one of the spectral components of the tsunami wave packet as it approached the Pacific coast of the US. These results suggest that the tsunami was the source of the TIDs over the US. Additionally, the TID periods and horizontal wavelengths clearly vary in longitude. These variations agree with theoretical gravity wave results concerning propagation and dissipation in the thermosphere.

  8. TIMED Doppler Interferometer: Overview and recent results

    Science.gov (United States)

    Killeen, T. L.; Wu, Q.; Solomon, S. C.; Ortland, D. A.; Skinner, W. R.; Niciejewski, R. J.; Gell, D. A.

    2006-10-01

    The Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED) satellite carries a limb-scanning Fabry-Perot interferometer designed to perform remote-sensing measurements of upper atmosphere winds and temperatures globally. This instrument is called the TIMED Doppler Interferometer, or TIDI. This paper provides an overview of the TIDI instrument design, on-orbit performance, operational modes, data processing and inversion procedures, and a summary of wind results to date. Daytime and nighttime neutral winds in the mesosphere and lower thermosphere/ionosphere (MLTI) are measured on TIDI using four individual scanning telescopes that collect light from various upper atmosphere airglow layers on both the cold and warm sides of the high-inclination TIMED spacecraft. The light is spectrally analyzed using an ultrastable plane etalon Fabry-Perot system with sufficient spectral resolution to determine the Doppler line characteristics of atomic and molecular emissions emanating from the MLTI. The light from all four telescopes and from an internal calibration field passes through the etalon and is combined on a single image plane detector using a Circle-to-Line Interferometer Optic (CLIO). The four geophysical fields provide orthogonal line-of-sight measurements to either side of the satellite's path and these are analyzed to produce altitude profiles of vector winds in the MLTI. The TIDI wind measurements presented here are from the molecular oxygen (0-0) band, covering the altitude region 85-105 km. The unique TIDI design allows for more extended local time coverage of wind structures than previous wind-measuring instruments from high-inclination satellites. The TIDI operational performance has been nominal except for two anomalies: (1) higher than expected background white light caused by a low-level light leak and (2) ice deposition on cold optical surfaces. Both anomalies are well understood and the instrumental modes and data analysis techniques have been

  9. On the temporal variability of the OH* emission layer at the mesopause: a study based on SD-WACCM4 and SABER

    Directory of Open Access Journals (Sweden)

    S. Kowalewski

    2014-01-01

    Full Text Available Airglow observations are a fundamental tool to study the mesospheric part of the atmosphere. In particular the OH* emission layer is subject of many theoretical and observational studies. The choice of different transition bands of the OH* emission can introduce systematic differences between these studies, hence a profound knowledge of these differences is required for comparison. One systematic difference is given by the vertical displacements between OH* profiles due to different transition bands. A previous study has shown that the vertical displacement is highly sensitive to quenching with atomic oxygen. In this work we follow up this idea by investigating the diurnal as well as the seasonal response of OH* to changes in concentrations of atomic and molecular oxygen, the two most effective quenching species of OH*. For this task we employ a quenching model to calculate vertical OH* concentration profiles from simulations made with the SD-WACCM4 chemistry transport model. From this approach we find that despite the strong impact of O and O2 quenching on the vertical OH* structure, a considerable variability between the vertical displacements of different OH* transition bands is also induced by the natural variability of the O3 and H profiles, which primarily participate in the formation of the mesospheric OH* layer. This in particular applies for the diurnal evolution of the vertical displacements, which cannot be explained by changes in abundances of OH* quenching species only. On the other hand, vertical displacements between OH* transition bands and the amount of effective O and O2 quenching show a coherent semi-annual oscillation at lower latitudes that is in phase with the seasonal variability of the diurnal migrating tide. In particular the role of O2 quenching shows a new aspect of the semi-annual oscillation that, to our knowledge, has not been discussed before. By comparison with limb radiance observations from the SABER

  10. Present status of the Japanese Venus climate orbiter

    Science.gov (United States)

    Nakamura, M.; Imamura, T.; Abe, T.; Ishii, N.

    The code name of 24th science spacecraft of ISAS/JAXA is Planet-C. It is the first Venus Climate Orbiter (VCO) of Japan. The ministry of finance of Japan finally agreed to start phase B study of VCO from this April, 2004. We plan 1-2 years phase B study followed by 2 years of flight model integration. The spacecraft will be launched between 2009 and 2010. After arriving Venus, 2 years of operation is expected. VCO will complemet the ESA's Venus Express mission which have several spectrometers and will reveal the composition of the Venusian atmosphere. On the other hand, VCO is designed to reveal the details of the atmospheric motion on Venus and approach the dynamics of the Venusian climate. Cooperation between Japanese VCO and ESA's Venus Express, in the colaboration framework of U.S., Europian, and Japanese scienctist is very important. To elucidate the driving mechanism of the 4-days super-rotation is one of our main targets. We have 4 cameras to take snap shots of the planets in different wave lengths. They are the IR1 camera (1 micron-meter), the IR2 camera (2.4 micron-meter), the LIR camera (10-12 micron-meter), and the UVI camera (340nm). They are attached to the side panel of the 3-axis stabilized spacecraft, and are directed to Venus with the spacecraft's attitude control. Snap shots are expected to be taken every 2 hours. The spacecraft has an orbit of 300km x 13Rv (Venusian radii) with 172 degrees inclination. Orbital period is 30 hours. The angular position of the spacecraft on this orbit is synchronized for 20 hours at its apoapsis with the global atmospheric circulation at the altitude of 50km, thus the snap shots of every 2 hours will be the images of the same side of the atmosphere. In addition to these 4 cameras, we have a Lightning and Airglow camera (LAC) in visible range. This will be operated when the orbiter is close to the planet.

  11. Mid-latitude ionospheric perturbation associated with the Spacelab-2 plasma depletion experiment at Millstone Hill

    Directory of Open Access Journals (Sweden)

    J. C. Foster

    Full Text Available Elevation scans across geomagnetic mid latitudes by the incoherent scatter radar at Millstone Hill captured the ionospheric response to the firing of the Space Shuttle Challenger OMS thrusters near the peak of the F layer on July 30, 1985. Details of the excitation of airglow and the formation of an ionospheric hole during this event have been reported in an earlier paper by Mendillo et al.. The depletion (factor ~2 near the 320 km Shuttle orbital altitude persisted for ~35 min and then recovered to near normal levels, while at 265 km the density was reduced by a factor of ~6; this significant reduction in the bottomside F-region density persisted for more than 3 hours. Total electron content in the vicinity of the hole was reduced by more than a factor of 2, and an oscillation of the F-region densities with 40-min period ensued and persisted for several hours. Plasma vertical Doppler velocity varied quasi-periodically with a ~80-min period, while magnetic field variations observed on the field line through the Shuttle-burn position exhibited a similar ~80-min periodicity. An interval of magnetic field variations at hydromagnetic frequencies (~95 s period accompanied the ionospheric perturbations on this field line. Radar observations revealed a downward phase progression of the 40-min period density enhancements of -1.12° km-1, corresponding to a 320-km vertical wavelength. An auroral-latitude geomagnetic disturbance began near the time of the Spacelab-2 experiment and was associated with the imposition of a strong southward IMF Bz across the magnetosphere. This created an additional complication in the interpretation of the active ionospheric experiment. It cannot be determined uniquely whether the ionospheric oscillations, which followed the Spacelab-2 experiment, were related to the active experiment or were the result of a propagating ionospheric disturbance (TID launched by the enhanced auroral

  12. Electron ionization of metastable nitrogen and oxygen atoms in relation to the auroral emissions

    Science.gov (United States)

    Pandya, Siddharth; Joshipura, K. N.

    Atomic and molecular excited metastable states (EMS) are exotic systems due to their special properties like long radiative life-time, large size (average radius) and large polarizability along with relatively smaller first ionization energy compared to their respective ground states (GS). The present work includes our theoretical calculations on electron impact ionization of metastable atomic states N( (2) P), N( (2) D) of nitrogen and O( (1) S), O( (1) D) of oxygen. The targets of our present interest, are found to be present in our Earth's ionosphere and they play an important role in auroral emissions observed in Earth’s auroral regions [1] as also in the emissions observed from cometary coma [2, 3] and airglow emissions. In particular, atomic oxygen in EMS can radiate, the visible O( (1) D -> (3) P) doublet 6300 - 6364 Å red doublet, the O( (1) S -> (1) D) 5577 Å green line, and the ultraviolet O( (1) S -> (3) P) 2972 Å line. For metastable atomic nitrogen one observes the similar emissions, in different wavelengths, from (2) D and (2) P states. At the Earth's auroral altitudes, from where these emissions take place in the ionosphere, energetic electrons are also present. In particular, if the metastable N as well as O atoms are ionized by the impact of electrons then these species are no longer available for emissions. This is a possible loss mechanism, and hence it is necessary to analyze the importance of electron ionization of the EMS of atomic O and N, by calculating the relevant cross sections. In the present paper we investigate electron ionization of the said metastable species by calculating relevant total cross sections. Our quantum mechanical calculations are based on projected approximate ionization contribution in the total inelastic cross sections [4]. Detailed results and discussion along with the significance of these calculations will be presented during the COSPAR-2014. References [1] A.Bhardwaj, and G. R. Gladstone, Rev. Geophys., 38

  13. Tle Triangulation Campaign by Japanese High School Students as a Space Educational Project of the Ssh Consortium Kochi

    Science.gov (United States)

    Yamamoto, Masa-Yuki; Okamoto, Sumito; Miyoshi, Terunori; Takamura, Yuzaburo; Aoshima, Akira; Hinokuchi, Jin

    and sprite halos with stripes like wave structures on airglow were successfully imaged in January 2010. In this talk, four years activities of the SSH consortium Kochi will be presented by participating high-school students and teachers with their own impressions.

  14. First measurement of helium on Mars: Implications for the problem of radiogenic gases on the terrestrial planets

    Science.gov (United States)

    Krasnopolsky, V. A.; Bowyer, S.; Chakrabarti, S.; Gladstone, G. R.; Mcdonald, J. S.

    1994-01-01

    108 +/- 11 photons of the martian He 584-A airglow detected by the Extreme Ultraviolet Explorer (EUVE) satellite during a 2-day exposure (January 22-23, 1993) correspond to the effective disk average intensity of 43 +/- 10 Rayleigh (Ra). Radiative transfer calculations, using a model atmosphere appropriate to the conditions of the observation and having an exospheric temperature of 210 +/- 20 K, result in a He mixing ratio of 1.1 +/- 0.4 ppm in the lower atmosphere. Nonthermal escape of helium is due to electron impact ionization and pickup of He(+) by the solar wind, to collisions with hot oxygen atoms, and to charge exchange with molecular species with corresponding column loss rates of 1.4 x 10(exp 5), 3 x 10(exp 4), and 7 x 10(exp 3)/sq cm/s, respectively. The lifetime of helium on Mars is 5 x 10(exp 4) years. the He outgassing rate, coupled with the Ar-40 atmospheric abundance and with the K:U:Th ratio measured in the surface rocks, is used as input to a single two-reservoir degassing model which is applied to Mars and then to Venus. A similar model with known abundances if K, U, and Th is applied to Earth. The models for Earth and Mars presume loss of all argon accumulated in the atmospheres during the first billion years by large-scale meteorite and planetesimal impacts. The models show that the degassing coefficients for all three planets may be approximated by function delta = delta(sub 0) x (t(sub 0)/t)(exp 1/2) with delta(sub 0) = 0.1, 0.04, and 0.0125 Byr for Earth, Venus, and Mars, respectively. After a R(exp 2) correction this means that outgassing processes on Venus and Mars are weaker than on Earth by factors of 3 and 30, respectively. Mass ratios of U and Th are almost the same for all three planets, while potassiumis depleted by a factor of 2 in Venus and Mars. Mass ratio of helium and argon are close to 5 x 10(exp -9) and 2 x 10(exp -8) g/g in the interiors of all three planets. The implications of these results are discussed.

  15. The Middle and Upper Atmosphere Observations over Syowa Station (69S, 39E), the Antarctic

    Science.gov (United States)

    Nakamura, Takuji; Tsutsumi, Masaki; Sato, Toru; Tomikawa, Yoshihiro; Yamanouchi, Takashi; Suzuki, Hidehiko; Ejiri, Mitsumu K.; Sato, Kaoru; Abo, Makoto; Nishiyama, Takanori; Matsuda, Takashi S.; Mizuno, Akira; Isono, Yasuko; Tsuda, Takuo T.

    Rayleigh signals. Resonance scatter lidar capability to extend the height coverage into the lower thermosphere is being developed and observations at mid-latitude has been started. Millimeter spectrometer has been observing both O3 and NO, and revealing seasonal and short term variabilities related to the solar activities and atmospheric circulations. Airglow imaging data has been extensively analyzed for clarifying behavior of short-period gravity waves in the MLT region. We expect the full-power operation planned in near future will establish a very powerful radio/optical observation core site for the middle and upper atmosphere studies as well as troposphere, at Syowa Station.

  16. Recent Activities on the Embrace Space Weather Regional Warning Center: the New Space Weather Data Center

    Science.gov (United States)

    Denardini, Clezio Marcos; Dal Lago, Alisson; Mendes, Odim; Batista, Inez S.; SantAnna, Nilson; Gatto, Rubens; Takahashi, Hisao; Costa, D. Joaquim; Banik Padua, Marcelo; Campos Velho, Haroldo

    2016-07-01

    the ionospheric profiles in two equatorial sites and in two low latitude sites; (b) several solar radio telescopes to monitor solar activity (under development); (c) the matrix of the GNSS TEC map over South America; (d) the Embrace Airglow All-sky Imagers Network (Embrace GlowNet); and (d) the Embrace Magnetometer Network (Embrace Magnet), all of them in South America. Also, the system allows subscription to space weather alerts and reports. Contacting Author: C. M. Denardini (clezio.denardin@inpe.br)

  17. Overview and Initial Results from the DEEPWAVE Airborne and Ground-Based Measurement Program

    Science.gov (United States)

    Fritts, D. C.

    2015-12-01

    The deep-propagating gravity wave experiment (DEEPWAVE) was performed on and over New Zealand, the Tasman Sea, and the Southern Ocean with core airborne measurements extending from 5 June to 21 July 2014 and supporting ground-based measurements spanning a longer interval. The NSF/NCAR GV employed standard flight-level measurements and new airborne lidar and imaging measurements of gravity waves (GWs) from sources at lower altitudes throughout the stratosphere and into the mesosphere and lower thermosphere (MLT). The new GV lidars included a Rayleigh lidar measuring atmospheric density and temperature from ~20-60 km and a sodium resonance lidar measuring sodium density and temperature at ~75-105 km. An airborne Advanced Mesosphere Temperature Mapper (AMTM) and two IR "wing" cameras imaged the OH airglow temperature and/or intensity fields extending ~900 km across the GV flight track. The DLR Falcon was equipped with its standard flight-level instruments and an aerosol Doppler lidar measuring radial winds below the Falcon. DEEPWAVE also included extensive ground-based measurements in New Zealand, Tasmania, and Southern Ocean Islands. DEEPWAVE performed 26 GV flights and 13 Falcon flights, and ground-based measurements occurred whether or not the aircraft were flying. Collectively, many diverse cases of GW forcing, propagation, refraction, and dissipation spanning altitudes of 0-100 km were observed. Examples include strong mountain wave (MW) forcing and breaking in the lower and middle stratosphere, weak MW forcing yielding MW penetration into the MLT having very large amplitudes and momentum fluxes, MW scales at higher altitudes ranging from ~10-250 km, large-scale trailing waves from orography refracting into the polar vortex and extending to high altitudes, GW generation by deep convection, large-scale GWs arising from jet stream sources, and strong MWs in the MLT arising from strong surface flow over a small island. DEEPWAVE yielded a number of surprises, among

  18. Deriving Atmospheric Properties and Escape Rates from MAVEN's Imaging UV Spectrograph (IUVS)

    Science.gov (United States)

    Schneider, Nicholas M.; IUVS Science Team

    2013-10-01

    MAVEN (Mars Volatile and Atmosphere EvolutioN) is a Mars Scout mission being readied for launch in November 2013. The key hardware and management partners are University of Colorado, Goddard Space Flight Center, University of California at Berkeley, Lockheed Martin, and the Jet Propulsion Laboratory. MAVEN carries a powerful suite of fields and particles instruments and a sophisticated remote sensing instrument, the Imaging UltraViolet Spectrograph (IUVS). This presentation begins by describing IUVS' science goals, instrument design, operational approach and data analysis strategy. IUVS supports the top-level MAVEN science goals: measure the present state of the atmosphere, observe its response to varying solar stimuli, and use the information to estimate loss from Mars' atmosphere over time. The instrument operates at low spectral resolution spanning the FUV and MUV ranges in separate channels, and at high resolution around the hydrogen Lyman alpha line to measure the D/H ratio in the upper atmosphere. MAVEN carries the instrument on an Articulated Payload Platform which orients the instrument for optimal observations during four segments of its 4.5 hr elliptical orbit. During periapse passage, IUVS uses a scan mirror to obtain vertical profiles of emissions from the atmosphere and ionosphere. Around apoapse, the instrument builds up low-resolution images of the atmosphere at multiple wavelengths. In between, the instrument measures emissions from oxygen, hydrogen and deuterium in the corona. IUVS also undertakes day-long stellar occultation campaigns at 2 month intervals, to measure the state of the atmosphere at altitudes below the airglow layer and in situ sampling. All data will be pipeline-processed from line brightnesses to column abundances, local densities and global 3-D maps. The focus of the presentation is development of these automatic processing algorithms and the data products they will provide to the Mars community through the PDS Atmospheres Node

  19. Exploring the interior structure of Venus with balloons and satellites

    Science.gov (United States)

    Mimoun, David; Cutts, Jim; Stevenson, Dave

    2015-04-01

    Although present daily in our sky as the brightest object at dusk and dawn, many characteristics of Venus remains a mystery. Its dense atmosphere hides the surface from orbital viewing, and the extreme conditions experienced at its surface (460°C, almost 100 bar of pressure at the surface) pose a formidable challenge to the sustained survival and operation of planetary landers. Despite their sharply contrasting atmospheres, Venus is not very different from Earth in size, its composition should be very similar, its orbit is very close to be circular and it is only a little closer to the Sun ( 0.7 A.U). So what are the processes that turned the twin sister of our planet into such a different object? And how can we better understand the processes that have shaped the terrestrial planets, and to understand their formation history? With its harsh surface environment, conventional seismology on Venus, requiring seismometers to be deployed at the surface for months or even years seems impractical. In June 2014, the Keck Institute for Space Studies (KISS) at the California Institute of Technology sponsored a one-week workshop with 30 specialists in the key techniques and technologies relevant to investigating Venus's interior structure focusing on alternative approaches to seismology . As the vertical component of surface motion on Venus is very efficiently coupled into the atmosphere as infrasonic waves, especially at low frequency, several alternative approaches to detecting seismic events can be considered. Seismo-acoustic waves propagate upwards producing pressure fluctuations in the middle atmosphere of Venus and the seismic wave energy is ultimately dissipated by local heating, ionospheric perturbation, or airglow. These atmospheric perturbations can therefore be recorded either in-situ (with a barometer network, deployed on balloons floating in the cloud layer near 55 km) or remotely via optical imaging or electromagnetic sounding deployed on a spacecraft. A report

  20. Thermospheric winds and temperatures above Mawson, Antarctica, observed with an all-sky imaging, Fabry-Perot spectrometer

    Directory of Open Access Journals (Sweden)

    C. Anderson

    2009-05-01

    Full Text Available A new all-sky imaging Fabry-Perot spectrometer has been installed at Mawson station (67°36' S, 62°52' E, Antarctica. This instrument is capable of recording independent spectra from many tens of locations across the sky simultaneously. Useful operation began in March 2007, with spectra recorded on a total of 186 nights. Initial analysis has focused on the large-scale daily and average behavior of winds and temperatures derived from observations of the 630.0 nm airglow line of atomic oxygen, originating from a broad layer centered around 240 km altitude, in the ionospheric F-region.

    The 1993 Horizontal Wind Model (HWM93, NRLMSISE-00 atmospheric model, and the Coupled Thermosphere/Ionosphere Plasmasphere (CTIP model were used for comparison. During the geomagnetically quiet period studied, observed winds and temperatures were generally well modelled, although temperatures were consistently higher than NRLMSISE-00 predicted, by up to 100 K. CTIP temperatures better matched our data, particularly later in the night, but predicted zonal winds which were offset from those observed by 70–180 ms−1 westward. During periods of increased activity both winds and temperatures showed much greater variability over time-scales of less than an hour. For the active night presented here, a period of 45 min saw wind speeds decrease by around 180 ms−1, and temperatures increase by approximately 100 K. Active-period winds were poorly modelled by HWM93 and CTIP, although observed median temperatures were in better agreement with NRLMSISE-00 during such periods.

    Average behavior was found to be generally consistent with previous studies of thermospheric winds above Mawson. The collected data set was representative of quiet geomagnetic and solar conditions. Geographic eastward winds in the afternoon/evening generally continued until around local midnight, when winds turned equatorward. Geographic meridional and

  1. Human Settlements in the South-Central U.S., Viewed at Night from the International Space Station

    Science.gov (United States)

    Dawson, Melissa; Evans, Cynthia; Stefanov, William; Wilkinson, M. Justin; Willis, Kimberly; Runco, Susan

    2012-01-01

    A recent innovation of astronauts observing Earth from the International Space Station (ISS) is documenting human footprints by photographing city lights at night time. One of the earliest night-time images from the ISS was the US-Mexico border at El Paso-Ciudad Juarez. The colors, patterns and density of city lights document the differences in the cultural settlement patterns across the border region, as well as within the urban areas themselves. City lights help outline the most populated areas in settlements around the world, and can be used to explore relative population densities, changing patterns of urban/suburban development, transportation networks, spatial relationship to geographic features, and more. The data also provides insight into parameters such as surface roughness for input into local and regional climate modeling and studies of light pollution. The ground resolution of night-time astronaut photography from the ISS is typically an order of magnitude greater than current Defense Meteorological Satellite Program (DMSP) data, and therefore can serve as a "zoom lens" for selected urban areas. Current handheld digital cameras in use on the ISS, optimized for greater light sensitivity, provide opportunities to obtain new detailed imagery of atmospheric phenomena such as airglow, aurora, and noctilucent clouds in addition to documenting urban patterns. ISS astronauts have taken advantage of increasingly sensitive digital cameras to document the world at night in unprecedented detail. In addition, the capability to obtain time-lapse imagery from fixed cameras has been exploited to produce dynamic videos of both changing surface patterns around the world and atmospheric phenomena. We will profile some spectacular images of human settlements over the South-Central U.S., and contrast with other images from around the world. More data can be viewed at http://eol.jsc.nasa.gov/Videos/CrewEarthObservationsVideos/. US-Mexico border is obvious by the different

  2. A study of mid-latitude 5577[angstrom] OI dayglow emissions

    Energy Technology Data Exchange (ETDEWEB)

    Hume, E.E. Jr.

    1992-01-01

    The green line (5577[angstrom]) is a bright, persistent component of the visible airglow produced by an electric quadrupole transition from the meta-stable second excited state ([sup 1]S[sub 0]) to the first excited state ([sup 1]D[sub 2]) of atomic oxygen. In this thesis, production and loss mechanisms important to the F-region dayglow 5577[angstrom] emission are investigated. Four major source reactions need to be incorporated in the modeling of the emission profile, photoelectron impact on atomic oxygen, dissociative recombination of O[sup +][sub 2], quenching of N[sub 2](A[sup 3][Sigma][sub u][sup +]) by atomic oxygen, and photo-dissociation of O[sub 2]. For some of the reactions, the properties of the rate coefficients, branching ratios, and cross sections are not well known. Models are used to determine the rate coefficients, branching ratios, and cross sections for these reactions. The impact of photoelectrons on atomic oxygen is the primary source of 5577[angstrom] dayglow emission in the thermosphere. The quenching of N[sub 2](A) by atomic oxygen is an important source of the 5577[angstrom] emission at the peak in the layer. The total quenching rate was determined using a vibrational model and a band model for N[sub 2] to study emissions at 3371[angstrom] from the Atmosphere Explorer satellite. The value of the rate coefficient deduced here agrees well with experimental values by Piper and Caledonia (1981) and Thomas and Kaufman (1985). The effective branching ratio determined by this study tends to support the results from Piper (1982) and De Souza et al. (1985). The effect of the distribution of the vibrational population of the N[sub 2](A[sup 3][Sigma][sub u][sup +]) state on the branching ratio is also discussed. The extension of the dayglow photochemistry into the twilight is also investigated. The model developed for the dayglow can reasonably reproduce the rapidly changing twilight emissions.

  3. State-to-state measurements of low-energy ion-molecule and ion-ion collisions by three dimensional momentum imaging

    Science.gov (United States)

    Urbain, Xavier

    2016-09-01

    While the measurement of total absolute cross sections remains challenging, the insight provided by differential cross sections and branching ratios is invaluable to assess the quality of theoretical predictions. Satisfactory agreement at the latter level gives better confidence in the proper identification of the reaction mechanism and key parameters. The three dimensional imaging of molecular dissociation, and more generally, the determination of all momentum vectors of the reaction products, gives direct access to the differential quantities of interest. For the prototype reaction of a proton colliding with H2, the secondary H2+current may be recorded to provide the total charge transfer yield. The dissociative charge transfer of the product ions with alkali targets leaves a characteristic signature in the total kinetic energy imparted to the H fragments. Its measurement is readily achieved by coincident detection on position sensitive detectors. This allows us to extract vibrational populations as a function of collision energy. A resonant enhancement of the charge transfer around 45 eV/amu is observed, that leaves the molecular ion in its vibrational ground state. Those observations are supported by state-of-the-art calculations. We have similarly explored the ionization of molecular oxygen by proton and alpha particle impact, at velocities characteristic of the solar wind. A somewhat more involved vibrational analysis of the O2+cations indicates a Franck-Condon like vibrational population of the ground electronic state from 50 eV to 10 keV, unlikely to modify the branching ratios of dissociative recombination, itself responsible for airglow emissions. More interestingly, a significant population of the 4Πu excited state is measured at velocities typical of the fast solar wind. Finally, we shall address the implementation of three dimensional imaging in merged ion-ion beam studies. Mutual neutralization involving anions and cations is a very efficient process

  4. Observations of day-to-day variability in precursor signatures to equatorial F-region plasma depletions

    Directory of Open Access Journals (Sweden)

    P. R. Fagundes

    its behaviour.

    Key words. Atmospheric composition and structure (airglow and aurora · Ionosphere (equatorial ionosphere; ionospheric irregularities

  5. Utah Valley University Field Station at Capitol Reef National Park: A Venue for Improved Student Learning and Retention

    Science.gov (United States)

    Nielsen, K.; Schultz, M.; Williams, B.; Gay, J.; Johnson, S.; Dunn, P.

    2015-12-01

    faint upper atmospheric airglow emissions. This presentation details the upper atmospheric undergraduate educational program at UVU, and will also include a section regarding the newly established interdisciplinary air pollution educational program, and how communities outside of UVU can use the facility.

  6. Identification of gravity wave sources using reverse ray tracing over Indian region

    Directory of Open Access Journals (Sweden)

    M. Pramitha

    2014-07-01

    Full Text Available Reverse ray tracing method is successfully implemented for the first time in the Indian region for identification of the sources and propagation characteristics of the gravity waves observed using airglow emissions from Gadanki (13.5° N, 79.2° E and Hyderabad (17.5° N, 78.5° E. Wave amplitudes are also traced back for these wave events by including both radiative and diffusive damping. Background temperature and wind data obtained from MSISE-90 and HWM-07 models, respectively, are used for the ray tracing. For Gadanki region suitability of these models is tested. Further, a climatological model of background atmosphere for Gadanki region has been developed using a long-term of nearly 30 years of observations available from a variety of ground-based (MST radar, radiosonde, MF radar, rocket-, and satellite-borne measurements. For considering real-time atmospheric inputs, ERA-Interim products are utilized. By this reverse ray method, the source locations for nine wave events could be identified to be in the upper troposphere, whereas, for five other events the waves seem to have been ducted in the mesosphere itself. Uncertainty in locating the terminal points in the horizontal direction is estimated to be within 50–100 and 150–300 km for Gadanki and Hyderabad wave events, respectively. This uncertainty arises mainly due to non-consideration of the day-to-day variability in tidal amplitudes. As no convection in-and-around the terminal points are noticed, it is unlikely to be the source. Interestingly, large (~9 m s−1 km−1 vertical shear in the horizontal wind is noted near the ray terminal points (at 10–12 km altitude and is identified to be the source for generating the nine wave events. Conditions prevailing at the terminal points for each of the 14 events are also provided. These events provide leads to a greater understanding of the tropical lower and upper atmospheric coupling through gravity waves.

  7. CIBER : a near-infrared probe of the epoch of reionization

    Science.gov (United States)

    Sullivan, Ian Sorensen

    The Cosmic Infrared Background Experiment (CIBER) is a NASA sounding rocket payload that was first launched in February 2009. CIBER consists of four co-aligned instruments designed to study the near-Infrared background by measuring fluctuations and the absolute spectrum. The platform of a sounding rocket enables observations of the near-Infrared background outside of narrow atmospheric windows that are uncontaminated by airglow. CIBER uses two spectrometers to measure the absolute brightness spectrum of the extragalactic near-Infrared background. One, a high-resolution Fabry-Perot spectometer, is tuned to the 854.5 nm CaII line of the solar spectrum, and is designed to measure the absolute brightness of the Zodiacal Light directly, which is the source of greatest uncertainty in the near-Infrared background spectrum. The second spectrometer measures the near-Infrared background spectrum from 700 nm to 1800 nm, spanning the wavelength range where a Lyman limit cutoff feature from reionization could appear. CIBER also houses two Infrared imaging telescopes, which have identical optics that give 2 x 2 degree field of views with 7 arcsecond pixels, but have different band defining filters. The first imager has a wide band centered at 1600 nm, and images the background at the expected peak of the spectrum. The imagers?~@~Y wide field of view allows them to measure the distinctive power spectrum of first-light galaxy fluctuations peaking at 10 arcminutes. The second imager has a wide band centered at 1000 nm that is intended to image at wavelengths shorter than the Lyman cutoff, and provides a powerful systematic test for any detection made at 1600 nm. First-light fluctuations should have a distinctive spatial power spectrum with very red 1600 nm / 1000 nm color, distinctly redder than the approximately solar color of any residual fluctuations arising from Zodiacal light, Galactic starlight, or moderate-redshift galaxies. This work describes the design and

  8. Determining the 630nm emission altitude using modelling and observations from a tristatic configuration of Fabry-Perot Interferometers and EISCAT radars.

    Science.gov (United States)

    Aruliah, Anasuya; Kosch, Michael

    Anasuya Aruliah, a.aruliah@ucl.ac.uk University College London, London, United Kingdom Michael Kosch, m.kosch@lancaster.ac.uk Lancaster University, Lancaster, United Kingdom Tristatic team Anasuya Aruliah,Ho-Ching Iris Yiu,Ian McWhirter, Michael Kosch,Kazuo Shiokawa,Shin-ichiro Oyama,Satonori Nozawa,Vikki Howells,Ian McCrea During early February 2010 a tristatic FPI-EISCAT experiment was run in order to investigate the peak emission altitude of the 630nm airglow and auroral emission in the region of the auroral oval. Two UCL Fabry-Perot Interferometers and a new STEL FPI have been located close to the three EISCAT radars at Tromsø, Kiruna and Sodankylü. The radars were pointed a at a common volume seen by all three FPIs, on assuming a peak emission height of 235km. This altitude is generally assumed to be fairly steady for FPI studies probing the behaviour of the upper atmosphere, though the height is a little different at other latitudes. The smoothing effect of the large viscosity of the upper thermosphere is invoked as a reason why the actual altitude is not too important, and there has been little investigation of the appropriateness of this assumption. However, mesoscale variability in the ionosphere has now been identified as producing a similar quantity of heating as does steady state convection; and FPIs and the CHAMP satellite have shown mesoscale structure in the high-latitude thermosphere. This indicates a need to revisit old assumptions that were based on the premise of thermospheric variability being large-scale. The STEL FPI at Ramfjord has a fully variable pointing direction mechanism and was programmed to point rapidly at successive volumes that would overlap the UCL KEOPS/Kiruna FPI look direction if the emission volume was 195km, 215km, 235km and 255km. Cross-correlation of the temperatures and intensity measurements would then identify the peak emission height. The EISCAT radar provided ionospheric parameters to model the 630nm emission profile

  9. TIMED Science With the Space Physics Data Facility's (SPDF) Data and Models Services

    Science.gov (United States)

    Bilitza, D.; McGuire, R. E.; Kovalick, T.; Candey, R. M.; Leckner, H.

    2005-12-01

    NASA's Space Physics Data Facility (SPDF) provides access to a large volume of data and models that are of relevance to Ionospheric, Thermospheric and Mesospheric (ITM) physics and to the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) mission in particular. SPDF has developed a number of web systems to facilitate user access to important data and model resources and is making these services available through Web Services (or Application Programming Interfaces, API) directly to applications such as VxOs. The Coordinated Data Analysis web (CDAWeb) provides access to data from most of NASA's currently operating space science satellites and many of the earlier missions covering the full expanse of the Earth-Sun system from mesosphere to heliosphere. CDAWeb lets user plot data using a wide range of parameter display options including mapped images and movies; capabilities also include parameter listings and data downloads in CDF and ASCII format. TIMED data display options, for example, include GUVI airglow intensities and TIDI neutral wind vectors in a transverse Mercator projection that shows simultaneously both poles and the equatorial region. Coupled with CDAWeb's comprehensive coverage of solar wind parameters the TIMED data will provide new insights into the ITM response to solar and magnetic storms. SPDF's SSCWeb interface enables users to plot orbits for the majority of space physics satellites and to query for magnetic field line conjunctions between multiple spacecraft and ground stations and for magnetic region occupancy and thus enables coordinates science investigation between TIMED and CEDAR ground stations. Recently an Interactive 3-D orbit viewer was added to SSCWeb. Access to legacy data from older ITM satellite missions is provided through the ATMOWeb browse and download system enabling the study of solar cycle effects on ITM parameters. SPDF's Modelweb service is the front-end to a unique collection of solar-terrestrial databased

  10. The S-NPP VIIRS Day-Night Band On-Orbit Calibration/Characterization and Current State of SDR Products

    Directory of Open Access Journals (Sweden)

    Shihyan Lee

    2014-12-01

    Full Text Available The launch of VIIRS on-board the Suomi-National Polar-orbiting Partnership (S-NPP on 28 October 2011, marked the beginning of the next chapter on nighttime lights observation started by the Defense Meteorological Satellite Program’s (DMSP OLS sensor more than two decades ago. The VIIRS observes the nighttime lights on Earth through its day-night band (DNB, a panchromatic channel covering the wavelengths from 500 nm to 900 nm. Compared to its predecessors, the VIIRS DNB has a much improved spatial/temporal resolution, radiometric sensitivity and, more importantly, continuous calibration using on-board calibrators (OBCs. In this paper, we describe the current state of the NASA calibration and characterization methodology used in supporting mission data quality assurance and producing consistent mission-wide sensor data records (SDRs through NASA’s Land Product Evaluation and Analysis Tool Element (Land PEATE. The NASA calibration method utilizes the OBCs to determine gains, offset drift and sign-to-noise ratio (SNR over the entire mission. In gain determination, the time-dependent relative spectral response (RSR is used to correct the optical throughput change over time. A deep space view acquired during an S-NPP pitch maneuver is used to compute the airglow free dark offset for DNB’s high gain stage. The DNB stray light is estimated each month from new-moon dark Earth surface observations to remove the excessive stray light over the day-night terminators. As the VIIRS DNB on-orbit calibration is the first of its kind, the evolution of the calibration methodology is evident when the S-NPP VIIRS’s official calibrations are compared with our latest mission-wide reprocessing. In the future, the DNB calibration methodology is likely to continue evolving, and the mission-wide reprocessing is a key to providing consistently calibrated DNB SDRs for the user community. In the meantime, the NASA Land PEATE provides an alternative source to obtain

  11. Subauroral red arcs as a conjugate phenomenon: comparison of OV1-10 satellite data with numerical calculations

    Directory of Open Access Journals (Sweden)

    A. V. Pavlov

    Full Text Available This study compares the OV1-10 satellite measurements of the integral airglow intensities at 630 nm in the SAR arc regions observed in the northern and southern hemisphere as a conjugate phenomenon, with the model results obtained using the time-dependent one-dimensional mathematical model of the Earth ionosphere and plasmasphere (the IZMIRAN model during the geomagnetic storm of the period 15–17 February 1967. The major enhancements to the IZMIRAN model developed in this study are the inclusion of He+ ions (three major ions: O+, H+, and He+, and three ion temperatures, the updated photochemistry and energy balance equations for ions and electrons, the diffusion of NO+ and O2+ ions and O(1D and the revised electron cooling rates arising from their collisions with unexcited N2, O2 molecules and N2 molecules at the first vibrational level. The updated model includes the option to use the models of the Boltzmann or non-Boltzmann distributions of vibrationally excited molecular nitrogen. Deviations from the Boltzmann distribution for the first five vibrational levels of N2 were calculated. The calculated distribution is highly non-Boltzmann at vibrational levels v > 2 and leads to a decrease in the calculated electron density and integral intensity at 630 nm in the northern and southern hemispheres in comparison with the electron density and integral intensity calculated using the Boltzmann vibrational distribution of N2. It is found that the intensity at 630 nm is very sensitive to the oxygen number densities. Good agreement between the modelled and measured intensities is obtained provided that at all altitudes of the southern hemisphere a reduction of about factor 1.35 in MSIS-86 atomic oxygen densities is included in the IZMIRAN model with the non-Boltzmann vibrational distribution of N2

  12. Laboratory Study of O2(b1Σ g+, υ = 1) Collisional Removal at Thermospheric Temperatures

    Science.gov (United States)

    Wouters, E. R.; Pejaković, D. A.; Phillips, K. E.; Kalogerakis, K. S.

    2003-12-01

    In the Earth's thermosphere, energy transfer from O(1D) to O2 generates oxygen molecules in the υ = 0 and 1 levels of the O2(b1Σg+) state. The emissions in the O2(b1Σ g+ - X3Σ g-) system (Atmospheric Band) present a major component of the Earth's airglow. Interpretation of the measured intensities of O2 Atmospheric Band emissions can yield altitude profiles of oxygen atom density and local temperature in the lower thermosphere. To achieve this goal accurate laboratory measurements of the collisional removal rate coefficients of O2(b, υ = 1) and their temperature dependence are essential. Atmospheric observations suggest that the relevant colliders for the removal of O2(b, υ = 1) in the lower thermosphere are O2 and O(3P). We report measurements of the rate coefficients for the collisional removal of O2(b, υ = 1) by O2, N2, and CO2, at temperatures in the range 300--1000 K. A state-specific two-laser technique is used, in which the visible output of the first laser directly excites O2 to O2(b, υ = 1), and the ultraviolet output of the second laser probes the O2(b, υ = 1) population by resonantly enhanced multiphoton ionization via the υ= 4 level of the d1Π g Rydberg state. The temporal evolution of the O2(b, υ = 1) population is monitored by varying the time delay between the two laser pulses. The rate coefficient of the collisional removal of O2(b, υ = 1) by O2 increases monotonically with temperature from about 1.5 x 10-11 cm3 s-1 to about 6*E-11 cm3 s-1 in the range 300--1000 K. Experiments with colliders N2 and CO2 determine the upper limits for the removal rate coefficients of O2(b, υ = 1) by N2 and CO2 to be 2 orders of magnitude smaller. This work extends previous studies of O2(b, υ = 1) at room and low temperatures.1,2 We are currently planning experiments to investigate the collisional removal of O2(b, υ = 1) by O atoms. This study was supported by the NSF's Grant ATM-0209229. The participation of K. Phillips in this project was funded by

  13. Expected first-order effects of a notional equatorial ring on Earth's night sky: a geometric consideration

    Science.gov (United States)

    Hancock, L. O.

    2013-12-01

    : a schema of ring effects on the southern sky: (i) extinction of extra-terrestrial light between celestial equator and horizon; (ii) brightening of extra-terrestrial light via light-through-dust effects near the southern horizon; and (iii) reflection of sunlight from celestial equator to horizon. These effects would be modulated by season (due to ring self-shadowing) and hour of the night (because of Earth's shadow). We suggest that the expected effects are not "missing" at all - similar effects are well known to observers but are taken to be fully accounted for by skyglow, airglow and light pollution, qualitatively similar phenomena that certainly exist. We conclude that ground-based observers' non-identification of an equatorial ring is not a counter-indicator of a ring's existence. As far as this consideration goes, the question of an Earth ring system is open.

  14. Multi-wavelength imaging observations of plasma depletions over Kavalur, India

    Directory of Open Access Journals (Sweden)

    H. S. S. Sinha

    small regions in the northern part of the image and then in about 90 min time, they attain their peak brightness and encompass the entire field-of-view in about 2 hrs 30 min. In some cases, brightness patterns contain one or two well developed plasma depletions within them. (f The brightness patterns reported here differ from the earlier observations in that they do not show any differential behaviour in the direction of movement before and after the midnight, and that they are present for extended periods of time as large as 6 hrs.

    Key words. Atmospheric composition and structure (air-glow and aurora; Ionosphere (equatorial ionosphere; ionospheric irregularities

  15. Initial Results from the DEEPWAVE Airborne and Ground-Based Measurement Program in New Zealand in 2014

    Science.gov (United States)

    Fritts, Dave; Smith, Ron; Taylor, Mike; Doyle, Jim; Eckermann, Steve; Dörnbrack, Andreas; Rapp, Markus; Williams, Biff; Bossert, Katrina; Pautet, Dominique

    2015-04-01

    The deep-propagating gravity wave experiment (DEEPWAVE) was performed on and over New Zealand, Tasmania, the Tasman Sea, and the Southern Ocean with core airborne measurements extending from 5 June to 21 July 2014 and supporting ground-based measurements beginning in late May and extending beyond the airborne component. DEEPWAVE employed two aircraft, the NSF/NCAR GV and the German DLR Falcon. The GV carried the standard flight-level instruments, dropsondes, and the Microwave Temperature Profiler (MTP). It also hosted new airborne lidar and imaging instruments built specifically to allow quantification of gravity waves (GWs) from sources at lower altitudes (e.g., orography, convection, jet streams, fronts, and secondary GW generation) throughout the stratosphere and into the mesosphere and lower thermosphere (MLT). The new GV lidars included a Rayleigh lidar measuring atmospheric density and temperature from ~20-60 km and a sodium resonance lidar measuring sodium density and temperature at ~75-100 km. An airborne Advanced Mesosphere Temperature Mapper (AMTM) was also developed for the GV, and together with additional IR "wing" cameras, imaged the OH airglow temperature and/or intensity fields extending ~900 km across the GV flight track. The DLR Falcon was equipped with its standard flight-level instruments and an aerosol Doppler lidar able to measure radial winds below the Falcon where aerosol backscatter was sufficient. Additional ground-based instruments included a 449 MHz boundary layer radar, balloons at multiple sites, two ground-based Rayleigh lidars, a second ground-based AMTM, a Fabry Perot interferometer measuring winds and temperatures at ~87 and 95 km, and a meteor radar measuring winds from ~80-100 km. DEEPWAVE performed 26 GV flights, 13 Falcon flights, and an extensive series of ground-based measurements whether or not the aircraft were flying. Together, these observed many diverse cases of GW forcing, propagation, refraction, and dissipation

  16. A Balloon-Borne Telescope System for Planetary Atmosphere and Plasma Studies

    Science.gov (United States)

    Taguchi, M.; Yoshida, K.; Sakamoto, Y.; Kanazawa, T.; Shoji, Y.; Sawakami, T.; Takahashi, Y.; Hoshino, N.; Sato, T.; Sakanoi, T.

    2007-12-01

    A telescope floating in the polar stratosphere can continuously monitor planets for more than 24 hours. Thin, clear and stable air of the stratosphere makes it possible to observe planets in a condition free from cloud with fine seeing and high atmospheric transmittance. Moreover, a balloon-borne telescope system is less expensive compared with a huge terrestrial telescope or a direct planetary probe mission. Targets of a balloon-borne telescope system will extend over various atmospheric and plasma phenomena on almost all the planets, i.e., a sodium tail of Mercury, lightning, airglow and aurora in the atmospheres of Venus, Jupiter and Saturn, escaping atmospheres of the Earth-type planets, satellite-induced luminous events in the Jovian atmosphere, etc. The first target is global dynamics of the Venusian atmosphere by detecting cloud motion in UV and NIR imagery. A decoupling mechanism and a pair of control moment gyros (CMGs) are mounted at the top of the gondola. The decoupling mechanism isolates the gondola from a balloon and also transfers an excess angular momentum of the CMGs to the balloon. The attitude of the gondola is stabilized at a constant sun azimuthal angle so that a solar cell panel faces to the sun. A 300 mm F30 Schmidt-Cassegrain telescope is installed at the bottom of the gondola. DC/DC converters, a PC, a high voltage power supply for a piezo-electrically moving mirror and digital video recorders are contained in a sealed cell. The azimuthal angle is detected by a sun-sensor. A PC processes sensor output to control DC motors used in the decoupling mechanism and CMGs with an accuracy in azimuthal attitude of about 0.5 deg. The two-axis gimbal mount of the telescope is controlled by the same PC, guiding an object within a field-of-view of a guide telescope. Residual tracking error is detected by a position sensitive photomultiplier tube and corrected by the two-axis moving mirror installed in the optical system. The optical path is divided into

  17. Deuterated Methane and Ethane in the Atmosphere of Jupiter

    Science.gov (United States)

    Parkinson, C. D.; Yung, Y. L.; Lee, A. Y.; Crisp, D.

    2003-12-01

    been calculated using the Caltech/JPL KINETICS 1-D photochemistry-diffusion model with the column H constrained using the H lyman-alpha airglow. Reactions involving C2H5D are described by Parkinson (2002). Performing sensitivity studies, we have found an enhancement of greater than two orders of magnitude in C2H5D due to the vibrational chemistry, which is significantly larger than that for CH3D enhancement reported by Parkinson et al (2003). This is of great interest and suggests that C2H5D should be detectable in the lower thermosphere: we propose that observations of this species should be made. Enhancement of deuterated hydrocarbons indicates that there may be exchange of these species between the statosphere and troposphere and further show their usefulness as isotopic tracers in the Jovian atmosphere.

  18. Identification of Gravity wave Sources over Tropical Latitudes Using Reverse Ray Tracing technique

    Science.gov (United States)

    Venkat Ratnam, Madineni; Pramitha, M.

    2016-07-01

    Sources and propagation characteristics of high-frequency gravity waves (GWs) observed in the mesosphere using airglow emissions from Gadanki (13.5oN, 79.2oE) and Hyderabad (17.5oN, 78.5oE) are investigated using reverse ray tracing. Wave amplitudes are also traced back, including both radiative and diffusive damping. For this a climatological model of the background atmosphere for the Gadanki region has been developed using nearly 30 years of observations available from a variety of ground based (MST radar, radiosondes, MF radar) and rocket- and satellite-borne measurements. With the reverse ray-tracing method, the source locations for wave events could be identified to be in the upper troposphere. Uncertainty in locating the terminal points of wave events in the horizontal direction is estimated to be within 50-100 km and 150-300 km for Gadanki and Hyderabad wave events, respectively. This uncertainty arises mainly due to non-consideration of the day-to-day variability in the tidal amplitudes. Interestingly, large (~9ms-1 km-1) vertical shears in the horizontal wind are noticed near the ray terminal points (at 10-12 km altitude) and are thus identified to be the source for generating the observed high phase- speed, high-frequency GWs. We also tried to identify the sources for the GWs which are observed during Indo-French campaign conducted during May 2014. Uniqueness of the present study lies in using near-real time background atmosphere data from simultaneous radiosonde and meteor radar covering both source and propagation/dissipation regions of GWs. When we searched for the sources near the terminal points, deep convection is found to be a source for these events. We also tried to identify the sources of inertia-gravity waves (IGWs) that are observed in the troposphere and lower stratosphere during different seasons using long-term (2006-2014) high resolution radiosonde observations. In general, 50% of the waves observed over this location have convection as

  19. Obituary: Herbert Gursky, 1930-2006

    Science.gov (United States)

    Doschek, George; Dahlburg, Jill

    2007-12-01

    imaging telescope (EIT) on the ESA/NASA Solar and Heliospheric Observatory. These experiments have shed considerable light on how solar activity affects the near-Earth environment with many potential space weather applications. In high-energy astronomy, Dr. Gursky made many contributions. He provided scientific oversight for the Advanced Research and Global Observation Satellite (ARGOS) Space Test Program spacecraft that contained five NRL instruments: the Unconventional Stellar Aspect (USA) experiment, the Global Imaging Monitor of the Ionosphere (GIMI), the High Resolution Airglow/Aurora Spectroscopy (HIRAAS) experiment, the Extreme Ultraviolet Imaging Photometer (EUVIP), and the Coherent Electromagnetic Radio Tomography (CERTO) instrument. He continued his interest in X-ray astronomy with the USA experiment, which obtained observations of many celestial sources such as galactic binary X-ray sources and pulsars. Always with an eye toward applications, Dr. Gursky was interested in using X-ray sources, specifically X-ray pulsars, as precise clocks to provide spacecraft with autonomous timing and navigation. Dr. Gursky also supported research in gamma ray astrophysics, such as the development of NRL's Oriented Scintillation Spectrometer Experiment (OSSE) for the NASA Compton Gamma Ray Observatory (CGRO) satellite, and analysis of solar flare gamma ray spectra obtained from the NASA Solar Maximum Mission. In atmospheric science, Dr. Gursky particularly encouraged practical applications of basic research. He recognized the importance of remote sensing for space weather, which resulted in the development at NRL of operational ultraviolet sensors on Defense Meteorological Satellite Program (DMSP) spacecraft that are now providing environmental data products to the Air Force Space Weather Agency. He initiated a program in middle atmosphere research that has been enormously successful and has spawned numerous experimental and theoretical advances, such as the Middle Atmosphere