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2009-01-01
Observations of the high-mass star-forming region AFGL 2591 reveal a large abundance of CO+, a molecule known to be enhanced by far-ultraviolet (FUV) and X-ray irradiation. In chemical models assuming a spherically symmetric envelope, the volume of gas irradiated by protostellar FUV radiation is very small due to the high extinction by dust. The abundance of CO+ is thus underpredicted by orders of magnitude. In a more realistic model, FUV photons can escape through an outflow region and irradiate gas at the border to the envelope. Thus, we introduce the first two-dimensional axisymmetric chemical model of the envelope of a high-mass star-forming region to explain the CO+ observations as a prototypical FUV tracer. The model assumes an axisymmetric power-law density structure with a cavity due to the outflow. The local FUV flux is ...
Multidimensional chemical modelling, II. Irradiated outflow walls
2009-06-04
Observations of the high-mass star forming region AFGL 2591 reveal a large abundance of CO+, a molecule known to be enhanced by far UV (FUV) and X-ray irradiation. In chemical models assuming a spherically symmetric envelope, the volume of gas irradiated by protostellar FUV radiation is very small due to the high extinction by dust. The abundance of CO+ is thus underpredicted by orders of magnitude. In a more realistic model, FUV photons can escape through an outflow region and irradiate gas at the border to the envelope. Thus, we introduce the first 2D axi-symmetric chemical model of the envelope of a high-mass star forming region to explain the CO+ observations as a prototypical FUV tracer. The model assumes an axi-symmetric power-law density structure with a cavity due to the outflow. The local FUV flux is calculated by a Monte Carlo radiative transfer code taking scattering on dust into account. A grid of precalculated chemical abundances, introduced in the first part of this series of papers, is used to quickly interpolate chemical abundances. This approach allows to calculate the temperature structure of the FUV heated outflow walls self-consistently with the chemistry. Synthetic maps of the line flux are calculated using a raytracer code. Single-dish and interferometric observations are simulated and the model results are compared to published and new JCMT and SMA observations. The two-dimensional model of AFGL 2591 is a ble to reproduce the JCMT single-dish observations and also explains the non-detection by the SMA. We conclude that the observed CO+ line flux and its narrow width can be interpreted by emission from the warm and dense outflow walls irradiated by protostellar FUV radiation.
Rubidium transport in X-irradiated human erythrocytes
1985-01-01
Outflow of 86Rb, a radioactive analogue of potassium, from human erythrocytes X-irradiated in vitro was studied with the following results. (1) The 86Rb level in the supernatants of irradiated and control cell suspensions reflected mainly 86Rb outflow and much less its active re-uptake. (2) The effect of irradiation on 86Rb outflow was more pronounced at a low temperature (40C) than at 370C. The lowest dose of X-irradiation exhibiting a significant effect on 86Rb outflow at 40C was 2.5 Gy. (3) K/Rb exchange did not seem to play an appreciable role in radiation-induced 86Rb outflow. (4) Calcium and its accumulation in irradiated cells was not found to be the cause of the effect of radiation on 86Rb outflow. (5) The effect of radiation on 86Rb ...
2010-06-16
(Abridged) We have conducted a study of [NeII] line emission based on a sample of 92 pre-main sequence stars mostly belonging to the infrared Class II, including 13 accreting transition disk objects and 14 objects driving jets and outflows. We find several significant correlations between L[NeII] and stellar parameters, in particular LX and the wind mass loss rate, dM/dt. Most correlations are, however, strongly dominated by systematic scatter. While there is a positive correlation between L[NeII] and LX, the stellar mass accretion rate, dMacc/dt, induces a correlation only if we combine the largely different subsets of jet sources and stars without jets. Our results suggest that L[NeII] is bi-modally distributed, with separate distributions for the two subsamples. The jet sources show systematically higher L[NeII], by 1-2 orders of magnitude with respect to objects without jets. Jet-driving stars also tend to show higher mass accretion rates. We therefore hypothesize that the trend with dMacc/dt reflects a trend with dM/dt that is more physically relevant for [NeII] emission. L[NeII] measured for objects without known outflows and jets is found to agree with simplified calculations of [NeII] emission from disk surface layers if the measured stellar X-rays are responsible for heating and ionizing of the gas. The large scatter in L[NeII] may be introduced by variations of disk properties and the irradiation spectrum, as previous ly suggested. The systematically enhanced [NeII] flux from jet sources clearly suggests a role for the jets themselves, as previously demonstrated by a spatially resolved observation of the outflow system in the T Tau triple.
On the Origin of the Lightest Molybdenum Isotopes
We discuss implications of recent precision measurements for the {sup 93}Rh proton separation energy for the production of the lightest molybdenum isotopes in proton-rich type II supernova ejecta. It has recently been shown that a novel neutrino-induced process makes these ejecta a promising site for the production of the light molybdenum isotopes and other 'p-nuclei' with atomic mass near 100. The origin of these isotopes has long been uncertain. A distinguishing feature of nucleosynthesis in neutrino-irradiated outflows is that the relative production of {sup 92}Mo and {sup 94}Mo is set by a competition governed by the proton separation energy of {sup 93}Rh. We use detailed nuclear network calculations and the recent experimental results for this proton separation energy to place constraints on the outflow characteristics that produce the lightest molybdenum isotopes in their solar proportions. It is found that for the conditions calculated in recent two-dimensional supernova simulations, and also for a large range of outflow characteristics around these conditions, the solar ratio of {sup 92}Mo to {sup 94}Mo cannot be achieved. This suggests that either proton-rich winds from type II supernova do not exclusively produce both isotopes, or that these winds are qualitatively different than calculated in today's supernova models.
On the Origin of the Lightest Molybdenum Isotopes
2007-10-24
We discuss implications of recent precision measurements for the {sup 93}Rh proton separation energy for the production of the lightest molybdenum isotopes in proton-rich type II supernova ejecta. It has recently been shown that a novel neutrino-induced process makes these ejecta a promising site for the production of the light molybdenum isotopes and other 'p-nuclei' with atomic mass near 100. The origin of these isotopes has long been uncertain. A distinguishing feature of nucleosynthesis in neutrino-irradiated outflows is that the relative production of {sup 92}Mo and {sup 94}Mo is set by a competition governed by the proton separation energy of {sup 93}Rh. We use detailed nuclear network calculations and the recent experimental results for this proton separation energy to place constraints on the outflow characteristics that produce the lightest molybdenum isotopes in their solar proportions. It is found that for the conditions calculated in recent two-dimensional supernova simulations, and also for a large range of outflow characteristics around these conditions, the solar ratio of {sup 92}Mo to {sup 94}Mo cannot be achieved. This suggests that either proton-rich winds from type II supernova do not exclusively produce both isotopes, or that these winds are qualitatively different than calculated in today's supernova models.
Results from DROXO. II. - [Ne II] and X-ray emission from Rho Ophiuchi young stellar objects
2009-06-26
The infrared [Ne II] and [Ne III] fine structure lines at 12.81um and 15.55um are predicted to trace the circumstellar disk gas subject to X-ray heating and ionization. We investigate the origin of these lines by comparing observations with models of X-ray irradiated disks and by searching for empirical correlations between the line luminosities and stellar and circumstellar parameters. We measure neon line fluxes and X-ray luminosities for 28 young stellar objects in the Rho Ophiuchi star formation region for which good quality infrared spectra and X-ray data have been obtained, the former with the Spitzer IRS and the latter with the Deep Rho Ophiuchi XMM-Newton Observation. We detect the [Ne II] and the [Ne III] lines in 10 and 1 cases, respectively. Line luminosities show no correlation with X-ray emission. The luminosity of the [Ne II] line for one star, and that of both the [Ne II] and [Ne III] lines for a second star, match the predictions of published models of X-ray irradiated disks; for the remaining 8 objects the [Ne II] emission is 1-3 dex higher than predicted on the basis of their L_X. Class I objects show significantly stronger [Ne II] lines than Class II and Class III ones. A correlation is moreover found between the [Ne II] line emission and the disk mass accretion rates. This might point toward a role of accretion-generated UV emission in the generation of the line or to other mechanisms related to mass inflows from circumstellar disks and envelopes and/or to the associated mass outflows (winds and jets). We conclude that the X-ray luminosity is not the only parameter that determines the [Ne II] emission. Explaining the strong [Ne II] emission of Class I objects likely requires the inclusion in the models of additional physical components such as the envelope, inflows, and outflows.
The origin of the [C II] emission in the S140 photon-dominated regions. New insights from HIFI
Using Herschel's HIFI instrument, we observe C ii along a cut through S140, as well as high-J transitions of CO and HCO+ at two positions on the cut, corresponding to the externally irradiated ionization front and the embedded massive star-forming core IRS1. The HIFI data were combined with available ground-based observations and modeled using the KOSMA-? model for photon-dominated regions (PDRs). We derive the physical conditions in S140 and in particular the origin of C ii emission around IRS1. We identify three distinct regions of C ii emission from the cut, one close to the embedded source IRS1, one associated with the ionization front, and one further into the cloud. The line emission can be understood in terms of a clumpy model of PDRs. At the position of IRS1, we identify at least two distinct components contributing to the [C ii] emission, one of them a small, hot component, which can possibly be identified with the irradiated outflow walls. This is consistent with the C ii peak at IRS1 coinciding with shocked H2 emission at the edges of the outflow cavity. We note that previously available observations of IRS1 can be reproduced well by a single-component KOSMA-? model. Thus, it is HIFI's unprecedented spatial and spectral resolution, as well as its sensitivity that has allowed us to uncover an additional hot gas component in the S140 region. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Acknowledgements and appendices (pages 5 to 7) are only available in electronic form at http://www.aanda.org
The origin of the [C II] emission in the S140 PDRs - new insights from HIFI
2010-07-29
Using Herschel's HIFI instrument we have observed [C II] along a cut through S140 and high-J transitions of CO and HCO+ at two positions on the cut, corresponding to the externally irradiated ionization front and the embedded massive star forming core IRS1. The HIFI data were combined with available ground-based observations and modeled using the KOSMA-tau model for photon dominated regions. Here we derive the physical conditions in S140 and in particular the origin of [C II] emission around IRS1. We identify three distinct regions of [C II] emission from the cut, one close to the embedded source IRS1, one associated with the ionization front and one further into the cloud. The line emission can be understood in terms of a clumpy model of photon-dominated regions. At the position of IRS1, we identify at least two distinct components contributing to the [C II] emission, one of them a small, hot component, which can possibly be identified with the irradiated outflow walls. This is consistent with the fact that the [C II] peak at IRS1 coincides with shocked H2 emission at the edges of the outflow cavity. We note that previously available observations of IRS1 can be well reproduced by a single-component KOSMA-tau model. Thus it is HIFI's unprecedented spatial and spectral resolution, as well as its sensitivity which has allowed us to uncover an additional hot gas component in the S140 region.
Anisotropic Galactic Outflows and Enrichment of the Intergalactic Medium. II. Numerical Simulations
2010-03-01
We combine an analytic model for anisotropic outflows and galaxy formation with numerical simulations of large-scale structure and halo formation to study the impact of galactic outflows on the evolution of the IGM. We have simulated the evolution of a comoving volume (15 Mpc)^3 in the LCDM universe. We follow the formation of 20000-60000 galaxies and simulate the galactic outflows produced by these galaxies, for five outflow opening angles, alpha=60, 90, 120, 150, and 180 degrees (isotropic outflows). Anisotropic outflows follow the path of least resistance and thus travel preferentially into low-density regions, away from cosmological structures where galaxies form. These anisotropic outflows are less likely to overlap with one another, or to hit pre-galactic collapsing halos and strip them of their gas, preventing a galaxy from forming. Going from 180 deg to 60 deg, the number of galaxies that actually form doubles, producing twice as many outflows, and these outflows overlap to a lesser extent. As a result, the metal volume filling factor of the IGM goes from 8% for isotropic outflows up to 28% for anisotropic ones. High density regions are more efficiently enriched than low density ones (~80% compared to ~20% by volume), even though most enriched regions are low densities. Increasing the anisotropy of outflows increases the extent of enrichment at all densities, low and high. This is in part because anisotropic outflows ar e more numerous. When this effect is factored-out, we find that the probability a galaxy will enrich systems at densities up to 10 rho_mean is higher for increasingly anisotropic outflows. This is an effect of the dynamical evolution of the IGM. Anisotropic outflows expand preferentially into underdense gas, but that gas can later accrete onto overdense structures.
2010-01-01
The integrity of actin cytoskeletal organization in aqueous humor outflow pathway is thought to play a critical role in modulation of aqueous humor outflow through the trabecular meshwork. Our understanding of the regulation of actin cytoskeletal dynamics in outflow pathway, however, is very limited. To explore the potential importance of Neural Wiskott-Aldrich syndrome protein (N-WASP), a critical regulator of actin polymerization/nucleation in aqueous humor outflow pathway, the effects of Wiskostatin, a selective pharmacological inhibitor of N-WASP, on aqueous humor outflow facility were evaluated using enucleated porcine eyes and a constant pressure perfusion system. Further, drug induced effects on actin cytoskeletal organization, cell adhesions, myosin II phosphorylation, matrix metal...
c2d Spitzer IRS spectra of embedded low-mass young stars: gas-phase emission lines
2010-05-18
A survey of mid-IR gas-phase emission lines of H2, H2O and various atoms toward a sample of 43 embedded low-mass young stars in nearby star-forming regions is presented. The sources are selected from the Spitzer "Cores to Disks" (c2d) legacy program. The environment of embedded protostars is complex both in its physical structure (envelopes, outflows, jets, protostellar disks) and the physical processes (accretion, irradiation by UV and/or X-rays, excitation through slow and fast shocks) which take place. A key point is to spatially resolve the emission in the Spitzer-IRS spectra. An optimal extraction method is used to separate both spatially unresolved (compact, up to a few 100 AU) and spatially resolved (extended, 1000 AU or more) emission from the IRS spectra. The results are compared with the c2d disk sample and literature PDR and shock models to address the physical nature of the sources. Both compact and extended emission features are observed. Warm (Tex few 100 K) H2, observed through the pure rotational H2 S(0), S(1) and S(2) lines, and [S I] 25 mu emission is observed primarily in the extended component. [S I] is observed uniquely toward truly embedded sources and not toward disks. On the other hand hot (Tex>700 K) H2, observed primarily through the S(4) line, and [Ne II] emission is seen mostly in the compact component. [Fe II] and [Si II] lines are observed in both spatial components. Hot H2O emission is found in th e compact component of some sources. The observed emission on >=1000 AU scales is characteristic of PDR emission and likely originates in the outflow cavities in the remnant envelope created by the stellar wind and jets from the embedded young stars. Weak shocks along the outflow wall can also contribute. The compact emission is likely of mixed origin, comprised of optically thick circumstellar disk and/or jet/outflow emission from the protostellar object.
2006-04-07
The kinematics of neutral gas and warm ionized gas have been mapped in one-dimension across ultraluminous starburst galaxies using interstellar absorption and emission lines, in Keck II ESI spectra. Blue-shifted absorption is found along more of the slit than anticipated, exceeding scales of 15 kpc across several systems. The large velocity gradient measured across some of these outflows is inconsistent with a flow diverging from the central starburst -- angular momentum conservation reduces the rotational velocity of an outflow as it expands. More widespread star formation, likely triggered by the merger, probably drives these outflows, although some models suggest the collision itself could generate a wind by shock heating interstellar gas throughout the disk. Young mergers with separated nuclei present the highest outflow masses, due mainly to the larger area over which the cool gas can be detected. In a typical ULIG, the mass carried by the cool phase of the outflow is around 10^8Msun, or a few percent of the total dynamical mass. Assuming the starburst activity has proceeded at the observed rate for the past 10 Myr, the kinetic energy of the cool outflows is a few percent of the supernova energy, consistent with starbursts powering the outflows. The cool wind is expected to be accelerated by momentum deposition, possibly from radiation pressure as well as supernovae. Such models imply turn-around radii for the cool outflows of at least 30 to 90 kpc. This cross-section presents a significant NaI absorption cross section. If most L > 0.1L* galaxies pass through a luminous starburst phase, then relics of cool outflows will create a significant redshift-path density. Galaxy formation models should include this cool phase of the outflow in addition to a hot wind in feedback models.
2009-10-02
The [Ne II] fine-structure emission line at 12.8 micron has been detected in several young stellar objects (YSO) spectra. This line is thought to be produced by X-ray irradiation of the warm protoplanetary disk atmospheres, however the observational correlation between [Ne II] luminosities and measured X-ray luminosities shows a large scatter. Such spread limits the utility of this line as a probe of the gaseous phase of disks, as several authors have suggested pollution by outflows as a probable cause of the observed scatter. In this work we explore the possibility that the large variations in the observed [Ne II] luminosity may be caused instead by different star-disk parameters. In particular we study the effects that the hardness of the irradiating source and the structure (flaring) of the disk have on the luminosity and spectral profile of the [Ne II] 12.8 micron line. We find that varying these parameter can indeed cause up to an order of magnitude variation in the emission luminosities which may explain the scatter observed, although our models predict somewhat smaller luminosities than those recently reported by other authors who observed the line with the Spitzer Space Telescope. Our models also show that the hardness of the spectrum has only a limited (undetectable) effect on the line profiles, while changes in the flaring power of the disk significantly affect the size of the [Ne II] emission region and, as a consequ ence, its line profile. In particular we suggest that broad line profiles centred on the stellar radial velocity may be indicative of flat disks seen at large inclination angles.
Mapping the outflow of OH5. 89-0. 39
1990-09-15
A fast, massive bipolar outflow is found to be associated with 5.89-0.39, a luminous, compact H II region. Using VLA observations, we have mapped the source in the continuum, in several OH lines, in H I absorption, and in the H76{alpha} recombination line. The inner ionized region, with a radius of 0.06 pc, shows a disc-like geometry, with some evidence for rotation in the outer part of the disc. The main-line OH masers in the surrounding neutral gas trace a biconical rapid outflow, with a total velocity width of 60 km s{sup -1}, perpendicular to the disc. The OH outflow is aligned with a much more extended flow observed in CO. Evidence for outflow is also seen in H I absorption, albeit at lower velocities. We conclude that the outflowing gas originates outside the ionized region. The H{sub 2}O masers also trace an outflow, but with a velocity gradient opposite to the OH and CO. (author).
A submillimetre survey of the kinematics of the Perseus molecular cloud - II. Molecular outflows
2010-06-17
We present a census of molecular outflows across four active regions of star formation in the Perseus molecular cloud (NGC 1333, IC348/HH211, L1448 and L1455), totalling an area of over 1000 sq arcmin. This is one of the largest surveys of outflow evolution in a single molecular cloud published to date. We analyse large-scale, sensitive CO J=3-2 datasets from the James Clerk Maxwell Telescope, including new data towards NGC 1333. Where possible we make use of our complementary 13CO and C18O data to correct for the 12CO optical depth and measure ambient cloud properties. Of the 65 submillimetre cores in our fields, we detect outflows towards 45. We compare various parameters between the outflows from Class 0 and I protostars, including their mass, momentum, energy and momentum flux. Class 0 outflows are longer, faster, more massive and have more energy than Class I outflows. The dynamical time-scales we derive from these outflows are uncorrelated to the age of the outflow driving source, computed from the protostar's bolometric temperature. We confirm the results of Bontemps et al., that outflows decrease in force as they age, suggesting a decline in the mass accretion rate. If F_rad=L_bol/c is the flux expected in radiation from the central source, then F_CO(Class I)~100F_rad and F_CO(Class 0)~1000F_rad. Finally, we note that the total energy contained in outflows in NGC 1333, L1448 and L1455 is greater than the estimated turbu lent energy in the respective regions, which may have implications for the regions' evolution.
2009-09-01
We analyze the physical conditions in the low-ionization component of starburst outflows (in contrast to the high-ionization wind fluid observed in X-rays), based on new Keck/LRIS spectroscopy of partially resolved absorption troughs in near-ultraviolet and optical spectra of Ultraluminous Infrared Galaxies. The large velocity width and blueshift present in seven, atomic transitions indicate a macroscopic velocity gradient within the outflowing gas. The \\mgII 2796, 2803 (and \\feII 2587, 2600) doublet lines in these data constrains the gas kinematics better than the heavily blended \\nad 5892, 98 doublet. The identical shape of the \\mgII 2796 absorption troughs to that of the normally weaker transition at 2803\\AA requires both transitions be optically thick at all outflow velocities. The fraction of the galactic continuum covered by the outflow at each velocity therefore dictates the shape of these absorption troughs. We suggest that the velocity offset of the deepest part of the troughs, where the covering factor of low-ionization gas is near unity, reflects the speed of a shell of swept-up, interstellar gas at the time of blowout. In a spherical outflow, we show that the fragments of this shell expand slowly relative to the geometrical dilution; and the covering fraction of low-ionization gas decreases with increasing radius. Our measurement of a covering factor that decreases with increasing velocity can therefore be interpret ed as evidence that the low-ionization outflow is accelerating. We also present measurements of C_f(v) in 4 species, place an upper limit of 3000 cm3 on the density of the outflowing gas, and discuss lower limits on the mass outflow rate.
Fine-Structure Line Emission from the Outflows of Young Stellar Objects
2010-04-29
The flux and line shape of the fine-structure transitions of \\NeII\\ and \\NeIII\\ at 12.8 and 15.55\\,$\\mu$m and of the forbidden transitions of \\OI\\ $\\lambda6300$ are calculated for young stellar objects with a range of mass-loss rates and X-ray luminosities using the X-wind model of jets and the associated wide-angle winds. For moderate and high accretion rates, the calculated \\NeII\\ line luminosity is comparable to or much larger than produced in X-ray irradiated disk models. All of the line luminosities correlate well with the main parameter in the X-wind model, the mass-loss rate, and also with the assumed X-ray luminosity --- and with one another. The line shapes of an approaching jet are broad and have strong blue-shifted peaks near the effective terminal velocity of the jet. They serve as a characteristic and testable aspect of jet production of the neon fine-structure lines and the \\OI\\ forbidden transitions.
THE OUTFLOWING WIND OF V1057 CYGNI
2009-01-01
In 1970-1971, V1057 Cyg rose from about m pg approx 16 to a peak near 10.5 mag. It has subsequently faded to about B = 15, and although it appeared to be a T Tauri star (TTS) before the outburst, it now resembles a rather peculiar rapidly rotating G-type supergiant. Before the outburst, it showed unmistakable evidence of high-velocity outflow (by the suppression of emission Ca II lambda3968 by the P Cyg absorption component of Hepsilon lambda3970). Such outflow absorptions are currently found at many strong lines (Halpha, Na I D1,2, K I lambdalambda7664, 7698, Ca II lambdalambda8498, 8662, ...). The same phenomenon has since been observed in a number of other FUors near maximum light, suggesting that it is a FUor characteristic that clearly ...
HH 223: a parsec-scale H2 outflow in the star-forming region L723
2010-08-24
The dark cloud Lynds 723 (L723) is a low-mass star-forming region where one of the few known cases of a quadrupolar CO outflow has been reported. Two recent works have found that the radio continuum source VLA 2, towards the centre of the CO outflow, is actually a multiple system of young stellar objects (YSOs). Several line-emission nebulae that lie projected on the east-west CO outflow were detected in narrow-band Halpha and [SII] images. The spectra of the knots are characteristic of shock-excited gas (Herbig-Haro spectra), with supersonic blueshifted velocities, which suggests an optical outflow also powered by the VLA 2 YSO system of L723. We imaged a field of ~5' X 5' centred on HH 223, which includes the whole region of the quadrupolar CO outflow with nir narrow-band filters . The H2 line-emission structures appear distributed over a region of 5.5' (0.5 pc for a distance of 300 pc) at both sides of the VLA 2 YSO system, with an S-shape morphology, and are projected onto the east-west CO outflow. Most of them were resolved in smaller knotty substructures. The [FeII] emission only appears associated with HH 223. An additional nebular emission from the continuum in Hc and Kc appears associated with HH 223-K1, the structure closest to the VLA 2 YSO system, and could be tracing the cavity walls. We propose that the H2 structures form part of a large-scale near-infrared outflow, which is also associated with the VLA 2 YSO syst em. The current data do not allow us to discern which of the YSOs of VLA 2 is powering this large scale optical/near-infrared outflow.
2010-03-04
(Abridged) Star formation-driven outflows are a critically important phenomenon in theoretical treatments of galaxy evolution, despite our limited ability to trace them across cosmological timescales. It has been suggested that the strongest QAL systems might arise in such outflows. If confirmed, "Ultra-strong" MgII (USMgII) absorbers may identify galactic winds over a huge baseline in cosmic time, independently of the luminous properties of the galaxy. To this end, we present the first detailed imaging/spectroscopic study of the fields of two USMgII absorber systems culled from a statistical absorber catalog, to investigate the physical processes leading to the large velocity spreads that define such systems. Each field contains two bright emission-line galaxies at similar redshift to that of the absorption. Their specific SFRs are among the highest for their masses at these redshifts, and their 4000A break and Balmer absorption strengths imply they have undergone recent (~ 0.01-1 Gyr) starbursts. The concomitant presence of two rare phenomena - starbursts and USMgII absorbers - strongly implies a causal connection. We consider these data and USMgII absorbers in general in the context of various models, and conclude that galactic outflows are generally necessary to account for the velocity-extent of the absorption, favouring starburst driven outflows over tidally-stripped gas from a major interaction which triggered the starbu rst. Unlike past discoveries of blueshifted gas in the spectra of galaxies at cosmological distances, identifying outflows in this manner unambiguously demonstrates that the material reaches the IGM. Finally, we discuss the implications of these results and speculate on the overall contribution of such systems to the global SFR density at z ~ 0.7.
2009-01-01
We analyze the physical conditions in the low-ionization component of starburst outflows (in contrast to the high-ionization wind fluid observed in X-rays), based on new Keck/LRIS spectroscopy of partially resolved absorption troughs in near-ultraviolet and optical spectra of Ultraluminous Infrared Galaxies. The large velocity width and blueshift present in seven atomic transitions indicate a macroscopic velocity gradient within the outflowing gas. The separation of the Mg II 2796, 2803 (and Fe II 2587, 2600) doublet lines in these data constrains the gas kinematics better than previous studies of the heavily blended Na I 5892, 5898 doublet. The identical shape of the Mg II 2796 absorption troughs to that of the normally weaker transition at 2803 A (after accounting for emission filling) requires both transitions be optically thick at all outflow velocities. The ...
Keck Hires Observations of the QSO First J104459.6+365605$$bEvidence for a Large Scale Outflow
This paper presents an analysis of a Keck HIRES spectrum of the QSO FIRST J104459.6+365605. The line of sight towards the QSO contains two clusters of outflowing clouds that give rise to broad blue shifted absorption lines. The outflow velocities of the clouds range from -200 to -1200 km/s and from -3400 to -5200 km/s, respectively. The width of the individual absorption lines ranges from 50 to more than 1000 km/s. The most prominent absorption lines are those of Mg II, Mg I, and Fe II. The low ionization absorption lines occur at the same velocities as the most saturated Mg II lines, showing that the Fe II, Mg I and Mg II line forming regions must be closely associated. Many absorption lines from excited states of Fe II are present, allowing a determination of the population of several low lying energy levels. From this we determine an electron density in the Fe II line forming regions of 4000 per cubic cm. Modelling the ionization state of the absorbing gas with this value of the electron density as a constraint, we find that the distance between the Fe II and Mg I line forming region and the continuum source is of order 700 parsec. From the correspondence in velocity between the Fe II, Mg I and Mg II lines we infer that the Mg II lines must be formed at the same distance. The Mg II absorption fulfills the criteria for Broad Absorption Lines defined by Weymann et al. (1991). This large distance is surprising, since BALs are generally thought to be formed in outflows at a much smaller distance from the nucleus.
Homologous type II radio bursts and coronal transients
1984-05-01
The homology of seven successive type II solar radio bursts, which occurred at the times of flares from an active region near the solar west limb on 1980, July 27-29, is described, together with evidence for coronal mass outflows accompanying these bursts. It is argued that homologous type II bursts imply that the corona is restructured in a similar manner by successive coronal transients.
Quantitative CW Nd:YAG pars plana transscleral photocoagulation in postmortem eyes
1990-12-01
The effect of different types of burns and numbers of lesions on, and the role of initial pressure head in, the rate of aqueous outflow was studied in enucleated human and porcine eyes. Noncontact and contact CW Nd:YAG laser applied to human eyes 3 mm posterior to the limbus produced a 34% and 51% increase, respectively, in outflow as compared with controls (P = .01). In porcine eyes, outflow increased directly with the number of noncontact burns as well as with the amount of perfusion pressure. Our results suggest that intraocular pressure and outflow are functions of both the intensity of irradiation and the surface area treated, and that each individual pressure head may require an optimal pars plana area of treatment of therapeutic degree to lower pressure and yet prevent overfiltration and phthisis. Our results also suggest that there may be a passive transneuroepithelial and transscleral outflow component in clinical laser cycloablation and, therefore, a need to grade laser treatments in order to prevent visual loss through unnecessary injury.
Quasar Outflow Contribution to AGN Feedback: Observations of QSO SDSS J0838+2955
2009-11-18
We present a detailed analysis of the Astrophysical Research Consortium 3.5 m telescope spectrum of QSO SDSS J0838+2955. The object shows three broad absorption line (BAL) systems at 22,000, 13,000, and 4900 km s^-1 blueshifted from the systemic redshift of z=2.043. Of particular interest is the lowest velocity system that displays absorption from low-ionization species such as Mg II, Al II, Si II, Si II*, Fe II and Fe II*. Accurate column densities were measured for all transitions in this lowest velocity BAL using an inhomogeneous absorber model. The ratio of column densities of Si II* and Fe II* with respect to their ground states gave an electron number density of log n_e (cm^-3) = 3.75 +/- 0.22 for the outflow. Photoionization modeling with careful regards to chemical abundances and the incident spectral energy distribution predicts an ionization parameter of log U_H = -1.93 +/- 0.21 and a hydrogen column density of log N_H (cm^-2) = 20.80 +/- 0.28. This places the outflow at 3.3+1.5-1.0 kpc from the central AGN. Assuming that the fraction of solid angle subtended by the outflow is 0.2, these values yield a kinetic luminosity of (4.5+3.1-1.8) x 10^45 erg s^-1, which is (1.4+1.1-0.6)% the bolometric luminosity of the QSO itself. Such large kinetic luminosity suggests that QSO outflows are a major contributor to AGN feedback mechanisms.
2010-04-09
We present a calculation of the atomic and low-ionisation emission line spectra of photoevaporating protoplanetary discs. Line luminosities and profiles are obtained from detailed photoionisation calculations of the disc and wind structures surrounding young active solar-type stars. The disc and wind density and velocity fields were obtained from the recently developed radiation-hydrodynamic models of Owen et al., that include stellar X-ray and EUV irradiation of protoplanetary discs at various stages of clearing, from primordial sources to inner hole sources of various hole sizes. Our models compare favourably with currently available observations, lending support to an X-ray driven photoevaporation model for disc dispersal. In particular, we find that X-rays drive a warm, predominantly neutral flow where the OI 6300A line can be produced by neutral hydrogen collisional excitation. Our models can, for the first time, provide a very good match to both luminosities and profiles of the low-velocity component of the OI 6300A line and other forbidden lines observed by Hartigan et al., which covered a large sample of T-Tauri stars. We find that the OI 6300A and the NeII 12.8um lines are predominantly produced in the X-ray-driven wind and thus appear blue-shifted by a few km/s for some of the systems when observed at non-edge-on inclinations. We note however that blue-shifts are only produced under certain conditions: X-ray luminosit y, spectral shape and inner hole size all affect the location of the emitting region and the physical conditions in the wind. We caution therefore that while a blueshifted line is a tell-tale sign of an outflow, the lack of a blueshift should not be necessarily interpreted as a lack of outflow.
SPITZER SPECTRAL LINE MAPPING OF PROTOSTELLAR OUTFLOWS. I. BASIC DATA AND OUTFLOW ENERGETICS
2009-01-01
We report the results of spectroscopic mapping observations carried out toward protostellar outflows in the BHR71, L1157, L1448, NGC 2071, and VLA 1623 molecular regions using the Infrared Spectrograph (IRS) of the Spitzer Space Telescope. These observations, covering the 5.2-37 mum spectral region, provide detailed maps of the eight lowest pure rotational lines of molecular hydrogen and of the [S I] 25.25 mum and [Fe II] 26.0 mum fine-structure lines. The molecular hydrogen lines, believed to account for a large fraction of the radiative cooling from warm molecular gas that has been heated by a non-dissociative shock, allow the energetics of the outflows to be elucidated. Within the regions mapped toward these five outflow sources, total H2 luminosities ranging from 0.02 to 0.75 Lsun were inferred for the sum of ...
Narrow associated QSO absorbers: clustering, outflows and the line-of-sight proximity effect
2008-02-29
Using data from the Sloan Digital Sky Survey data release 3 (SDSS DR3) we investigate how narrow (40% of CIV absorbers within 3,000km/s of the QSO are not a result of large-scale clustering but rather are directly associated with the quasar itself; (iii) that this intrinsic absorber population extends to outflow velocities of order 12,000km/s; (iv) that this outflow component is present in both radio-loud and radio-quiet quasars; and (v) that a small high-velocity outflow component is observed in the MgII population, but any further intrinsic absorber component is undetectable in our clustering analysis. We also find an indication that absorption systems within 3,000km/s are more abundant for radio-loud than for radio-quiet quasars. This suggests either that radio-loud objects live in more massive halos, or that their radio activity generates an additional low-velocity outflow, or both.
Low-ionization Line Emission from Starburst Galaxies: A New Probe of Galactic-Scale Outflows
2010-08-23
We study the kinematically narrow, low-ionization line emission from a bright, starburst galaxy at z = 0.69 using slit spectroscopy obtained with Keck/LRIS. The spectrum reveals strong absorption in MgII and FeII resonance transitions with Doppler shifts of -200 to -300 km/s, indicating a cool gas outflow. Emission in MgII near and redward of systemic velocity, in concert with the observed absorption, yields a P Cygni-like line profile similar to those observed in the Ly alpha transition in Lyman Break Galaxies. Further, the MgII emission is spatially resolved, and extends significantly beyond the emission from stars and HII regions within the galaxy. Assuming the emission has a simple, symmetric surface brightness profile, we find that the gas extends to distances > ~7 kpc. We also detect several narrow FeII* fine-structure lines in emission near the systemic velocity, arising from energy levels which are radiatively excited directly from the ground state. We suggest that the MgII and FeII* emission is generated by photon scattering in the observed outflow, and emphasize that this emission is a generic prediction of outflows. These observations provide the first direct constraints on the minimum spatial extent and morphology of the wind from a distant galaxy. Estimates of these parameters are crucial for understanding the impact of outflows in driving galaxy evolution.
The near-infrared excitation of the HH211 protostellar outflow
2005-02-04
The protostellar outflow HH211 is of considerable interest since it is extremely young and highly collimated. Here, we explore the outflow through imaging and spectroscopy in the near-infrared to determine if there are further diagnostic signatures of youth. We confirm the detection of a near-infrared continuum of unknown origin. We propose that it is emitted by the driving millimeter source, escapes the core through tunnels, and illuminates features aligning the outflow. Narrow-band flux measurements of these features contain an unusually large amount of continuum emission. [Fe II] emission has been detected and is restricted to isolated condensations. However, the characteristics of vibrational excitation of molecular hydrogen resemble those of older molecular outflows. We attempt to model the ordered structure of the western outflow as a series of shocks, finding that bow shocks with J-type dissociative apices and C-type flanks are consistent. Moreover, essentially the same conditions are predicted for all three bows except for a systematic reduction in speed and density with distance from the driving source. We find increased K-band extinctions in the bright regions as high as 2.9 magnitudes and suggest that the bow shocks become visible where the outflow impacts on dense clumps of cloud material. We propose that the outflow is carved out by episodes of pulsating jets. The jets, driven by central explosive events, are responsible for excavating a central tunnel through which radiation temporarily penetrates.
The impact of the warm outflow in the young (GPS) radio source & ULIRG PKS 1345+12 (4C 12.50)
2010-08-18
(Abridged) We present new deep VLT/FORS optical spectra with intermediate resolution and large wavelength coverage of the GPS radio source and ULIRG PKS1345+12 (4C12.50; z=0.122), taken with the aim of investigating the impact of the nuclear activity on the circumnuclear ISM. PKS1345+12 is a powerful quasar and is also the best studied case of an emission line outflow in a ULIRG. Using the density sensitive transauroral emission lines [S II]4068,4076 and [O II]7318,7319,7330,7331, we pilot a new technique to accurately model the electron density for cases in which it is not possible to use the traditional diagnostic [S II]6716/6731, namely sources with highly broadened complex emission line profiles and/or high (Ne > 10^4 cm^-3) electron densities. We measure electron densities of Ne=2.94x10^3 cm^-3, Ne=1.47x10^4 cm^-3 and Ne=3.16x10^5 cm^-3 for the regions emitting the narrow, broad and very broad components respectively. We calculate a total mass outflow rate of 8 M_sun yr^-1. We estimate the total mass in the warm gas outflow is 8x10^5 M_sun. The total kinetic power in the warm outflow is 3.4x10^42 erg s^-1. We find that only a small fraction (0.13% of Lbol) of the available accretion power is driving the warm outflow, significantly less than currently required by the majority of quasar feedback models (~5-10\\% of Lbol), but similar to recent findings by Hopkins et al. (2010) for a two-stage feedback model. The models also p redict that AGN outflows will eventually remove the gas from the bulge of the host galaxy. The visible warm outflow in PKS1345+12 is not currently capable of doing so. However, it is entirely possible that much of the outflow is either obscured by a dense and dusty natal cocoon and/or in cooler or hotter phases of the ISM. This result is important not just for studies of young (GPS/CSS) radio sources, but for AGN in general.
Kinematics of Interstellar Gas in Nearby UV-Selected Galaxies Measured with HST/STIS Spectroscopy
2006-05-09
We measure Doppler shifts of interstellar absorption lines in HST/STIS spectra of individual star clusters in nearby UV-selected galaxies. Values for systemic velocities, which are needed to quantify outflow speeds, are taken from the literature, and verified with stellar lines. We detect outflowing gas in eight of 17 galaxies via low-ionization lines (e.g., CII, SiII, AlII), which trace cold and/or warm gas. The starbursts in our sample are intermediate in luminosity (and mass) to dwarf galaxies and luminous infrared galaxies (LIRGs), and we confirm that their outflow speeds (ranging from -100 km/s to nearly -520 km/s with an accuracy of ~80 km/s) are intermediate to those previously measured in dwarf starbursts and LIRGs. We do not detect the outflow in high-ionization lines (such as CIV or SiIV); higher quality data will be needed to empirically establish how velocities vary with the ionization state of the outflow. We do verify that the low-ionization UV lines and optical NaI doublet give roughly consistent outflow velocities solidifying an important link between studies of galactic winds at low and high redshift. To obtain higher signal-to-noise, we create a local average composite spectrum, and compare it to the high-z Lyman Break composite spectrum. Surprisingly, the low-ionization lines show similar outflow velocities in the two samples. We attribute this to a combination of weighting towards higher luminosities in the local composite, as well as both samples being on average brighter than the ``turnover'' luminosity in the v-SFR relation.
2004-02-10
Observations of the PSR B1259-63/SS2883 binary system using the CANGAROO-II Cherenkov telescope are reported. This nearby binary consists of a 48msec radio pulsar in a highly eccentric orbit around a Be star, and offers a unique laboratory to investigate the interactions between the outflows of the pulsar and Be star at various distances. It has been pointed out that the relativistic pulsar wind and the dense mass outflow of the Be star may result in the emission of gamma rays up to TeV energies. We have observed the binary in 2000 and 2001, 47 and 157 days after the October 2000 periastron. Upper limits at the 0.13--0.54 Crab level are obtained. A new model calculation for high-energy gamma-ray emission from the Be star outflow is introduced and the estimated gamma-ray flux considering Bremsstrahlung, inverse Compton scattering, and the decay of neutral pions produced in proton-proton interactions, is found to be comparable to the upper limits of these observations. Comparing our results with these model calculations, the mass-outflow parameters of the Be star are constrained.
2004-01-01
A study of morphology, kinematics and ionization structure of the IR merger NGC 5514, is presented. This study is based mainly on Integral 2D spectroscopy obtained on 4.2 m William Herschel Telescope (La Palma, Spain) and data from CASLEO (Argentina). Clear evidence of two extra-nuclear starbursts with young outflows and LINER activity are reported. One of these outflow generate a supergiant bubble, where the emission lines and kinematics maps show 4 extended ejections. These results suggest that the bubble is in the rupture phase.
Radio signatures of upper and lower reconnection outflow shocks
2004-01-01
For the flare of 28 September 2001, we discuss simultaneously appearing slow drift (type II-like) bursts at about 327 and 58 MHz as radio signature of the upper and lower reconnection outflow termination shock (TS). The features appear during the impulsive phase, but well after the regular traveling-shock type II burst, and during the rise of a CME. The sequence of the regular type II and the following standing shock signatures are well in accordance with the energy release diagnostic from the time derivative of the GOES flux. The upper and lower TS features are suggestive of a flux anti-correlation tendency. We use radio imaging data (Nancay radio heliograph), SOHO EIT and Yohkoh SXT images to support the TS hypothesis. The result gives new observational support for assuming magnetic reconnection as flare energy release mechanism. (orig.)
QUASAR OUTFLOW CONTRIBUTION TO AGN FEEDBACK: OBSERVATIONS OF QSO SDSS J0838+2955
2009-01-01
We present a detailed analysis of the Astrophysical Research Consortium 3.5 m telescope spectrum of QSO SDSS J0838+2955. The object shows three broad absorption line (BAL) systems at 22,000, 13,000, and 4900 km s-1 blueshifted from the systemic redshift of z = 2.043. Of particular interest is the lowest velocity system that displays absorption from low-ionization species such as Mg II, Al II, Si II, Si II*, Fe II, and Fe II*. Accurate column densities were measured for all transitions in this lowest velocity BAL using an inhomogeneous absorber model. The ratio of column densities of Si II* and Fe II* with respect to their ground states gave an electron number density of log ne (cm-3) = 3.75 +- 0.22 for the outflow. Photoionization modeling with careful regards to chemical abundances and the incident spectral energy distribution ...
1999-01-01
Experimental single event upset characterization of the Pentiumregsign MMX and PentiumregsignII microprocessors using proton irradiation are presented. Results show the Pentium II processor core cross-section is ten times that of the MMX
High Velocity Outflows in Quasars
2007-01-29
High velocity (HV) outflows are an important but poorly understood aspect of quasar/SMBH evolution. Outflows during the luminous accretion phase might play a critical role in "unveiling" young dusty AGN and regulating star formation in the host galaxies. Most quasar studies have focussed on the broad absorption lines (BALs). We are involved in a program to study a nearly unexplored realm of quasar outflow parameter space: HV winds with v>10,000 km/s up to v~0.2c but small velocity dispersions (narrow absorption lines), such that (Delta v)/v << 1. Narrow-line HV flows merit specific attention because they complement the BAL work and pose unique challenges for models of the wind acceleration, mass loss rates, launch radii, geometry, etc. We have selected the brightest quasars at 1.8<z<3.5 with candidate narrow HV outflow lines (CIV 1548 A) in existing SDSS spectra and followed up with monitoring observations to i) characterize, for the first time, the variability in a sample of absorbers spanning a wide range of velocities and FWHMs, including some marginal BALs, ii) identify/confirm more of the true outflow systems, e.g., among the more ambiguous narrow lines, and iii) test the wind models and derive better constraints on basic outflow properties, such as the kinematics, locations, and physical conditions.
Molecular and atomic emission-line images of DR 21 and GGD 37
Molecular and atomic emission-line images of DR 21 and GGD 37 PI: J.R. Houck Technical contact: Dan Watson DR 21 and GGD 37 (Cep A West) are two of the best-resolved examples of bipolar outflows and shocks from massive young stellar objects. In this program we will use the high-spectral-resolution modules of the IRS to obtained detailed images of emission by molecular hydrogen (three pure rotational lines), water (13 pure rotational lines) , and several low-excitation ions and atoms (e.g. [Si II], [Fe II], [S I] and [Ne II]). The structure of the shocks will be resolved in the images; in particular the dual cloud-shock/jet-shock structures will be cleanly separated in the many nearly-edge-on shock rims in these objects. This provides a unique opportunity -- not possible from suborbital platformas -- for study of the interaction of a YSO outflow and its surrounding cloud, using probes that trace the bulk of the material (H2) as well as the bulk of the radiated energy (H2O) in the shocked gas, and will provide strong constraints on models of the interaction and on the influence of outflows and shocks on ongoing star formation.
1986-02-25
An apparatus for burning combustible solid organic material such as wood is described in a environment in which combustion is directed downwardly. The apparatus consists of: A. A fuel chamber having a closed upper portion and a major dimension in the vertical direction such that the fuel chamber is generally upright, B. A combustion zone in the lower portion of the fuel chamber defined by a convergent outflow passage at the bottom of the fuel chamber and a pair of walls on opposite sides of the lower portion, the walls being sloped inwardly toward one another at the outflow passage, and the outflow passage comprising a gap between the walls, C. A Hearth element forming each the sloping wall, the hearth element including I. At least one row of spaced slots extending into the interior of the hearth element and a lateral air inlet channel connected to the slots of each row and a source of combustion air, and II. A flue outlet communicating with the outflow passage, the flue outlet including spaced, parallel tubes in the hearth element, with the tubes being juxtaposed the slots and extending perpendicular to the air inlet channels, D. Means connected to the flue outlet to permit exhaustion of flue gases from the apparatus, and E. means for loading fuel into the fuel chamber.
Spiral waves and the secondary star in the nova-like variable V3885 Sgr
2005-01-01
We present seven nights' blue (4300–5000 Å) spectroscopy of the nova-like variable star V3885 Sgr. The line spectrum shows a typical combination of broad absorption and emission in Hγ, Hβ and He I, which is associated with the accretion disc. We also observe antiphased narrow emission, which we attribute to irradiation of the secondary star. The He IIλ4686 and N III–C III–C IV emission lines are devoid of structure and are most likely formed in an outflow. We measure radial velocity shifts in the absorption and emission lines, from which we fit an orbital period of 4.971 26 ± 0.000 36 h. From the velocity semi-amplitudes of the disc and companion star, we are able to constrain the binary mass ratio to q> 0.7. The phase-folded spectra provide dense coverage of the entire orbital cycle. Doppler tomograms of the hydrogen and He I lines reveal spiral structure in the accretion disc and the irradiated donor star. We believe that this is the first unambiguous detection of spiral waves in a nova-like variable. Publisher: Blackwell Publishers Contributor: Swinburne University of Technology. Faculty of Information and Communication Technologies. Centre for Astrophysics and Supercomputing. Relation: Monthly notices of the Royal Astronomical Society Format: pp. 251-258 Other identifier: swin:1460 Language: English Source: Monthly notices of the Royal Astronomical Society, Vol. 363, no. 1 (2005), pp. 251-258 Rights: 2005 RAS.
2005-10-03
We have conducted phase-reference multi-epoch observations of the 22.2 GHz water masers using the VLBA and multi-frequency study of the continuum emission using the VLA towards the high-mass SFR AFGL 5142. The water maser emission comes from two elongated structures (indicated as Group I and Group II), with the measured proper motions aligned along the structures' elongation axes. Each group consists of two (blue- and red-shifted) clusters of features separated by a few hundreds and thousands of AU respectively for Group I and Group II. The maser features of Group II have both positions and velocities aligned along a direction close to the axis of the outflow traced by HCO+ and SiO emission on angular scales of tens of arcsec. We predict that the maser emission arises from dense, shocked molecular clumps displaced along the axis of the molecular outflow. The two maser clusters of Group I are oriented on the sky along a direction forming a large angle (> 60 degrees) with the axis of the jet/outflow traced by Group II maser features. We have detected a compact (8.4 and 22 GHz) continuum source that falls close to the centroid of Group I masers, indicating that the source ionizing the gas is also responsible for the excitation of the water masers. The kinematic analysis indicates that the Group I masers trace outflowing rather than rotating gas, discarding the Keplerian disk scenario proposed in a previous paper for Group I. Since the axis joining the two maser clusters of Group II does not cross the position of the continuum source, Group II masers might be excited by an (undetected) massive YSO, distinct from the one (pinpointed by the VLA continuum emission) responsible for the excitation of the Group I masers.
The SINFONI MgII Program for Line Emitters (SIMPLE): Discovering starburts near QSO sight-lines
2007-09-28
Low-ionization transitions such as the MgII 2796/2803 doublet trace cold gas in the vicinity of galaxies. It is not clear whether this gas is part of the interstellar medium of large proto-disks, part of dwarfs, or part of entrained material in supernovae-driven outflows. Studies based on MgII statistics, e.g. stacked images and clustering analysis, have invoked starburst-driven outflows where MgII absorbers are tracing the denser and colder gas of the outflow. A consequence of the outflow scenario is that the strongest absorbers ought to be associated with starbursts. We use the near-IR integral field spectrograph SINFONI to test whether starbursts are found around z~1 MgII absorbers. For 67% (14 out of 21) of the absorbers with rest-frame equivalent width larger than 2 AA, we do detect Ha in emission within 200 km/s of the predicted wavelength based on the \\MgII redshift. The star-formation rate (SFR) inferred from Halpha ranges from 1 to 20 Msun/yr, i.e. showing a level of star-formation larger than in M82 by a factor of >4 on average. Our flux limit (3-sigma) corresponds to a SFR of 0.5 Msun/yr. We find evidence (at >95% confidence) for a correlation between SFR and equivalent width, indicating a physical connection between starburst phenomena and gas seen in absorption. In the cases where we can extract the velocity field, the host-galaxies reside in halos with mean mass =11.2 in good agreement with clustering mea surments.
Integral field spectroscopy of type-II QSOs at z=0.3-0.4
2010-06-21
We present and analyse integral-field observations of six type-II QSOs with z=0.3-0.4, selected from the Sloan Digital Sky Survey (SDSS). Two of our sample are found to be surrounded by a nebula of warm ionized gas, with the largest nebula extending across 8" (40 kpc). Some regions of the extended nebulae show kinematics that are consistent with gravitational motion, while other regions show relatively perturbed kinematics: velocity shifts and line widths too large to be readily explained by gravitational motion. We propose that a ~20 kpc x20 kpc outflow is present in one of the galaxies. Possible mechanisms for triggering the outflow are discussed. In this object, we also find evidence for ionization both by shocks and the radiation field of the AGN.
Optical Spectroscopy of GRO J1655-40
1999-11-17
We have obtained optical spectra of the soft X-ray transient GRO J1655-40 during different X-ray spectral states (quiescence, high-soft and hard outburst) between 1994 Aug and 1997 Jun. Characteristic features observed during the 1996-97 high-soft state were: a) broad absorption lines at Halpha and Hbeta, probably formed in the inner disk; b) double-peaked HeII 4686 emission lines, formed in a temperature-inversion layer on the disk surface, created by the soft X-ray irradiation; c) double-peaked Halpha emission, with a strength associated with the hard X-ray flux, suggesting that it was probably emitted from deeper layers than He II 4686. The observed rotational velocities of all the double-peaked lines suggest that the disk was extended slightly beyond its tidal radius. Three classes of lines were identified in the spectra taken in 1994 Aug-Sep, during a period of low X-ray activity between two strong X-ray flares: broad absorption, broad (flat-topped) emission and narrow emission. We have found that the narrow emission lines (single-peaked or double-peaked) cannot be explained by a thin-disk model. We propose that the system was in a transient state, in which the accretion disk might have had an extended optically thin cocoon and significant matter outflow. After the onset of a hard X-ray flare the disk signatures disappeared, and strong single-peaked Halpha and Paschen emission was detected, suggesting that the cocoon became opaque to optical radiation. High-ionisation lines disappeared or weakened. Two weeks after the end of the flare, the cocoon appeared to be once again optically thin.
1999-11-03
We find in a detailed morphological study (at 15 pc resolution) that the extended massive star formation process, shows: (i) extended triple asymmetrical spiral arms structure (r = 5 kpc); and (ii) the spiral arms emanate from three different nuclei. The main optical nucleus shows a small spiral-disk (r = 500 pc) which is a continuation of the external one and reach the very nucleus. And this very nucleus shows blue elongate structure (63 pc x 30 pc), and luminous blue star cluster properties. We study the kinematics of this system and present a detailed Halpha velocity field for the central region (r = 5 kpc). In the main optical nucleus we found a clear "outflow component" associated to galactic-winds and a "inflow radial motion" (in the spiral-disk nuclear structure, r = 700 pc). In addition we detected the outflow component in the central and external regions (r < 5-6 kpc), with a very wide opening angle of 140. We found that the mean value of the inflow region (at PA = 80) is practically perpendicular to the axis of the bipolar outflow (at PA = 160). We analyze in detail the physical conditions in the giant H II regions located in the asymmetric spiral arms, the two main optical nuclei, and the outflow component. In the central region (r = 5-6 kpc) we detected that the nuclear starburst and the extended giant H II regions have very similar properties. We suggest that the interaction between dynamical effects, the galactic--wind (outflow), low-energy cosmic rays, and the molecular+ionized gas (probably in the inflow phase) could be the possible mechanism that generate the "similar extended properties in the massive star formation, at scale of 5-6 kpc!". We analyze for NGC3256 the possible evolution from luminous IR galaxy to QSOs.
2010-07-21
The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel Space Observatory allows the first observations of light diatomic molecules at high spectral resolution and in multiple transitions. Here, we report deep integrations using HIFI in different lines of hydrides towards the high-mass star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+ and SH+ have not been detected. All molecules except for CH and CH+ are seen in absorption with low excitation temperatures and at velocities different from the systemic velocity of the protostellar envelope. Surprisingly, the CH(JF,P = 3/2_2,- - 1/2_1,+) and CH+(J = 1 - 0, J = 2 - 1) lines are detected in emission at the systemic velocity. We can assign the absorption features to a foreground cloud and an outflow lobe, while the CH and CH+ emission stems from the envelope. The observed abundance and excitation of CH and CH+ can be explained in the scenario of FUV irradiated outflow walls, where a cavity etched out by the outflow allows protostellar FUV photons to irradiate and heat the envelope at larger distances driving the chemical reactions that produce these molecules.
2009-05-20
(Abridged) We present two-dimensional hydrodynamical simulations of slowly rotating gas that is under the influence of the gravity of a super massive black hole and is irradiated by a thin UV accretion disc and a spherical X-ray corona. We calculate the accretion luminosity of a system based on the accretion-rate which is assumed to be equal to the mass-supply rate at the radius of ~10^-2 pc. For the models with high temperature gas at large radii (~10 pc) and high luminosities, we find a strong correlation between the mass-outflow rate (Mdot_out) and the luminosity (L). The power law index (q) describing the Mdot_out-L relation is q=2.0(+/-0.1), which is very similar to that for radiation-driven stellar and disc wind models. More surprisingly, for high density at large radii, we find steady state solutions with the accretion luminosity exceeding the Eddington limit. The super-Eddington accretion proceeds in the equatorial region and is possible because the radiation flux from the disc is significantly reduced in the equatorial direction due to the geometrical foreshortening effect. In all models, an outflow is driven from an inflow with sub-Keplerian rotation. For high temperature at large radii, the inflow occurs over a wide range of the polar angles, and the outflow occurs in a relatively narrow polar cone. However, for the super-Eddington cases with low temperature at large radii, the inflow persists only very close to the equatorial plane, resembling a thin accretion disc, while the outflow arises in a wide range of radii and polar angles. The geometry of this extreme inflow-outflow solution is very similar to a radiation-driven wind from a luminous Keplerian accretion disc.
Imaging chemical differentiation around the low-mass protostar L483-mm
2004-01-01
This paper presents a millimeter wavelength aperture-synthesis study of the spatial variations of the chemistry in the envelope around the deeply embedded low-mass protostar L483-mm on 1000 AU (5") scales. Lines of 8 molecular species including CN, C18O, CS, C34S, HCN, H13CN, HCO+ and N2H+ have been observed using the Owens Valley Radio Observatory Millimeter Array. Continuum emission at 2.7-3.4 millimeter is well-fit by a pure envelope model down to the sensitivity of the interferometer without introducing a disk/compact source, in contrast to what is seen for other protostars. A velocity gradient in the densest material is traced by HCN, CS and N2H+, and is perpendicular to the large-scale CO outflow, with a pattern consistent with rotation around a 1 solar mass central object. Velocity gradients in the propagation direction of the outflow suggest a clear interaction between the outflowing material and "quiescent" core. The C18O observations are fit with a "drop" abundance profile where CO is frozen-out in a region of the envelope with temperatures lower than 40 K and densities higher than 1.5e5 cm^{-3}, which is also required to reproduce single-dish observations. The N2H+ emission strongly resembles that of NH3 and is found to be absent toward the central continuum source. This is a direct consequence of the high CO abundances in the inner region as illustrated by a chemical model for the L483 envelope. The observed CN emission forms a spatial borderline between the outflowing and quiescent material probed by, respectively, HCO+ and N2H+, and also shows intermediate velocities compared to these two species. A scenario is suggested in which CN is enhanced in the walls of an outflow cavity due to the impact of UV irradiation either from the central protostellar system or related to shocks caused by the outflow.
The Persistence of Cool Galactic Winds in High Stellar Mass Galaxies Between z~1.4 and ~1
2009-12-15
We present an analysis of the MgII 2796, 2803 and FeII 2586, 2600 absorption line profiles in coadded spectra of 468 galaxies at 0.7 10^19.3 cm^-2, and extend to velocities of ~500 km/s. While galaxies with SFR > 10 Msun/yr host strong outflows in both this and the W09 sample, we do not detect outflows in lower-SFR (i.e., log M_*/Msun 10.5 as they age between z=1.4 and z~1, presumably because of their high absolute SFRs. Finally, using high resolution HST/ACS imaging in tandem with our spectral analysis, we find evidence for a weak trend (at 1 sigma significance) of increasing outflow absorption strength with increasing galaxy SFR surface density.
Molecular Clouds: Observation to Experiment
2004-05-06
Our ongoing investigation of how 'Pillars' and other structure form in molecular clouds irradiated by ultraviolet (UV) stars has revealed that the Rayleigh-Taylor instability is strongly suppressed by recombination in the photoevaporated outflow, that clumps and filaments may be key, that the evolution of structure is well-modeled by compressible hydrodynamics, and that directionality of the UV radiation may have significant effects. We discuss a generic, flexible set of laboratory experiments that can address these issues.
Physical Conditions in Quasar Outflows: VLT Observations of QSO 2359-1241
2008-07-03
We analyze the physical conditions of the outflow seen in QSO 2359-1241 (NVSS J235953-124148), based on high resolution spectroscopic VLT observations. This object was previously studied using Keck/HIRES data. The main improvement over the HIRES results is our ability to accurately determine the number density of the outflow. For the major absorption component, level population from five different Fe II excited level yields n_H=10^4.4 cm^-3 with less than 20% scatter. We find that the Fe ii absorption arises from a region with roughly constant conditions and temperature greater than 9000 K, before the ionization front where temperature and electron density drop. Further, we model the observed spectra and investigate the effects of varying gas metalicities and the spectral energy distribution of the incident ionizing radiation field. The accurately measured column densities allow us to determine the ionization parameter log(U) = -2.4 and total column density of the outflow (log(N_H) = 20.6 cm^-2). Combined with the number density finding, these are stepping stones towards determining the mass flux and kinetic luminosity of the outflow, and therefore its importance to AGN feedback processes.
The RTNS-II 14-MeV neutron source facility at Lawrence Livermore National Laboratory is described. Average neutron source parameters are outlined. A brief general description of the irradiation program to the present time is given. A short discussion of guidelines for prospective users is also given.
The RTNS-II 14-MeV neutron source facility at Lawrence Livermore National Laboratory is described. Average neutron source parameters are outlined. A brief general description of the irradiation program to the present time is given. A short discussion of guidelines for prospective users is also given.
1982-01-01
The RTNS-II 14-MeV neutron source facility at Lawrence Livermore National Laboratory is described. Average neutron source parameters are outlined. A brief general description of the irradiation program to the present time is given. A short discussion of guidelines for prospective users is also given.
1982-01-01
The RTNS-II 14-MeV neutron source facility at Lawrence Livermore National Laboratory is described. Average neutron source parameters are outlined. A brief general description of the irradiation program to the present time is given. A short discussion of guidelines for prospective users is also given
The goal of part II of this study was to evaluate the effects of gamma-radiation on circulating blood cells, functional characteristics of splenocytes, and cytokine expression after whole-body irradiation at varying ...
C:\\Documents and Settings\\jho...uqw.default\\Cache\\C4CF45D3d01
and a high-velocity CO outflow, which is aligned with the optical jet structure. ...... seen in H2 (2.12 m) and [Fe ii] (1.65 m) emission toward the ..... toward low-mass YSOs. There have been surveys for OH maser ...
OWR/RTNS-II low exposure spectral effects experiment
1983-01-01
Miniature flat tensile specimens of Fe, Cu, 316 stainless steel and A302B pressure vessel steel are to be irradiated to a range of fluences in RTNS-II and the Omega West Reactor at 90/sup 0/C and 290/sup 0/C. The first RTNS-II irradiation is now in progress, and preparations are being made for the first Omega West Reactor irradiation. Some specimens are also being irradiated at room temperature in RTNS-II. The flat tensile specimens lend themselves to a variety of measurements, many of which, including the tensile tests, can be done on the same specimen.
1990-01-01
We studied the effect of topical dexamethasone (1%) and preoperative beta irradiation on a model of glaucoma fistulizing surgery in the rabbit. Intraocular pressure and gross facility of aqueous outflow following surgery were not influenced by either treatment, although blebs persisted longer in the irradiated eyes. Steroids reduced clinically observable inflammation as well as the number of inflammatory cells identifiable by microscopy. Fibroblast production temporarily slowed, and ultrastructural examination demonstrated lipid-filled vacuoles and dilated mitochondria in these eyes. Also, the scar was thinner at 24 days. Beta irradiation delayed wound healing and the scar was thinner in the early postoperative stages, but the light microscopic appearance of the scar was unaltered at 59 days. Inflammation was more pronounced initially, with abundant fibrin in ...
Irradiation performance of metallic driver fuel in Experimental Breeder Reactor II to high burnup
1980-08-01
The Experimental Breeder Reactor II Mark-II metallic-driver-fuel element has been irradiated to high burnup to assess element lifetime and performance reliability. The purpose of this paper is to describe the irradiation performance of the Mark-II fuel element to 10 at.% burnup. Fission gas behavior, fuel deformation, fuel-cladding chemical interaction, fuel-cladding mechanical interaction, and cladding dilation are examined for their effect on Mark-II behavior. 27 refs.
Stochastic annealing simulation of copper under neutron irradiation
1998-03-01
This report is a summary of a presentation made at ICFRM-8 on computer simulations of defect accumulation during irradiation of copper to low doses at room temperature. The simulation results are in good agreement with experimental data on defect cluster densities in copper irradiated in RTNS-II.
The quasar-frame velocity distribution of narrow C iv absorbers
2008-01-01
ABSTRACT We report on a survey for narrow (full widths at half-minimum -1) C iv absorption lines in a sample of bright quasars at redshifts Formula Not Shown in the Sloan Digital Sky Survey. Our main goal is to understand the relationship of narrow C iv absorbers to quasar outflows and, more generally, to quasar environments. We determine velocity zero-points using the broad Mg ii emission line, and then measure the absorbers' quasar-frame velocity distribution. We examine the distribution of lines arising in quasar outflows by subtracting model fits to the contributions from cosmologically intervening absorbers and absorption due to the quasar host galaxy or cluster environment. We find that a substantial number ( Formula Not Shown per cent) of absorbers with Formula Not Shown A in the ve...
Interferometric observations of the 1-0 transition of HCO(+) toward NGC 7538 IRS 1
Interferometric observations of the molecular cloud toward the compact H II region IRS 1 in NGC 7538 in the 1-0 line of HCO(+) are reported. Employing a resolution of 8.5 arcsec, a highly elongated molecular cloud oriented at position angle 52 deg is found, perpendicular to the axis of the bipolar CO outflow. In perfect alignment with the blueshifted lobe in CO, strong blueshifted line wings are detected in HCO(+). The origin of the flow is at the center of the HCO(+) cloud, 15 arcsec to the south of IRS 1, which is clearly not the source that powers this outflow. So far no other indication of star formation has been detected at this position. 8 references.
Interferometric observations of the 1-0 transition of HCO(+) toward NGC 7538 IRS 1
1988-07-01
Interferometric observations of the molecular cloud toward the compact H II region IRS 1 in NGC 7538 in the 1-0 line of HCO(+) are reported. Employing a resolution of 8.5 arcsec, a highly elongated molecular cloud oriented at position angle 52 deg is found, perpendicular to the axis of the bipolar CO outflow. In perfect alignment with the blueshifted lobe in CO, strong blueshifted line wings are detected in HCO(+). The origin of the flow is at the center of the HCO(+) cloud, 15 arcsec to the south of IRS 1, which is clearly not the source that powers this outflow. So far no other indication of star formation has been detected at this position. 8 references.
Interferometric observations of the 1-0 transition of HCO(+) toward NGC 7538 IRS 1
1988-01-01
Interferometric observations of the molecular cloud toward the compact H II region IRS 1 in NGC 7538 in the 1-0 line of HCO(+) are reported. Employing a resolution of 8.5 arcsec, a highly elongated molecular cloud oriented at position angle 52 deg is found, perpendicular to the axis of the bipolar CO outflow. In perfect alignment with the blueshifted lobe in CO, strong blueshifted line wings are detected in HCO(+). The origin of the flow is at the center of the HCO(+) cloud, 15 arcsec to the south of IRS 1, which is clearly not the source that powers this outflow. So far no other indication of star formation has been detected at this position. 8 references
Gemini observations of disks and jets in young stellar objects and in active galaxies
We present first results from the Near-infrared Integral Field Spectrograph (NIFS) located at Gemini North. For the active galaxies Cygnus A and Perseus A we observe rotationally-supported accretion disks and adduce the existence of massive central black holes and estimate their masses. In Cygnus A we also see remarkable high-excitation ionization cones dominated by photoionization from the central engine. In the T-Tauri stars HV Tau C and DG Tau we see highly-collimated bipolar outflows in the [Fe II] ? 1.644 micron line, surrounded by a slower molecular bipolar outflow seen in the H2 lines, in accordance with the model advocated by Pyo, T.-S., et al., Astrophys. J. 570, 724 (2002).
Gemini Observations of Disks and Jets in Young Stellar Objects and in Active Galaxies
2007-06-04
We present first results from the Near-infrared Integral Field Spectrograph (NIFS) located at Gemini North. For the active galaxies Cygnus A and Perseus A we observe rotationally-supported accretion disks and adduce the existence of massive central black holes and estimate their masses. In Cygnus A we also see remarkable high-excitation ionization cones dominated by photoionization from the central engine. In the T-Tauri stars HV Tau C and DG Tau we see highly-collimated bipolar outflows in the [Fe II] 1.644 micron line, surrounded by a slower molecular bipolar outflow seen in the H_2 lines, in accordance with the model advocated by Pyo et al. (2002).
Irradiation experiments of recycled PuO2-UO2 fuels by SAXTON reactor, (5). Fuel performance analysis
1975-01-01
The post-irradiation examination results of mixed oxide fuels irradiated in SAXTON reactor are used for the verification of a fuel performance analysis code ''ACTIVE-II'', and the performance of the fuels under irradiation is estimated by the ACTIVE-II code. (auth.)
The Enigmatic Young Low-Mass Variable TWA 30
2010-03-19
TWA 30 is a remarkable young (7+/-3 Myr), low-mass (0.12+/-0.04 Msun), late-type star (M5+/-1) residing 42+/-2 pc away from the sun in the TW Hydrae Association. It shows strong outflow spectral signatures such as [S II], [O I], [O II], [O III], and Mg I], while exhibiting weak Halpha emission (-6.8+/-1.2 Angstroms). Emission lines of [S II] and [O I] are common to T Tauri stars still residing in their natal molecular clouds, while [O III] and Mg I] emission lines are incredibly rare in this same population; in the case of TWA 30, these latter lines may arise from new outflow material colliding into older outflow fronts. The weak Halpha emission and small radial velocity shifts of line emission relative to the stellar frame of rest (generally <=10 km/s) suggest that the disk is viewed close to edge-on and that the stellar axis may be inclined to the disk, similar to the AA Tau system, based on its temporal changes in emission/absorption line strengths/profiles and variable reddening (A_V=1.5-9.0). The strong Li absorption (0.61+/-0.13 Angstroms) and common kinematics with members of the TWA confirm its age and membership to the association. Given the properties of this system such as its proximity, low mass, remarkable outflow signatures, variability, and edge-on configuration, this system is a unique case study at a critical time in disk evolution and planet-building processes.
Dynamics of Rotating Accretion Flows Irradiated by a Quasar
2007-08-31
We study the axisymmetric, time-dependent hydrodynamics of rotating flows that are under the influence of supermassive black hole gravity and radiation from an accretion disk surrounding the black hole. This work is an extension of the earlier work presented by Proga, where nonrotating flows were studied. Here, we consider effects of rotation, a position-dependent radiation temperature, density at large radii, and uniform X-ray background radiation. As in the non-rotating case, the rotating flow settles into a configuration with two components (1) an equatorial inflow and (2) a bipolar inflow/outflow with the outflow leaving the system along the pole. However, with rotation the flow does not always reach a steady state. In addition, rotation reduces the outflow collimation and the outward flux of mass and kinetic energy. Moreover rotation increases the outward flux of the thermal energy and can lead to fragmentation and time-variability of the outflow. We also show that a position-dependent radiation temperature can significantly change the flow solution. In particular, the inflow in the equatorial region can be replaced by a thermally driven outflow. Generally, as it have been discussed and shown in the past, we find that self-consistently determined preheating/cooling from the quasar radiation can significantly reduce the rate at which the central BH is fed with matter. However, our results emphasize also a little appreciated feature. Namely, quasar radiation drives a non-spherical, multi-temperature and very dynamic flow. These effects become dominant for luminosities in excess of 0.01 of the Eddington luminosity.
Two-component jet simulations: II. Combining analytical disk and stellar MHD outflow solutions
2009-05-22
Theoretical arguments along with observational data of YSO jets suggest the presence of two steady components: a disk wind type outflow needed to explain the observed high mass loss rates and a stellar wind type outflow probably accounting for the observed stellar spin down. Each component's contribution depends on the intrinsic physical properties of the YSO-disk system and its evolutionary stage. The main goal of this paper is to understand some of the basic features of the evolution, interaction and co-existence of the two jet components over a parameter space and when time variability is enforced. Having studied separately the numerical evolution of each type of the complementary disk and stellar analytical wind solutions in Paper I of this series, we proceed here to mix together the two models inside the computational box. The evolution in time is performed with the PLUTO code, investigating the dynamics of the two-component jets, the modifications each solution undergoes and the potential steady state reached.
The three-dimensional structure of sunspots II. The moat flow at two different heights
2009-12-21
Many sunspots are surrounded by a radial outflow called the moat flow. We investigate the moat flow at two different heights of the solar atmosphere for a sunspot whose magnetic properties were reported in the first paper of this series. We use two simultaneous time series taken with the Transition Region And Coronal Explorer (TRACE) in white light and in the UV at 170 nm. The field-of-view is centered on the small sunspot NOAA 10886 located near disk center. Horizontal velocities are derived by applying two different local correlation tracking techniques. Outflows are found everywhere in the moat. In the inner moat, the velocities from the UV series are larger than those from white light, whereas in the outer part of the moat we find the converse result. The results imply that the white light velocities represent a general outflow of the quiet sun plasma in the moat, while UV velocities are dominated by small bright points that move faster than the general plasma flow.
A WIDE-FIELD NARROWBAND OPTICAL SURVEY OF THE BRAID NEBULA STAR FORMATION REGION IN CYGNUS OB7
We study the population of Herbig-Haro (HH) flows and jets in an area of Cygnus OB7 designated the Braid Nebula star formation region. This complex forms part of the L 1003 dark cloud, and hosts two FU Orionis (FUor)-like objects as well as several other active young stars. To trace outflow activity and to relate both known and newly discovered flows to young star hosts we intercompare new, deep, narrowband H{alpha} and [S II] optical images taken on the Subaru 8 m Telescope on Mauna Kea, Hawaii. Our images show that there is considerable outflow and jet activity in this region suggesting the presence of an extensive young star population. We confirm that both of the FUor-like objects drive extensive HH flows and document further members of the flows in both objects. The L 1003 star formation complex is a highly kinematically active region with young stars in several different stages of evolution. We trace collimated outflows from numerous young stars although the origin of some HH objects remains elusive.
Multi-dimensional modelling of X-ray spectra for AGN accretion-disk outflows II
2010-02-03
Highly-ionized fast accretion-disk winds have been suggested as an explanation for a variety of observed absorption and emission features in the X-ray spectra of Active Galactic Nuclei. Simple estimates have suggested that these flows may be massive enough to carry away a significant fraction of the accretion energy and could be involved in creating the link between supermassive black holes and their host galaxies. However, testing these hypotheses, and quantifying the outflow signatures, requires high-quality theoretical spectra for comparison with observations. Here we describe extensions of our Monte Carlo radiative transfer code that allow us to generate realistic theoretical spectra for a much wider variety of disk wind models than possible in our previous work. In particular, we have expanded the range of atomic physics simulated by the code so that L- and M-shell ions can now be included. We have also substantially improved our treatment of both ionization and radiative heating such that we are now able to compute spectra for outflows containing far more diverse plasma conditions. We present example calculations that illustrate the variety of spectral features predicted by parametrized outflow models and demonstrate their applicability to the interpretation of data by comparison with observations of the bright quasar PG1211+143. We find that the major features in the observed 2 - 10 keV spectrum of this object can be wel l-reproduced by our spectra, confirming that it likely hosts a massive outflow.
By using the Integral Field Spectroscopy mode of the Kyoto Tri-dimensional Spectrograph II we have mapped the two-dimensional distribution of kinematics in a wide variety of emission lines in the narrow-line region of NGC 4151. We decomposed the emission lines and defined two components: a narrow component and a broad component. The narrow component has smaller FWHM values, and is spatially more extended than the broad component. We applied a simple model to each component, a rotation in the galactic plane for the narrow component and a biconical outflow model for the broad one. The two-dimensional velocity distributions of the narrow component was well-fitted to a normal rotation in the galactic plane, with the best-fit parameters being similar among the emission lines. We found that the residual maps show similar large positive values at a knot around 6'' southwest form the nucleus. For the central region, excluding the knot, the velocity field was fitted better, and the residual was small as the relative wavelength-calibration accuracy of the instrument among lenslets. We modeled the broad component with a simple biconical outflow axisymmetrical with respect to its axis by assuming a constant outflowing velocity, a constant FWHM value, and the emission line strength declining according to a power law with the distance from the nucleus. The best-fit model suggests that PA for the axis of the biconical outflow is close to the direction of the [OIII] line emission elongation. Our line of sight was included within the outflowing bicone, which had filled cones.
WIDE-FIELD NEAR-INFRARED IMAGING OF THE L1551 DARK CLOUD
2009-01-01
We present wide-field near-infrared images of the densest part of the L1551 dark cloud taken with the narrow-band filters for [Fe II] lambda 1.644 mum and H2 v = 1-0 S(1) lines, together with the broadband H and K s filters. Numerous [Fe II] and H2 emission features were detected from the regions around HL/XZ Tau, HH 30, HH 262, L1551 NE, and L1551 IRS 5. Most of the [Fe II] features are compact or jet-like, suggesting that the emission arises from fast shocks occurring in the ejecta of jets. The H2 features are more diffuse and widely distributed in outflow lobes, with none of the H2 features showing the well-collimated emission associated with jets. This implies that the H2 emission originates from slower shocks where the ejecta interacts with ambient material. The outflow structure ...
HST Observations of Chromospheres in Metal Deficient Field Giants
2007-09-13
HST high resolution spectra of metal-deficient field giants more than double the stars in previous studies, span about 3 magnitudes on the red giant branch, and sample an abundance range [Fe/H]= -1 to -3. These stars, in spite of their age and low metallicity, possess chromospheric fluxes of Mg II (2800 Angstrom) that are within a factor of 4 of Population I stars, and give signs of a dependence on the metal abundance at the lowest metallicities. The Mg II k-line widths depend on luminosity and correlate with metallicity. Line profile asymmetries reveal outflows that occur at lower luminosities (M_V = -0.8) than detected in Ca K and H-alpha lines in metal-poor giants, suggesting mass outflow occurs over a larger span of the red giant branch than previously thought, and confirming that the Mg II lines are good wind diagnostics. These results do not support a magnetically dominated chromosphere, but appear more consistent with some sort of hydrodynamic, or acoustic heating of the outer atmospheres.
2010-09-07
IPHASXJ194359.5+170901 is a new high-excitation planetary nebula with remarkable characteristics. It consists of a knotty ring expanding at a speed of 28 km/s, and a fast collimated outflow in the form of faint lobes and caps along the direction perpendicular to the ring. The expansion speed of the polar caps is 100 km/s, and their kinematical age is twice as large as the age of the ring. Time-resolved photometry of the central star of IPHASXJ194359.5+170901 reveals a sinusoidal modulation with a period of 1.16 days. This is interpreted as evidence for binarity of the central star, the brightness variations being related to the orbital motion of an irradiated companion. This is supported by the spectrum of the central star in the visible range, which appears to be dominated by emission from the irradiated zone, consisting of a warm (6000-7000 K) continuum, narrow C III, C IV, and N III emission lines, and broader lines from a flat H I Balmer sequence in emission. IPHASXJ194359.5+170901 helps to clarify the role of (close) binaries in the formation and shaping of planetary nebulae. The output of the common-envelope evolution of the system is a strongly flattened circumstellar mass deposition, a feature that seems to be distinctive of this kind of binary system. Also, IPHASXJ194359.5+170901 is among the first post-CE PNe for which the existence of a high-velocity polar outflow has been demonstrated. Its kinematical age might indi cate that the polar outflow is formed before the common-envelope phase. This points to mass transfer onto the secondary as the origin, but alternative explanations are also considered.
1989-01-01
The Japanese experimental fast reactor JOYO MK-II has been operated at 100 MW since March 1983 as a fuel and material irradiation facility. Many types of fuel irradiation tests for the prototype reactor MONJU and demonstration type fast breeder reactor FBR have been conducted by using four types of irradiation rings, including an instrumented test assembly (INTA). The paper discusses experience with driver fuel irradiation and MONJU-type fuel irradiation tests.
Preirradiation Data summary for the GRIT-II HTGR irradiation test specimens
1995-05-01
This document comprises a report of preirradiation data on the NPR-5 and NPR-8 fuel types tested in the GRIT-II HTGR Irradiation Test in the Advanced Test Reactor. A summary of fuel characterization, GRIT-II test fabrication data, outlines of fabrication procedures, and a discussion of the GRIT technique for individual fuel bead testing is presented. Objective of the test is to provide individual irradiated HTGR fuel beads for post-irradiation valuation with total target burnups of 25, 50, and 75% fissions of initial metal atoms (FIMA).
2009-10-05
We present the results of new spectral diagnostic investigations applied to high-resolution long-slit spectra of the RW Aur bipolar jet obtained with HST/STIS. The spectra include the forbidden doublets [O I] 6300,6363 \\AA, [S II] 6716,6731 \\AA, and [N II] 6548, 6583 \\AA that we utilized to determine electron density, electron temperature, hydrogen ionisation fraction, total hydrogen density, radial velocity and the mass outflow rate. We were able to extract the parameters as far as 3".9 in the red- and 2".1 in the blueshifted beam. The RW Aur jet appears to be the second densest outflow from a T Tauri star studied so far, but its other properties are quite similar to those found in other jets from young stars. The overall trend of the physical parameters along the first few arcseconds of the RW Aur jet is similar to that of HH 30 and DG Tau and this can reflect analogies in the mechanisms operating in that region, suggesting the same engine is accelerating the jets in the T Tauri stars with outflows. Our study of the RW Aur jet indicates for the first time that, despite the detected marked asymmetries in physical and kinematic properties between the two lobes, the mass outflow rates in the two lobes are similar. This appears to indicate that the central engine has constraining symmetries on both sides of the system, and that the observed asymmetries are probably due to different environmental conditions.
An analysis of a spectrum of V838 Monocerotis in October 2005
2009-07-06
V838 Mon erupted at the beginning of 2002. Among various scenarios proposed to explain the nature of the outburst, the most promising is a stellar merger event. The results of spectroscopic observations of the object obtained in October 2005 with the Keck/HIRES instrument, presented in detail in Paper I, are analysed and discussed. Our analysis of the molecular bands and the P-Cyg profiles of atomic lines shows that the object loses matter with a velocity of up to 215 km/s and a rate of 10^{-6} - 10^{-5} M_sun/yr. In the profiles of some atomic lines, we have also found evidence of matter infall. A narrow absorption component, which is particularly strong in some P-Cyg profiles, may indicate that a jet-like outflow has also been formed. We show that the observed emission in the [Fe II] lines and an eclipse-like event observed in November/December 2006 was probably caused by interactions of the expanding matter, ejected by V838 Mon in 2002, with radiation from the B3V companion. In particular, the observed profiles of the [Fe II] lines can be easily modelled in this scenario and allow us to estimate parameters of the system, such as the position of the B3V companion relative to V838 Mon and the line of sight, density in the outflowing matter, and mass lost in the 2002 eruption. The observed appearance of strong H-alpha emission, just before and during the eclipse-like event, can be interpreted as a result of the accretion of the outflowing matter onto the B3V companion: the accreted matter, shocked above the stellar surface, can be a source of extreme-UV and soft X-ray radiation capable of ionizing and exciting H in the outflow.
1985-07-01
The cell flow and cell loss of an in vivo growing Ehrlich ascites tumour were calculated by sequential estimation of changes in total number of cells in the cell cycle compartments. Normal growth was compared with the grossly disturbed cell flow evident after a 5 Gy X-irradiation. The doubling time of normal, exponentially growing cells was 24 hr. The generation time was 21 hr and the potential doubling time was 21 hr. Thus, the growth fraction was 1.0 and the cell loss rate about 0.5%/hr. Following irradiation, a transiently increased relative outflow rate from all cell cycle compartments was found at about 3 and 40 hr, and from S phase at 24 hr after irradiation. Increase in cell loss as well as non-viable cells was observed at 24 hr after irradiation at the time of release of the irradiation-induced G/sub 2/ blockage. The experiments show the applicability and limitations of cell flow and cell loss calculations by sequential analysis of the total number of cells in the various parts of the cell cycle.
Amount of mobilizable stem cells in perturbed hemopoiesis
1985-05-01
The level of mobilizable 9-day colony-forming units (CFU-s), which represents a constant fraction of the normal mouse bone marrow CFU-s pool, was assayed in BDF1 mice with perturbed hemopoiesis (i.e., during increased turnover of CFU-s or increased CFU-s traffic after irradiation). After low-level irradiation, regeneration of the mobilizable CFU-s fraction was significantly slower than that of bone marrow CFU-s. Depletion of the mobilizable CFU-s pool was observed if a permanently increased outflow of CFU-s from the bone marrow was induced by endotoxin injection. After 40% withdrawal of the blood volume, the mobilizable CFU-s pool expanded marginally. Assuming that the level of mobilizable CFU-s is a consequence of production and outflow from the bone marrow compartment, changes in the pool size of mobilizable CFU-s may be a sensitive indicator of balanced or unbalanced hemopoiesis.
The Intrinsic Absorber in QSO 2359-1241$$bKeck and HST Observations
2000-08-17
We present detailed analyses of the absorption spectrum seen in QSO 2359-1241 (NVSS J235953-124148). Keck HIRES data reveal absorption from twenty transitions arising from: He I, Mg I, Mg II, Ca II, and Fe II. HST data show broad absorption lines (BALs) from Al III 1857, C IV 1549, Si IV 1397, and N V 1240. Absorption from excited Fe II states constrains the temperature of the absorber to 2000K < T < 10,000K and puts a lower limit of 10^5 cm^{-3} on the electron number density. Saturation diagnostics show that the real column densities of He I and Fe II can be determined, allowing to derive meaningful constraints on the ionization equilibrium and abundances in the flow. The ionization parameter is constrained by the iron, helium and magnesium data to -3.0 < log(U) < -2.5 and the observed column densities can be reproduced without assuming departure from solar abundances. From comparison of the He I and Fe II absorption features we infer that the outflow seen in QSO 2359-1241 is not shielded by a hydrogen ionization front and therefore that the existence of low-ionization species in the outflow (e.g., Mg II, Al III, Fe II) does not necessitate the existence of such a front. We find that the velocity width of the absorption systematically increases as a function of ionization and to a lesser extent with abundance. Complementary analyses of the radio and polarization properties of the object are discussed in a companion paper (Brotherton et al. 2000).
A CLASS I AND CLASS II CH3OH MASER SURVEY OF EGOs FROM THE GLIMPSE SURVEY
2009-01-01
We present the results of a high angular resolution Very Large Array (VLA) Class I 44 GHz and Class II 6.7 GHz CH3OH maser survey of a sample of approx20 massive young stellar object (MYSO) outflow candidates selected on the basis of extended 4.5 mum emission in Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire images. These 4.5 mum selected candidates are referred to as extended green objects (EGOs), for the common coding of this band as green in three-color Infrared Array Camera images. The detection rate of 6.7 GHz Class II CH3OH masers, which are associated exclusively with massive YSOs, toward EGOs is approx
2008-04-08
We have carried out the observations of the OMC-2 FIR 3/4 region with the NMA and ASTE in the H$^{13}$CO$^{+}$ (1--0), $^{12}$CO (3--2, 1--0), SiO ($v$=0, $J$=2--1), CS (2--1), and CH$_3$OH ($J_K$=7$_K$--6$_K$) lines and in the 3.3 mm continuum emission. Our NMA observations in the H$^{13}$CO$^{+}$ emission have revealed 0.07 pc-scale dense gas associated with FIR 4. The $^{12}$CO (3--2,1--0) emission shows high-velocity blue and red shifted components at the both north-east and south-west of FIR 3, suggesting a molecular outflow nearly along the plane of the sky driven by FIR 3. The SiO and the CH$_{3}$OH emission are detected around the interface between the outflow and the dense gas. Furthermore, the $^{12}$CO (1--0) emission shows an L-shaped structure in the P-V diagram. These results imply presence of the shock due to the interaction between the molecular outflow driven by FIR 3 and the dense gas associated with FIR 4. Moreover, our high angular-resolution observations of FIR 4 in the 3.3 mm continuum emission have first found that FIR 4 consists of eleven dusty cores. The separation among these cores is on the same order of the Jeans length, suggesting that the fragmentation into these cores has been caused by the gravitational instability. The time scale of the fragmentation is similar to the time scale of the interaction between the molecular outflow and the dense gas. We suggest that the interaction between the molecu lar outflow from FIR 3 and the dense gas associated with FIR 4 triggered the fragmentation into these dusty cores, and hence the next generation the cluster formation.
RTNS-II fusion-neutron facility for material-damage studies
1983-06-01
The Rotating Target Neutron Source-II (RTNS-II) is operated by Lawrence Livermore National Laboratory (LLNL) for the US (DOE) and Japan (Monbusho). Joint support and utilization of the facility by Japan and the US has been in effect for nearly 1 1/2 years. Irradiations, using the fusion neutrons produced at RTNS-II, are done in support of the fusion energy programs of the US and Japan. In addition, add-on non-fusion related irradiations can and have been done at RTNS-II.
Optimization of a fuel converter for the MERLIN materials testing facility
1998-07-01
SCK-CEN is at the present time developing the MERLIN materials testing facility, to be placed in the pool at the BR2 high flux materials testing reactor. It aims at irradiating large amounts of steel samples that are subsequently to be analyzed in the framework of reactor vessel embrittlement research programmes. In order to fulfill the required fast neutron flux conditions, a converter made of highly enriched uranium fuel plates, has to be inserted between the reactor vessel and the samples. The converter will transform the BR2 thermal neutron outflow into the required fast neutron flux. This converter has to be optimised. (author)
Radio observation of electron acceleration at solar flare reconnection outflow termination shocks
2004-01-01
Using meter-wave solar radio spectral observations of the 2001 September 28 flare, we discuss simultaneously appearing type II-like bursts observed at 40-80 MHz and approx300 MHz as radio signatures of the upper and lower reconnection outflow termination shock (TS). The features are identified during the impulsive phase but well after the regular traveling-shock type II burst and during the rise of a coronal mass ejection. The upper and lower TS features reveal a tendency for flux anticorrelation over time. We use radio imaging data (Nancay radio heliograph) and Yohkoh soft X-ray images to support the TS hypothesis. Assuming shock drift acceleration, we compute the flux of accelerated electrons for lower TS conditions that lead to an electron population with energies of approx15 keV. (orig.)
2005-01-13
A study of outflow (OF) and BAL systems in Mrk 231 (and in similar IR QSOs) is presented. This study is based mainly on 1D and 2D spectroscopy (obtained at La Palma/WHT, HST, IUE, ESO/NTT, KPNO, APO and CASLEO observatories) plus HST images. For Mrk 231 we report evidence that the extreme nuclear OF process has at least 3 main components, which are probably associated with: (i) the radio jet, at pc scale, and (ii(the extreme starburst at pc and kpc scale. This OF has generate 4 or more concentric expanding bubbles and the BAL systems. The variability of the short lived BAL-III system was studied. Finally, the IR colour diagram and the UV BAL system of IR+OF+FeII QSOs are analysed. We propose that the phase of young QSO is associated with:accretion of large amount of gas (by the SMBH)+extreme starburst+extreme composite OFs/BALs.
Gamma Ray Bursts: back to the blackboard
2009-11-03
Exceptional observational breakthroughs in the field of Gamma Ray Burst research are not paralleled by theoretical advances. In this review, based on the introductory talk given at the "The Shocking Universe" meeting, I argue that any present day model of GRBs, especially of Short type, is grossly incomplete. I will highlight various contradictions with observations that many models face and briefly mention a number of ideas that might or might not work. In particular, I will discuss (i) a possibility that early X-ray afterglows are coming from internal dissipation, and not from the forwards shock; (ii) that prompt radiation is beamed in the outflow frame.
Compact molecular disc and ionized gas outflows within 350 pc of the active nucleus of Mrk 1066
2010-09-27
We present stellar and gaseous kinematics of the inner 350 pc radius of the Seyfert galaxy Mrk1066 derived from J and Kl bands data obtained with the Gemini NIFS at a spatial resolution of 35 pc. The stellar velocity field is dominated by rotation in the galaxy plane but shows an S-shape distortion along the galaxy minor axis which seems to be due to an oval structure seen in an optical continuum image. Along this oval, between 170 and 280 pc from the nucleus we find a partial ring of low sigma (~50 km/s) attributed to an intermediate age stellar population. Fro measurements of the emission-line fluxes and profiles ([PII]1.19um, [FeII]1.26um, Pa-beta and H2 2.12um), we have constructed maps for the gas centroid velocity, velocity dispersion, as well as channel maps. The velocity fields for all emission lines are dominated by a similar rotation pattern to that observed for the stars, but are distorted by the presence of two structures: (i) a compact rotating disc with radius r~70 pc; (ii) outflows along the radio jet which is oriented approximately along the galaxy major axis. The compact rotating disc is more conspicuous in the H2 emitting gas, which presents the smallest sigma values and most clear rotation pattern, supporting a location in the galaxy plane. We estimate a gas mass for the disc of ~10^7Msun. The H2 kinematics further suggests that the nuclear disc is being fed by gas coming from the outer regions. The outflow i s more conspicuous in the [FeII] emitting gas, which presents the highest sigma values (up to 150 km/s) and the highest blue and redshifts of up to 500 km/s, while the highest stellar rotation velocity is only 130 km/s. We estimate a mass-outflow rate in ionized gas of 0.06 Msun/yr. The derived kinematics for the emitting gas is similar to that observed in previous studies supporting that the H2 is a tracer of the AGN feeding and the [FeII] of its feedback.
Post irradiation test report of irradiated DUPIC simulated fuel
2001-12-01
The post-irradiation examination of irradiated DUPIC (Direct Use of Spent PWR Fuel in CANDU Reactors) simulated fuel in HANARO was performed at IMEF (Irradiated Material Examination Facility) in KAERI during 6 months from October 1999 to March 2000. The objectives of this post-irradiation test are i) the integrity of the capsule to be used for DUPIC fuel, ii) ensuring the irradiation requirements of DUPIC fuel at HANARO, iii) performance verification in-core behavior at HANARO of DUPIC simulated fuel, iv) establishing and improvement the data base for DUPIC fuel performance verification codes, and v) establishing the irradiation procedure in HANARO for DUPIC fuel. The post-irradiation examination performed are {gamma}-scanning, profilometry, density, hardness, observation the microstructure and fission product distribution by optical microscope and electron probe microanalyser (EPMA)
Development of irradiation technology for MK-III
2003-01-01
In addition to 6 types of off-line rigs (UNIS-A, -B, -C, and CMIR, SMIR, AMIR) and 4 types of on-line rigs (Instrumented Test Assembly: INTA, Material Test Rig with Temperature Control: MARICO, Upper Core Structure Irradiation Plug Rig: UPR, EX-Vessel Irradiation Rig: EXIR) used in the ''JOYO'' MK-II core, a capsule type irradiation rig, the upgrading of MARICO and D-type irradiation fuel assembly were newly developed in order to conduct irradiation tests of various fuels and materials. In addition, the development of an evaluation code, dosimeter and temperature monitor has been advanced in order to grasp irradiation conditions such as irradiation temperature and fluence accurately. Here, the present state of the irradiation technology development is described. (author)
ATCA 3 mm observations of NGC 6334I and I(N): dense cores, outflows, and an UCH II region
2008-01-01
Aims.We investigate the dense gas, the outflows, and the continuum emission from the massive twin cores NGC 6334I and I(N) at high spatial resolution. Methods.We imaged the region with the Australia Telescope Compact Array (ATCA) at 3.4 mm wavelength in continuum, as well as CH3CN (5K-4K) and HCN(1-0) spectral line emission. Results.While the continuum emission in NGC 6334I mainly traces the UCHII region, toward NGC 6334I(N) we detect continuum emission from four of the previously identified dust continuum condensations that are of protostellar or pre-stellar nature. The CH3CN (5K-4K) lines are detected in all K-components up to energies of 128 K aboveground toward two protostellar condensations in both regions. We find line width increasing with increasing K for all sources, which indicates a higher degree of internal motions of the hotter gas probed by these high K-transitions. Toward the main mm and CH3CN source in NGC 6334I, we identify a velocity gradient approximately perpendicular to the large-scale molecular outflow. This may be interpreted as a signature of an accretion disk, although other scenarios, e.g., an unresolved double source, could produce a similar signature. No comparable signature is found toward any of the other sources. HCN does not trace the dense gas well in this region but it is dominated by the molecular outflows. While the outflow in NGC 6334I exhibits a normal Hubble-law like velocity structure, the data are consistent with a precessing outflow close to the plane of the sky for NGC 6334I(N). Furthermore, we observe a wide (~15.4 km s-1) HCN absorption line, much broader than the previously observed CH3OH and NH3 absorption lines. Several explanations for the difference are discussed. The fits-files of the 3.4 mm continuum images and of the HCN(1-0) and CH3CN (5K-4K) data-cubes are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/481/169 Publisher: EDP Sciences Format: application/pdf Other identifier: Beuther, H., Walsh, A.J., Thorwith, S., Zhang, Q., Hunter, T.R., Megeath, S.T., and Menten, K.M. (2008) ATCA 3 mm observations of NGC 6334I and I(N): dense cores, outflows, and an UCH II region. Astronomy & Astrophysics, 481 (1). pp. 169-181. ISSN 1432-0746
Star formation in the Cometary Globule Ori I-2
2009-10-13
We investigate the young stellar population in and near the cometary globule Ori,I-2. The analysis is based on deep Nordic Optical Telescope R-band and H-alpha images, JCMT SCUBA 450 and 850 micron images combined with near-infrared 2MASS photometry and mid-infrared archival Spitzer images obtained with the IRAC (3.6, 4.5, 5.8 and 8 micron), and MIPS (24 and 70 micron) instruments. We identify a total of 125 sources within the 5'x5' region imaged by IRAC. Of these sources 87 are detected in the R-band image and 51 are detected in the 2MASS survey. The detailed physical properties of the sources are explored using a combination of near/mid-infrared color-color diagrams, greybody fitting of SEDs and an online SED fitting tool that uses a library of 2D radiation transfer based accretion models of young stellar objects with disks. Ori I-2 shows clear evidence of triggered star formation with four young low luminosity pre-main sequence stars embedded in the globule. At least two, possibly as many as four, additional low-mass PMS objects, were discovered in the field which are probably part of the young sigma-Orionis cluster. Among the PMS stars which have formed in the globule, MIR-54 is a young, deeply embedded Class 0/I object, MIR-51 and 52 are young Class II sources, while MIR-89 is a more evolved, heavily extincted Class II object with its apparent colors mimicking a Class 0/I object. The Class II source, MIR-52, which is stron g a H-alpha emission line star appears to drive an outflow approximately aligned with the outflow from MIR-54, and because of the proximity of the two outflows, either star could contribute. MIR-89 appears to excite a low excitation HH object, HH 992, discovered for the first time in this study.
High Angular Resolution [Fe II] ?1.644 ?m Spectroscopy of YSOs with Subaru Telescope
We present results of the velocity-resolved spectroscopy of the [Fe II] ?1.644 ?m emission toward outflow sources with the Subaru Telescope at the angular resolution of 0.16'' ? 0.5'' arcseconds. The observed sources are L1551 IRS 5, DG Tau, HL Tau and RW Aur, which are located in the Taurus-Aurigae Molecular Cloud, one of the closest star forming regions (0.1'' = 14 AU). We were able to resolve outflow structure in the vicinity of the sources at a scale of a few tens of AU. The position-velocity diagram of each object shows two velocity components: the high velocity component (HVC: 200 - 400 kms) and the low velocity component (LVC: 50 - 150 kms), which are clearly distinct in space and velocity. The HVC may be a highly collimated jet presumed from its narrow velocity width and high velocity. The LVC, on the other hand, may be a widely opened disk wind inferred from its broad velocity width and low velocity. The spectrum taken perpendicular to the L1551 IRS 5 outflow at its base shows that the LVC has a spatially wide subcomponent, supporting the above interpretation. We demonstrated that the [Fe II] 1.644 ? spectroscopy is a very powerful tool for the studies of fast jets and winds that directly emanate from star-disk systems.
1990-01-01
We studied the effect of topical dexamethasone (1%) and preoperative beta irradiation on a model of glaucoma fistulizing surgery in the rabbit. Intraocular pressure and gross facility of aqueous outflow following surgery were not influenced by either treatment, although blebs persisted longer in the irradiated eyes. Steroids reduced clinically observable inflammation as well as the number of inflammatory cells identifiable by microscopy. Fibroblast production temporarily slowed, and ultrastructural examination demonstrated lipid-filled vacuoles and dilated mitochondria in these eyes. Also, the scar was thinner at 24 days. Beta irradiation delayed wound healing and the scar was thinner in the early postoperative stages, but the light microscopic appearance of the scar was unaltered at 59 days. Inflammation was more pronounced initially, with abundant fibrin in the wound. Recovery of the conjunctival epithelium was delayed. The delay in fibroblast recruitment and wound contraction, the thinner scar tissue, and the increased survival of the bleb are all factors that suggest that beta irradiation may be a useful adjunct to glaucoma surgery.
2010-05-26
B[e] supergiants are surrounded by large amounts of hydrogen neutral material, traced by the emission in the optical [OI] lines. This neutral material is most plausibly located within their dense, cool circumstellar disks, which are formed from the (probably non-spherically symmetric) wind material released by the star. Neither the formation mechanism nor the resulting structure and internal kinematics of these disks (or disk-like outflows) are well known. However, rapid rotation, lifting the material from the equatorial surface region, seems to play a fundamental role. The B[e] supergiant LHA 115-S 65 (S65) in the SMC is one of the two most rapidly rotating B[e] stars known. Its almost edge-on orientation allows a detailed kinematical study of its optically thin forbidden emission lines. With a focus on the [OI] lines, we test the two plausible disk scenarios: the outflowing and the Keplerian rotating disk. Based on high- and low-resolution optical spectra, we investigate the density and temperature structure in those disk regions that are traced by the [OI] emission to constrain the disk sizes and mass fluxes needed to explain the observed [OI] line luminosities. In addition, we compute the emerging line profiles expected for either an outflowing disk or a Keplerian rotating disk, which can directly be compared to the observed profiles. Both disk scenarios deliver reasonably good fits to the line luminosities and profiles of the [OI] lines. Nevertheless, the Keplerian disk model seems to be the more realistic one, because it also agrees with the kinematics derived from the large number of additional lines in the spectrum. As additional support for the presence of a high-density, gaseous disk, the spectrum shows two very intense and clearly double-peaked [CaII] lines. We discuss a possible disk-formation mechanism, and similarities between S65 and the group of LBVs.
Hierarchical Growth and Cosmic Star Formation: Enrichment, Outflows and Supernova Rates
The cosmic star formation histories are evaluated for different minimum masses of the initial halo structures, with allowance for realistic gas outflows. With a minimum halo mass of 10^{7} - 10^{8} M_odot and a moderate outflow efficiency, we reproduce both the current baryon fraction and the early chemical enrichment of the IGM. The intensity of the formation rate of ``normal'' stars is also well constrained by the observations: it has to be dominated by star formation in elliptical galaxies, except perhaps at very low redshift. The fraction of baryons in stars is predicted as are also the type Ia and II supernova event rates. Comparison with SN observations in the redshift range z=0-2 allows us to set strong constraints on the time delay of type Ia supernovae (a total delay of \\sim 4 Gyr is required to fit the data), the lower end of the mass range of the progenitors (2 - 8 M_odot) and the fraction of white dwarfs that reproduce the type Ia supernova (about 1 per cent). The intensity in the initial starburst of zero metallicity stars below 270 M_\\odot must be limited in order to avoid premature overenrichment of the IGM. Only about 10 - 20 % of the metals present in the IGM at z = 0 have been produced by population III stars at very high z. The remaining 80 - 90 % are ejected later by galaxies forming normal stars, with a maximum outflow efficiency occurring at a redshift of about 5. We conclude that 10^{-3} of the mass in baryons must lie in first massive stars in order to produce enough ionizing photons to allow early reionization of the IGM by z \\sim 15.
Disassembly of irradiated lithium-bonded capsules containing vanadium alloy specimens
1996-04-01
Capsules containing vanadium alloy specimens from irradiation experiments in FFTF and EBR-II are being processed to remove the lithium bond and retrieve the specimens for testing. The work has progressed smoothly.
Experience with automatic reactor control at EBR-II
1985-01-01
Satisfactory operation of the ACRDS has extended the capabilities of EBR-II to a transient test facility, achieving automatic transient control. Test assemblies can now be irradiated in transient conditions overlapping the slower transient capability of the TREAT reactor.
Microstructural comparison of HT-9 irradiated in HFIR and EBR-II
A series of specimens of HT-9 heat 91354 have been examined following irradiation in HFIR to 39 dpa at 300, 400, 500 and 600/sup 0/C and following irradiation in EBR-II to 29 dpa at 390 and 500/sup 0/C. HFIR irradiation was found to have promoted helium bubble formation at all temperatures and voids at 400/sup 0/C. Cavitation had not been observed at lower fluence, nor was it found in EBR-II irradiated specimens. The onset of void swelling in HFIR is attributed to helium generation. The observations provide an explanation for saturation of ductile-brittle transition temperature shifts with increasing fluence.
Microstructural comparison of HT-9 irradiated in HFIR and EBR-II
1985-05-01
A series of specimens of HT-9 heat 91354 have been examined following irradiation in HFIR to 39 dpa at 300, 400, 500 and 600/sup 0/C and following irradiation in EBR-II to 29 dpa at 390 and 500/sup 0/C. HFIR irradiation was found to have promoted helium bubble formation at all temperatures and voids at 400/sup 0/C. Cavitation had not been observed at lower fluence, nor was it found in EBR-II irradiated specimens. The onset of void swelling in HFIR is attributed to helium generation. The observations provide an explanation for saturation of ductile-brittle transition temperature shifts with increasing fluence.
Tensile properties of 9Cr-1MoVNb and 12Cr-1MoVW steels irradiated to 23 dpa at 390 to 550deg C
1991-01-01
Normalized-and-tempered 9Cr-1MoVNb and 12Cr-1MoVW steels were irradiated in the Experimental Breeder Reactor II (EBR-II) at 390, 450, 500, and 550deg C to displacement damage levels of up to 23 to 25 dpa. Tensile tests were conducted at the irradiation temperatures on three types of specimens: irradiated specimens, normalized-and-tempered specimens, and specimens thermally aged 5000 h at the irradiation temperatures. Observations from these tests were compared with results on these same materials irradiated in EBR-II at the same temperatures to 9 to 13 dpa. Irradiation of specimens at 390deg C to 23 to 25 dpa caused an increase in strength and a decrease in ductility relative to the aged and unaged control specimens. However, there was little change from the specimens irradiated to 9 to 13 dpa. After irradiation at 450, 500, and 550deg C, there was little difference between ...
The synthesis of the covalent linkage of Cobalt(II)tetrasulfophthalocyanine (Co(II)TSP) to the surface of titanium dioxide (TiO2) particles is described. Upon irradiation with light, which exceeds the bandgap energy of TiO2, Co(II)TSP is reduced to Co(I)TSP under anoxic condition...
The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel Space Observatory allows the first observations of light diatomic molecules at high spectral resolution and in multiple transitions. Here, we report deep integrations using HIFI in different lines of hydrides towards the high-mass star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+ and SH+ have not been detected. All molecules except for CH and CH+ are seen in absorption with low excitation temperatures and at velocities different from the systemic velocity of the protostellar envelope. Surprisingly, the CH(JF,P = 3/22,- - 1/21,+ ) and CH+(J = 1-0, J = 2-1) lines are detected in emission at the systemic velocity. We can assign the absorption features to a foreground cloud and an outflow lobe, while the CH and CH+ emission stems from the envelope. The observed abundance and excitation of CH and CH+ can be explained in the scenario of FUV irradiated outflow walls, where a cavity etched out by the outflow allows protostellar FUV photons to irradiate and heat the envelope at larger distances driving the chemical reactions that produce these molecules. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Apppendices and Table 1 (pages 6 to 7) are only available in electronic form at http://www.aanda.org
The complex structure of HH 110 as revealed from Integral Field Spectroscopy
2010-01-01
ABSTRACT HH 110 is a rather peculiar HerbigHaro object in Orion that originates due to the deflection of another jet (HH 270) by a dense molecular clump, instead of being directly ejected from a young stellar object. Here we present new results on the kinematics and physical conditions of HH 110 based on Integral Field Spectroscopy. The 3D spectral data cover the whole outflow extent (4.5 arcmin, 0.6 pc at a distance of 460 pc) in the spectral range 6500-7000 A. We built emission-line intensity maps of Ha, [N ii] and [S ii] and of their radial velocity channels. Furthermore, we analysed the spatial distribution of the excitation and electron density from [N ii]/Ha, [S ii]/Ha and [S ii] 6716/6731 integrated line-ratio maps, as well as their behaviour as a function of velocity, from line-rat...
STAR FORMATION IN RELIC H II REGIONS OF THE FIRST STARS: BINARITY AND OUTFLOW DRIVING
2009-01-01
Star formation in relic H II regions of the first stars is investigated using magnetohydrodynamical simulations with a nested-grid method that covers approx10 orders of magnitude in spatial scale and approx20 orders of magnitude in density contrast. Due to larger fraction of H2 and HD molecules, its prestellar thermal evolution is considerably different from that in the first star formation. Reflecting the difference, two hydrostatic cores appear in a nested manner: a protostar is enclosed by a transient hydrostatic core, which appears during the prestellar collapse. If the initial natal core rotates fast at a rate with rotational to gravitational energy ratio beta0 approx
1992-09-01
The BEATRIX-II irradiation experiment was an in situ, fast neutron, tritium release experiment to evaluate the performance of ceramic fusion solid breeders at extended burnups. The experiment consisted of two sequential irradiations: Phase I for 300 EFPD and Phase II for 200 EFPD that resulted in lithium burnups from 4{endash}6%. Thin-walled Li{sub 2}O ring specimens capable of temperature changes were irradiated in both Phase I and Phase II. Temperature changes were also used to determine the tritium inventory and to characterize the effect or irradiation history and sweep gas composition. Solid-cylindrical temperature-gradient specimens were irradiated to characterize their stability with respect to heat transport, lithium transport and physical integrity over the duration of the experiment. Phase I included a solid monolithic specimen of Li{sub 2}O while Phase II included a sphere bed of Li{sub 2}ZrO{sub 3}.
1992-09-01
The BEATRIX-II irradiation experiment was an in situ, fast neutron, tritium release experiment to evaluate the performance of ceramic fusion solid breeders at extended burnups. The experiment consisted of two sequential irradiations: Phase I for 300 EFPD and Phase II for 200 EFPD that resulted in lithium burnups from 4[endash]6%. Thin-walled Li[sub 2]O ring specimens capable of temperature changes were irradiated in both Phase I and Phase II. Temperature changes were also used to determine the tritium inventory and to characterize the effect or irradiation history and sweep gas composition. Solid-cylindrical temperature-gradient specimens were irradiated to characterize their stability with respect to heat transport, lithium transport and physical integrity over the duration of the experiment. Phase I included a solid monolithic specimen of Li[sub 2]O while Phase II included a sphere bed of Li[sub 2]ZrO[sub 3].
Estimation of irradiation temperature within the irradiation program Rheinsberg
The temperature monitoring within the irradiation programme Rheinsberg II was performed by diamond powder monitors. The method bases on the effect of temperature on the irradiation-induced increase of the diamond lattice constant. The method is described by a Russian code. In order to determine the irradiation temperature, the lattice constant is measured by means of a X-ray diffractometer after irradiation and subsequent isochronic annealing. The kink of the linearized temperature-lattice constant curves provides a value for the irradiation temperature. It has to be corrected according to the local neutron flux. The results of the lattice constant measurements show strong scatter. Furthermore there is a systematic error. The results of temperature monitoring by diamond powder are not satisfying. The most probable value lays within 255 C and 265 C and is near the value estimated from the thermal condition of the irradiation experiments.
HST/ACS Ha imaging of the Carina Nebula: outflow activity traced by irradiated Herbig-Haro Jets
2010-01-01
ABSTRACT We report the discovery of new Herbig-Haro (HH) jets in the Carina Nebula, and we discuss the protostellar outflow activity of a young OB association. These are the first results of an Ha imaging survey of Carina conducted with the Hubble Space Telescope (HST)/Advanced Camera for Surveys. Adding to the one previously known example (HH 666), we detect 21 new HH jets, plus 17 new candidate jets, ranging in length from 0.005 to 3 pc. Using the Ha emission measure to estimate jet densities, we derive jet mass-loss rates ranging from 8 x 10 Formula Not Shown to 10 Formula Not Shown M yr-1, but a comparison to the distribution of jet mass-loss rates in Orion suggests that we may be missing a large fraction of the jets below 10 Formula Not Shown M yr-1. A key qualitative result is that e...
Constitutive secretion of chemokines by cultured human trabecular meshwork cells.
Trabecular meshwork endothelial (TME) cells secrete a number of factors, such as enzymes and cytokines, which modulate the functions of the cells and the extracellular matrix of the conventional aqueous outflow pathway. TME cells usually secrete these factors in response to stimuli such as mechanical stretching, laser irradiation and pro-inflammatory cytokines. Here, we report that cultured human TME cells isolated from two non-glaucomatous individuals secrete significant quantities of the chemotactic cytokines IL8, CXCL6 and MCP1 in the absence of any stimulation. The secretion of these chemokines was augmented by treatment with the pro-inflammatory cytokines TNFalpha and IL1beta. By way of comparison, there was little or very low production of the three chemokines by human non-pigmented ciliary epithelial cells in the absence of stimulation. Our findings provide support to our recent observations that monocytes, presumably under the influence of chemotactic signals, circulate through the trabecular meshwork in the normal state and also that cytokines regulate the permeability of Schlemm's canal endothelial cells. In addition, the fact that normal TME cells constitutively secrete chemotactic cytokines strengthens the notion that cytokines play a key role in the homeostasis of the outflow of the aqueous humor and, possibly, in the pathogenesis of glaucoma.
2004-07-01
The effects of low-dose rate gamma-irradiation were investigated on model mice for type II diabetes mellitus, C57BL/KsJ-db/db. The mice develop the type II diabetes by 10 weeks of age due to obesity and are characterized by hyperinsulinemia. Female 10-week old mice, a group of 12 mice, were irradiated at 0.65 mGy/hr from 137-Cs (370 GBq). The urine glucose levels of all of the mice were strongly positive at the beginning of the irradiation. In the irradiated group, the decrease in the glucose level was observed in 3 mice. Such recovery from the diabetes was never observed in 12 mice of non-irradiated control group. There is no systematic difference in the change of body weight, food assumption, and amount of drinking water, between the irradiated group and the non-irradiated group or between the recovered mice and the non-recovered mice. The survival was better in the irradiated group: the surviving fraction at the age of 90 weeks was 75% in the irradiated group, while 40% in the non-irradiated. Marked difference was also observed in the appearance of the coat hair, skin, and tail; better condition was kept in the irradiated group. In the irradiated mice mortality was delayed and the healthy appearance was prolonged in the irradiated mice by about 20 ? 30 weeks compared with the non-irradiated mice. These results suggest that the low-dose irradiation modified the condition of the diabetic mice, which lead not only to the recovery of the diabetes, but also to the suppression of the aging process. (Author)
The morphology of minor axis gaseous outflows in edge-on Seyfert galaxies
Context: Spiral galaxies often have extended outflows that permeate beyond the region of the disk. Such outflows have been seen both in starburst galaxies, actively star forming galaxies and galaxies with an AGN. In the latter galaxies it is unknown whether the large-scale outflows are driven by star formation activity or purely by the active nucleus. Aims: The aim of our investigation is to study the frequency of extended minor-axis outflows in edge-on Seyfert galaxies to investigate the role of the AGN, the circumnuclear environment and star formation activity within the disk regions, and their importance for IGM enrichment on large scales. Methods: We obtained optical narrowband imaging observations of a distance limited, northern hemisphere sample of 14 edge-on Seyfert spiral galaxies. Because of the distance-limited nature of the sample, it is restricted to relatively low-luminosity Seyfert galaxies. The data were obtained with BUSCA attached to the 2.2 m telescope at the Calar Alto observatory. Narrowband imaging in two different ionizational stages (H? and [O iii] ) was performed to attempt a discrimination between processes associated with the active nucleus and those connected to star forming activity within the disk. The median 3-? sensitivities for detection of high-latitude extended emission in the sample galaxies are 3.610-17 erg s-1 cm-2 arcsec-2 for the H? images and 6.910-17 erg s-1 cm-2 arcsec-2 for the [O iii] images. We use the data to study the distribution of extraplanar emission with respect to the AGN and the underlying disk H ii regions. Results: The H? morphology of the Seyfert galaxies is usually complex, but only in three out of 14 galaxies did we find evidence for minor axis disk outflows. At the sensitivity of our observations [O iii] emission is generally detected only in the nuclear region. For Ark 79 we present the first evidence of a secondary nuclear component, best visible in the [O iii] image, which has a linear separation from the primary nucleus of about 850 pc. Conclusions: .Overall, our results show that extraplanar emission of similar brightness and extent as in the previously known cases of NGC 3079 and NGC 4388 is not common in Seyfert galaxies of otherwise similar properties. Comparison with our previous results shows that for nearby edge-on spiral galaxies star formation may be a more powerful mechanism for producing DIG than AGN activity. While in general AGN activity undoubtedly plays some role in driving minor-axis outflows, this probably requires higher AGN luminosities than are encountered in our small distance-limited sample. Based on observations collected at the Centro Astronmico Hispano Alemn (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fr Astronomie and the Instituto de Astrofsica de Andaluca (CSIC). Tables 2, 5 and Figs. 6-24 are only available in electronic form at http://www.aanda.org
Long-Term Evolution of Slowly Rotating Collapsar in Special Relativistic Magnetohydrodynamics
2009-05-14
We present our numerical results of two-dimensional magnetohydrodynamic (MHD) simulations of the collapse of rotating massive stars in light of the collapsar model of gamma-ray bursts (GRBs). Pushed by recent evolution calculations of GRB progenitors, we focus on lower angular momentum of the central core than the ones taken mostly in previous studies. By performing special relativistic simulations including both realistic equation of state and neutrino coolings, we follow a unprecedentedly long-term evolution of the slowly rotating collapsars up to $\\sim$ 10 s, accompanied by the formation of jets and accretion disks. Our results show that for the GRB progenitors to function as collapsars, there is a critical initial angular momentum, below which matter is quickly swallowed to the central objects, no accretion disks and no MHD outflows are formed. When larger than the criteria, we find the launch of the MHD jets in the following two ways. For models with stronger initial magnetic fields, the magnetic pressure amplified inside the accretion disk can drive the MHD outflows, which makes the strong magnetic explosions like a 'magnetic tower' (type II). For the models with weaker initial magnetic fields, the magnetic tower stalls first and the subsequent MHD outflows are produced by some eventual inflows of the accreting material from the equator to the polar regions (type I). Regardless of type I or II, the jets can attain only mi ldly relativistic speeds with the explosion energy less than $10^{49} \\erg$, which could possibly be related to the X-ray flashes. Due to high opacity for neutrinos inside the disk, we find that the luminosities of $\\nu_e$ and $\\bar{\\nu}_e$ become almost comparable, which is advantageous for making the energy deposition rate larger.
Cepheus A East: Unraveling the Mysteries
New infrared images of Cep A East are presented that show two regions of shock-excited line emission from separate bipolar flows. We identify the dominant sources powering the outflows and argue that the results support a multiple outflow model (Narayanan & Walker) as opposed to a quadrupolar outflow scenario. The images include near-infrared broadband (K [2.158 mu m], L" [3.81 mu m], and M' [4.67 mu m]) and spectral line ([Fe II] emission line at 1.644 mu m and H2 1-0 S[1] line at 2.122 mu m) observations, as well as continuum emission, at 1.644 mu m and 2.122 mu m. Considering our data and other results, we present a unified, self-consistent picture of the disk and shock structure. The northern emission region appears to be the result of the ablation of a dense molecular clump (coincident with HW 6) in the path of a diverting jet from YSO HW 2 and subsequent multiple bow shocks with prompt entrainment arising from the interaction of the jet with the molecular cloud Cep A-2. The southern line emission region near HW 7 resembles the "artillery shell" bow shocks found in Orion and is most likely a J-type shock caused by a jet from another YSO, possibly HW 3(d)ii.
2009-01-01
ABSTRACT We present results from modelling of quasi-simultaneous broad-band (radio through X-ray) observations of the Galactic stellar black hole (BH) transient X-ray binary (XRB) systems XTE J1118+480 and GX 339-4 using an irradiated disc + compact jet model. In addition to quantifying the physical properties of the jet, we have developed a new irradiated disc model which also constrains the geometry and temperature of the outer accretion disc by assuming a disc heated by viscous energy release and X-ray irradiation from the inner regions. For the source XTE J1118+480, which has better spectral coverage of the two in optical and near-infrared (OIR) wavelengths, we show that the entire broad-band continuum can be well described by an outflow-dominated model + an irradiated disc. The best-f...
Spatially extended absorption around the z=2.63 radio galaxy MRC 2025-218: outflow or infall?
2008-09-09
We present an investigation into the absorber in front of the z=2.63 radio galaxy MRC 2025-218, using integral field spectroscopy obtained at the Very Large Telescope, and long slit spectroscopy obtained at the Keck II telescope. The properties of MRC 2025-218 are particularly conducive to study the nature of the absorbing gas, i.e., this galaxy shows bright and spatially extended Ly-alpha emission, along with bright continuum emission from the active nucleus. Ly-alpha absorption is detected across ~40x30 kpc^2, has a covering factor of ~1, and shows remarkably little variation in its properties across its entire spatial extent. This absorber is kinematically detached from the extended emission line region (EELR). Its properties suggest that the absorber is outside of the EELR. We derive lower limits to the HI, HII and H column densities for this absorber of 3x10^16, 7x10^17 and 2x10^18 cm^-2, respectively. Moreover, the relatively bright emission from the active nucleus has allowed us to measure a number of metal absorption lines: CI, CII, CIV, NV, OI, SiII, SiIV, AlII and AlIII. The column density ratios are most naturally explained using photoionization by a hard continuum, with an ionization parameter U~0.0005-0.005. Shocks or photoionization by young stars cannot reproduce satisfactorily the measured column ratios. Using the ratio between the SiII* and SiII column densities, we derive a lower limit of >10 cm^-3 for the ele ctron density of the absorber. The data do not allow useful constraints to be placed on the metallicity of the absorber. We consider two possibilities for the nature of this absorber: the cosmological infall of gas, and an outflow driven by supernovae or the radio-jets.
Observations of Mass Loss from the Transiting Exoplanet HD 209458b
2010-05-11
Using the new Cosmic Origins Spectrograph (COS) on the {\\it Hubble Space Telescope (HST)}, we obtained moderate-resolution, high signal/noise ultraviolet spectra of HD 209458 and its exoplanet HD 209458b during transit, both orbital quadratures, and secondary eclipse. We compare transit spectra with spectra obtained at non-transit phases to identify spectral features due to the exoplanet's expanding atmosphere. We find that the mean flux decreased by $7.8\\pm 1.3$\\% for the C~II 1334.5323~\\AA\\ and 1335.6854~\\AA\\ lines and by $8.2\\pm 1.4$\\% for the Si~III 1206.500~\\AA\\ line during transit compared to non-transit times in the velocity interval --50 to +50 km~s$^{-1}$. Comparison of the C~II and Si~III line depths and transit/non-transit line ratios shows deeper absorption features near --10 and +15 km~s$^{-1}$ and less certain features near --40 and +30--70 km~s$^{-1}$, but future observations are needed to verify this first detection of velocity structure in the expanding atmosphere of an exoplanet. Our results for the C~II lines and the non-detection of Si~IV 1394.76~\\AA\\ absorption are in agreement with \\citet{Vidal-Madjar2004}, but we find absorption during transit in the Si~III line contrary to the earlier result. The $8\\pm 1$\\% obscuration of the star during transit is far larger than the 1.5\\% obscuration by the exoplanet's disk. Absorption during transit at velocities between --50 and +50~km~s$^{-1}$ in the C~II and Si~III lines requires high-velocity ion absorbers, but models that assume that the absorbers are high-temperature thermal ions are inconsistent with the COS spectra. Assuming hydrodynamic model values for the gas temperature and outflow velocity at the limb of the outflow as seen in the C~II lines, we find mass-loss rates in the range (8--40)$\\times 10^{10}$ g~s$^{-1}$. Our mass-loss rate estimate is consistent with theoretical hydrodynamic models that include metals in the outflowing gas.
2007-08-23
We compute the structure and degree of neutronization of general relativistic magnetohydrodynamic (GRMHD) outflows originating from the inner region of neutrino-cooled disks. We consider both, outflows expelled from a hydrostatic disk corona and outflows driven by disk turbulence. We show that in outflows driven thermally from a static disk the electron fraction quickly evolves to its equilibrium value which is dominated by neutrino capture. Those outflows are generally proton rich and, under certain conditions, can be magnetically dominated. They may also provide sites for effective production of 56Ni. Centrifugally driven outflows and outflows driven by disk turbulence, on the other hand, can preserve the large in-disk neutron excess. Those outflows are, quite generally, subrelativistic by virtue of the large mass flux driven by the additional forces.
Gamma irradiation of yellow and blue colorants in polystyrene packaging materials
2006-01-15
The effect of 10- and 20-kGy gamma irradiation was studied on chromophtal yellow 2RLTS (Yellow 110-2, 3, 4, 5-tetrachloro-6-cyanobenzoic acid) and Irgalite Blue GBP (copper (II) phthalocyanine blue) colorants, which were added to polystyrene (PS) material used to package food prior to irradiation. Analytical results obtained suggest that irradiation did not generate any new chemicals in the PS polymer containing either yellow or blue colorant at a concentration of up to 1% (w/w). Both yellow and blue colorants are relatively stable to gamma irradiation.
Gamma irradiation of yellow and blue colorants in polystyrene packaging materials
2006-01-01
The effect of 10- and 20-kGy gamma irradiation was studied on chromophtal yellow 2RLTS (Yellow 110-2, 3, 4, 5-tetrachloro-6-cyanobenzoic acid) and Irgalite Blue GBP (copper (II) phthalocyanine blue) colorants, which were added to polystyrene (PS) material used to package food prior to irradiation. Analytical results obtained suggest that irradiation did not generate any new chemicals in the PS polymer containing either yellow or blue colorant at a concentration of up to 1% (w/w). Both yellow and blue colorants are relatively stable to gamma irradiation
1980-10-01
From 1967 to 1979, 40 children with Wilms' tumor were given a therapy comprising irradiation, operation and chemotherapy. Till 1972 preoperative irradiation was performed delivering a dose of 20 Gy followed by operation and actinomycin-D. The postoperative irradiation dose was 20 or 30 Gy. Of 22 patients 7 died. Since 1973, therapy depends on age and tumor volume and consists in a combination of multidrug therapy, operation and irradiation (25 to 35 Gy). Of 19 children, 18 are still alive. No irradiation was given to patients younger than 1 year in stages I and II and to older children in stage I.
2004-01-01
The results of the two-detector coincidence measurements of the doppler broadening of annihilation radiation on a variety of the reactor pressure vessel steels of VVER type are reported. The following subjects were studied: (i) the non-irradiated materials. (ii) the changes induced by neutron irradiation as a function of fluence and flux. (iii) the effect of the regeneration annealing of irradiated materials. The irradiation-induced migration of Cu atoms towards positron annihilation sites in dislocations was observed which turned out to be removed by annealing at 475 C. (orig.)
The loopy UV line profiles of RU Lupi: accretion, outflows, and fluorescence
2005-04-29
We present far-ultraviolet spectra of the classical T Tauri star RU Lupi covering the 912-1710 A spectral range, as observed by the HST/STIS and FUSE satellites. We use these spectra, which are rich in emission and absorption lines, to probe both the accreting and outflowing gas. Absorption in the Ly-alpha profile constrains the extinction to A_V=0.07 mag, which we confirm with other diagnostics. We estimate a mass accretion rate of (5\\pm2)\\times10^{-8}$ M_\\odot/yr using the optical-NUV accretion continuum. The accreting gas is also detected in bright, broad lines of C IV, Si IV, and N V, which all show complex structures across the line profile. Many other emission lines, including those of H_2 and Fe II, are pumped by Ly-alpha. RU Lupi's spectrum varies significantly in the FUV; our STIS observations occurred when RU Lupi was brighter than several other observations in the FUV, possibly due to a high mass accretion rate.
The Revised Version of Class I Methanol Maser Catalog
2010-05-21
The revised version of the class I methanol maser catalog is presented. It contains 182 sources - new class I methanol masers detected in the direction of EGOs were added to the previous number (~160 sources have been published in the first version of this catalog - see reference in the text). Electronic version has been generated in the form of html file - http://www.asc.rssi.ru/MMI. A statistical analysis was carried out within 2' around a maser position to find an identification of class I methanol masers with any objects typical for star-forming regions - UCHII regions, IRAS sources, bipolar outflows, CS lines as of dense gas tracer, masers (class II methanol masers, OH and H2O) and EGO. None of the bipolar outflow, already registered in the direction of class I methanol maser, did not coincide with EGO. The result is submitted in a form of a diagram.
2010-08-06
After the initiation of the explosion of core-collapse supernovae, neutrinos emitted from the nascent neutron star drive a supersonic baryonic outflow. This neutrino-driven wind interacts with the more slowly moving, earlier supernova ejecta forming a wind termination shock (or reverse shock), which changes the local wind conditions and their evolution. Important nucleosynthesis processes (alpha-process, charged-particle reactions, r-process, and vp-process) occur or might occur in this environment. The nucleosynthesis depends on the long-time evolution of density, temperature, and expansion velocity. Here we present two-dimensional hydrodynamical simulations with an approximate description of neutrino-transport effects, which for the first time, follow the post-bounce accretion, onset of the explosion, wind formation, and the wind expansion through the collision with the preceding supernova ejecta. Our results demonstrate a great impact of the anisotropic ejecta distribution on the position of the reverse shock, wind profile, and long-time evolution and show a big effect of multidimensional features on nucleosynthesis-relevant conditions.
2009-01-01
We report the first mid-infrared detection of highly disturbed ionized gas in the ultraluminous infrared galaxy (ULIRG) IRAS F00183-7111. The gas, traced by the 12.81 mum [Ne II] and 15.56 mum [Ne III] lines, spans a velocity range of-3500 to +3000 km s-1 with respect to systemic velocity. Optical and near-infrared spectroscopic studies show no evidence for similarly high velocity gas components in forbidden lines at shorter wavelengths. We interpret this as the result of strong extinction (AV = 10-50) on the high-velocity gas, which identifies the base of the outflow traced in 5007 A [O III] as a plausible origin. Unusual excitation conditions are implied by a comparison of the mid-infrared low-excitation neon line emission and the polycyclic aromatic hydrocarbon (PAH) emission for a sample of 56 ULIRGs. For IRAS ...
Equatorward moving arcs and substorm onset
Key observations of phenomena during the growth phase of a substorm are being reviewed with particular attention to the equatorward motion of the hydrogen and electron arcs. The dynamic role of the electron, the so-called growth phase arc, is analyzed. It is part of a current system of type II that is instrumental in changing the dominantly equatorward convection from the polar cap into a sunward convection along the auroral oval. A quantitative model of the arc and associated current system allows determining the energy required for the flow change. It is suggested that high-? plasma outflow from the central current sheet of the tail creates the current generator. Assessment of the energy supplied in this process proves its sufficiency for driving the arc system. The equatorward motion of the arcs is interpreted as a manifestation of the shrinkage of the near-Earth transition region (NETR) between the dipolar magnetosphere and the highly stretched tail. This shrinkage is caused by returning magnetic flux to the dayside magnetosphere as partial replacement of the flux eroded by frontside reconnection. As the erosion of the NETR is proceeding, more and more magnetic flux is demanded from the central current sheet of the near-Earth tail until highly accelerated plasma outflow causes the current sheet to collapse. Propagation of the collapse along the tail triggers reconnection and initiates the substorm.
A WIDE-FIELD NARROWBAND OPTICAL SURVEY OF THE BRAID NEBULA STAR FORMATION REGION IN CYGNUS OB7
2010-01-01
We study the population of Herbig-Haro (HH) flows and jets in an area of Cygnus OB7 designated the Braid Nebula star formation region. This complex forms part of the L 1003 dark cloud, and hosts two FU Orionis (FUor)-like objects as well as several other active young stars. To trace outflow activity and to relate both known and newly discovered flows to young star hosts we intercompare new, deep, narrowband Halpha and [S II] optical images taken on the Subaru 8 m Telescope on Mauna Kea, Hawaii. Our images show that there is considerable outflow and jet activity in this region suggesting the presence of an extensive young star population. We confirm that both of the FUor-like objects drive extensive HH flows and document further members of the flows in both objects. The L 1003 star formation complex is a highly kinematically active region with young stars in several different ...
High spectral resolution observations of the [N II] 6548 + 6584 A and H alpha emission lines from the young planetary nebula MyCn 18 have been obtained using the Manchester echelle spectrometer combined with the Anglo-Australian Telescope. These spatially resolved spectra reveal not only the kinematical characteristics of the two bright rings of emission, which define the well-known "engraved hourglass" structure of this object, but also the dramatic motions of the faint, irregular knots of emission observed outside the main nebular structure. The knots are moving with velocities >=500 km s-1 away from the central star, an order of magnitude faster than the motions observed from the main nebula, making them among the highest velocity outflows ever observed from a planetary nebula. A bipolar, rotating, episodic jet mechanism is favored for their origin.
Application of fuzzy logic for selection of turbines and weirs in hydro power plants
1999-07-01
A new outflow controller structure for hydro power plants is presented. The outflow control loop is characterized by the fact that for controlling the total reservoir outflow several actuators (turbines and weirs) are available. Based on multicriteria decision making techniques within a fuzzy set framework the outflow controller selects the best actuator and updates the input of the respective local flow controller. The performance of the outflow controller is illustrated in simulation studies. (author)
Photochemical reactions in solutions of the platinum(II) complex with 8-quinolinol
2007-01-01
The rate of photochemical reaction in solutions of luminescent platinum(II) complex with 8-quinolinol was studied in relation to the type of solvent, irradiation time, photon energy and intensity of a luminous flux, concentration of the complex, and presence of oxygen. The structure of the photochemical reaction product was studied by X-ray photoelectron, IR, and electronic absorption spectroscopy. The quantitative kinetic parameters and quantum yield of the photochemical reaction performed under various irradiation conditions are reported.
Neutron flux parameters at irradiation positions in the new research reactor FRM-II
2006-08-15
The new research reactor FRM-II in Garching, Germany, was at full power 20 MW for the first time on 24th August, 2004. Since then, highly thermalized neutrons are available also for neutron activation analysis (NAA). In this report, all essential neutron flux parameters needed to calculate neutron induced reaction rates based on the Hogdahl or Westcott convention are presented for all irradiation positions in this reactor.
Neutron flux parameters at irradiation positions in the new research reactor FRM-II
The new research reactor FRM-II in Garching, Germany, was at full power 20 MW for the first time on 24th August, 2004. Since then, highly thermalized neutrons are available also for neutron activation analysis (NAA). In this report, all essential neutron flux parameters needed to calculate neutron induced reaction rates based on the Hgdahl or Westcott convention are presented for all irradiation positions in this reactor.
Free radical kinetics of irradiated durum wheat
2000-01-01
In the present work, a detailed ESR investigation of characteristic features and kinetic behaviors at three different temperatures of free radicals produced in a species of durum wheat cultivated in Turkey and irradiated at doses of up to 5 kGy by a gamma source, is reported. Unirradiated wheat samples exhibit a weak, single-line ESR signal originating from a radical of unknown structure called radical III in this work. Irradiation produces two more radicals identified as hydroxyalkyl (I) and aldehydalkyl (II) radicals beside radical III. The radicals (I, II and III) follow complicated kinetics. Species I and II initially decay very fast after the irradiation followed by slower decay. Radical half-life times depend on whether they were induced in the crystalline or amorphous fractions of the wheat starch. Activation energy values of the radicals were found to ...
NGC 4102: High Resolution Infrared Observations of a Nuclear Starburst Ring
2010-08-12
The composite galaxy NGC 4102 hosts a LINER nucleus and a starburst. We mapped NGC 4102 in the 12.8 micron line of [NeII], using the echelon spectrometer TEXES on the NASA IRTF, to obtain a data cube with 1.5" spatial and 25 km/s spectral, resolution. Combining near-infrared, radio, and the [NeII] data shows that the extinction to the starburst is substantial, more than 2 magnitudes at K band, and that the neon abundance is less than half solar. We find that the star formation in the nuclear region is confined to a rotating ring or disk of 4.3" (~300 pc) diameter, inside the Inner Lindblad Resonance. This region is an intense concentration of mass, with a dynamical mass of ~3 x 10^9 solar masses, and of star formation. The young stars in the ring produce the [NeII] flux reported by Spitzer for the entire galaxy. The mysterious blue component of line emission detected in the near-infrared is also seen in [NeII]; it is not a normal AGN outflow.
Subtask 12H1: Vanadium alloy irradiation experiment X530 in EBR-II
1995-03-01
The objective of the X530 experiment in EBR-II was to obtain early irradiation performance data, particularly the fracture properties, on the new 500-kg production heat of V-4Cr-4Ti material before the scheduled reactor shutdown at the end of September 1994. To obtain early irradiation performance data on the new 500-kg production heat of the V-4Cr-4Ti material before the scheduled EBR-II shutdown, an experiment, X530, was expeditiously designed and assembled. Charpy, compact tension, tensile and TEM specimens with different thermal mechanical treatments (TMTs), were enclosed in two capsules and irradiated in the last run of EBR-II, Run 170, from August 9 through September 27. For comparison, specimens from some of the previous heats were also included in the test. The accrued exposure was 35 effective full power days, yielding a peak damage of {approx}4 dpa in the specimens. The irradiation is now complete and the vehicle is awaiting to be discharged from EBR-II for postirradiation disassembly. 4 figs., 2 tabs.
1990-08-01
One hundred and ten patients with Stage II epidermoid carcinomas of the mobile tongue were treated by interstitial irradiation (Group I: 85 patients) or external irradiation to the primary and the regional lymphatics followed by an interstitial boost (Group II: 25 patients). The neck was managed by either an elective neck dissection (43 patients) completed by external irradiation in 13 patients with pathological specimen or close follow-up (40 patients) with therapeutic neck dissection for relapses (7 patients) in Group I. Primary local control was 88% in Group I and 36% in Group II. Regional control was 91% in Group I and 5/6 in Group II for patients whose primary tumor was controlled. Five-year absolute disease-free survival (DFS) was 42% in Group I and 24% in Group II, but there was an imbalance in the distribution of larger tumors fovaoring Group I. There were 30 radiation-induced cimplications and four patients required corrective surgery. This retrospective analysis showed better results in patients whose primary was treated by interstitial irradiation alone which has the extra advantage of preserving salivary function. (author). 24 refs.; 8 tabs.
An overview of the EBR-II PRA (Probabilistic Risk Assessment)
1990-01-01
Experimental Breeder Reactor-II, EBR-II, is a 60 MW(t) liquid sodium cooled, pool type fast reactor which has operated successfully as a power reactor and irradiation facility for over 25 years. Argonne National Laboratory is currently performing a Probabilistic Risk Assessment of EBR-II. An overview of the PRA is presented with special attention to those issues which are important to EBR-II such as the passive decay heat removal capabilities and the passive shut down capability provided by the reactivity feedbacks. 7 refs., 3 figs., 1 tab.
Validation results based on the spent fuel demonstration program at FCF
Over the last decade Argonne National Laboratory has developed reactor depletion methods and models to determine radionuclide inventories of irradiated EBR-II fuels. A brief description of these burnup methodologies is presented herein. Predicted masses for the irradiated Zirconium-alloy driver fuel based on these calculational methodologies have been validated using available data from destructive measurements--first from measurements of lead EBR-II experimental test assemblies and later using data obtained from processing irradiated EBR-II fuel assemblies in the Fuel Conditioning Facility. The results of Analytical Laboratory measurements obtained for EBR-II driver fuel samples obtained over the duration of the Spent Fuel Demonstration Program are compared with calculated values. These validation results demonstrate these methods meet the FCF operations and material control and accountancy requirements.
Validation results based on the spent fuel demonstration program at FCF
2000-03-24
Over the last decade Argonne National Laboratory has developed reactor depletion methods and models to determine radionuclide inventories of irradiated EBR-II fuels. A brief description of these burnup methodologies is presented herein. Predicted masses for the irradiated Zirconium-alloy driver fuel based on these calculational methodologies have been validated using available data from destructive measurements--first from measurements of lead EBR-II experimental test assemblies and later using data obtained from processing irradiated EBR-II fuel assemblies in the Fuel Conditioning Facility. The results of Analytical Laboratory measurements obtained for EBR-II driver fuel samples obtained over the duration of the Spent Fuel Demonstration Program are compared with calculated values. These validation results demonstrate these methods meet the FCF operations and material control and accountancy requirements.
1994-04-01
BEATRIX-II, Phase II was an in situ tritium recovery experiment designed to characterize the behavior of lithium ceramics irradiated to high burnup in a fast neutron flux. A thin-walled Li{sub 2}O ring specimen was irradiated at temperatures in the range from 520 to 640 C in helium sweep gases containing 0, 0.01 and 0.1% H{sub 2} to a 5% lithium burnup. The tritium recovery behavior of Li{sub 2}O was characterized by using temperature transients and sweep gas composition changes to effect changes in the tritium inventory.
Comparison of measured and calculated composition of irradiated EBR-II blanket assemblies.
1998-07-13
In anticipation of processing irradiated EBR-II depleted uranium blanket subassemblies in the Fuel Conditioning Facility (FCF) at ANL-West, it has been possible to obtain a limited set of destructive chemical analyses of samples from a single EBR-II blanket subassembly. Comparison of calculated values with these measurements is being used to validate a depletion methodology based on a limited number of generic models of EBR-II to simulate the irradiation history of these subassemblies. Initial comparisons indicate these methods are adequate to meet the operations and material control and accountancy (MC and A) requirements for the FCF, but also indicate several shortcomings which may be corrected or improved.
Radioprotective copper (II) (3,5-diisopropylsalicylate)2 accelerates recovery of immunocompetence
1986-01-01
Copper (II)(3,5-diisopropylsalicate)2 (Cu(II) (3,5-dips)2) afforded significant protection when administered subcutaneously 3 hr before whole body irradiation. At 800 Rad (170 Rad/min) using a cesium-137 irradiator, 86% of mice receiving 80 mg/kg of the copper complex survived while only 40% of irradiated mice receiving only the polyvinyl alcohol vehicle survived. Seven days after irradiation femoral bone marrow cells were depleted by 99.5%. This depletion was evident whether or not mice were treated with Cu(II)(3,5-dips)2. The ability of bone marrow cells from copper-treated mice to respond to colony-stimulating factors in mouse lung-conditioned medium recovered rapidly reaching 70% of control values 24 days after irradiation, while vehicle-treated, irradiated mice reached only 10% of control activity after 24 days. The antibody ...
The mechanism of chondrogenesis inhibition by X-irradiation
2003-01-01
The purpose of this study is to investigate the mechanism of inhibition of chondrogenic differentiation by X-irradiation. Cultures of chick limb bud mesenchymal cells were exposed to various dose of X-ray and chondrogenesis was examined. X-irradiation inhibited accumulation of proteoglycan based on the observation of alcian blue staining and expression of chondorcyte specific-type II collagen. X-irradiation also inhibited expression of protein kinase Ca while expression of PKClambda(iota, epsilon was not altered. Expression of Erk-1 was not changed by X-irradiation but phosphorylation of Erk-1 was increased. In addition, inhibition of Erk-1 phosphorylation by PD98059 overcame inhibitory effect of X-irradiation on the chondrogenic differentiation. PNA staining data showed that X-irradiation inhibited cellular ...
Node-positive cervical cancer: impact of pelvic irradiation and patterns of failure
1995-01-01
Purpose: The roles of postoperative pelvic and prophylactic paraaortic irradiation in pelvic node positive cervical cancer are currently controversial. A retrospective study was undertaken to examine the effect of pelvic irradiation on pelvic control and survival and to analyze the patterns of recurrence to determine whether indications exist for prophylactic paraaortic irradiation. Methods and Materials: From 1964 to 1991, 143 cases of FIGO Stage I and II cervical cancer undergoing exploratory laparotomy, pelvic lymph node dissection, and radical hysterectomy had positive pelvic lymph nodes. Postoperatively, 108 cases were treated with whole pelvic irradiation while 35 patients were observed. Prophylactic paraaortic irradiation was not given. Results: Patients who received postoperative whole pelvic irradiation compared with those treated with radical ...
2008-11-11
The startling discovery of Prochter and Prochaska (2006) that the frequency of very strong (W_r(2796)>1 A) MgII absorbers along gamma-ray burst (GRB) lines of sight ([dN/dz]_{GRB} = 0.90) is more than three times the frequency along quasar lines of sight ([dN/dz]_{QSO} = 0.24), over similar redshift ranges, has yet to be understood.We reconsider the possibility that the excess of very strong MgII absorbers toward GRBs is intrinsic either to the GRBs themselves or to their immediate environment, and associated with bulk outflows with velocities as large as v_{max} ~ 0.3c. In order to examine this hypothesis, we accumulate a sample of 27 W_r(2796) > 1 A absorption systems found toward 81 quasars, and compare their properties to those of 9 W_r(2796)>1 A absorption systems found toward 6 GRBs; all systems have been observed at high spectral resolution (R = 45,000) using the Ultraviolet and Visual Echelle Spectrograph on the Very Large Telescope. We make multiple comparisons of the absorber properties across the two populations, testing for differences in metallicity, ionization state, abundance patterns, dust abundance, kinematics, and phase structure. We find no significant differences between the two absorber populations using any of these metrics, implying that, if the excess absorbers toward GRB lines of sight are indeed intrinsic, they must be produced in a process which has strong similarities to the processes yielding strong MgII systems in association with intervening galaxies. Although this may seem a priori unlikely, given the high outflow velocities required for any intrinsic model, we note that the same conclusion was reached, recently, with respect to the narrow absorption line systems seen in some quasars.
Diffuse Far-UV Line Emission from the Low-Redshift Lyman Break Galaxy Analog KISSR242
2010-09-10
We present new ultraviolet (UV) observations of the luminous compact blue galaxy KISSR242, obtained with the HST-COS. We identify multiple resolved sub-arcsecond near-UV sources within the COS aperture. The far-UV spectroscopic data show strong outflow absorption lines, consistent with feedback processes related to an episode of massive star-formation. OI, CII, and SiII--SiIV are observed with a mean outflow velocity v_{out} = -60 km/s. We also detect faint fine-structure emission lines of singly ionized silicon for the first time in a low-redshift starburst galaxy. These emissions have been seen previously in deep Lyman break galaxy surveys at z ~ 3. The SiII* lines are at the galaxy rest velocity, and they exhibit a quantitatively different line profile from the absorption features. These lines have a width of ~ 75 km/s, too broad for point-like emission sources such as the HII regions surrounding individual star clusters. The size of the SiII* emitting region is estimated to be ~ 250 pc. We discuss the possibility of this emission arising in overlapping super star cluster HII regions, but find this explanation to be unlikely in light of existing far-UV observations of local star-forming galaxies. We suggest that the observed SiII* emission originates in a diffuse warm halo populated by interstellar gas driven out by intense star-formation and/or accreted during a recent interaction that may be fueling the present starburst e pisode in KISSR242.
A Kennicutt-Schmidt Law for Intervening Absorption Line Systems
2010-08-18
We argue that most strong intervening metal absorption line systems, where the rest equivalent width of the MgII 2796A line is >0.5A, are interstellar material in, and outflowing from, star-forming disks. We show that a version of the Kennicutt-Schmidt law is readily obtained if the MgII equivalent widths are interpreted as kinematic broadening from absorbing gas in outflowing winds originating from star-forming galaxies. Taking a phenomenological approach and using a set of observational constraints available for star-forming galaxies, we are able to account for the density distribution of strong MgII absorbers over cosmic time. The association of intervening material with star-forming disks naturally explains the metallicity and dust content of strong MgII systems as well as their high HI column densities, and does not require the advection of metals from compact star-forming regions into the galaxy halos to account for the observations. We find that galaxies with a broad range of luminosities can give rise to absorption of a given rest-equivalent width, and discuss possible observational strategies to better quantify true galaxy-absorber associations and further test our model. We show that the redshift evolution in the density of absorbers closely tracks the star formation history of the universe and that strong intervening systems can be used to directly probe the physics of both bright and faint galaxies over a broad reds hift range. By identifying strong intervening systems with galaxy disks and quantifying a version of the Kennicutt-Schmidt law that applies to them, a new probe of the interstellar medium is found which provides complementary information to that obtained through emission studies of galaxies. Implications of our results for galaxy feedback and enrichment of the intergalactic medium are discussed. [abridged]
Strength and ductility of austenitic stainless steels irradiated in various fast reactor spectra
1980-01-01
A systematic investigation of radiation damage in various fast reactor spectra was conducted to support verification of damage correlation parameters for improved predictions in the soft spectrum regime. The Experimental Breeder Reactor II (EBR-II) irradiation experiment consisted of four capsules containing identical groups of austenitic stainless steel specimens, each of which was irradiated to a different fluence level. Different spectra were obtained by positioning specimens at four axial locations in each capsule. Specimen irradiation temperatures were low (644-699 K) such that displacement of atoms was expected to be the dominant damage mechanism. Strength and ductility properties, measured in conventional tension tests, were selected to monitor radiation damage. Results from specimens irradiated in the first three capsules are reported here. ...
Radiation imposed limits on superconducting magnets: A data base for copper stabilizers
1987-01-01
Two of eight differently prepared copper stabilizer samples, previously irradiated in the RTNS-II at LLNL, the IPNS-1 and the BSR at ORNL, have been irradiated to a fluence of 1.33 /times/ 1022 n/m2 at RTNS-II. During the course of the irradiation the samples were periodically removed (without warming) for measurements of the transverse magnetoresistance and returned for continued irradiation. This experiment extends the range of neutron-irradiation-induced resistivity by a factor of five over the previous experiments. A simple model is developed which reproduces the magnetoresistance results of all the experiments to an accuracy of 2.5%. 13 refs., 6 figs
Radiation imposed limits on superconducting magnets: A data base for copper stabilizers
1988-01-01
Two of eight differently prepared copper stabilizer samples, previously irradiated in the RTNS-II at LLNL, the IPNS-1 at ANL, and the BSR at ORNL, have been irradiated to a fluence of 1.33x1022 n/m2 at RTNS-II. During the course of the irradiation the samples were periodically removed (without warming) for measurements of the transverse magnetoresistance and returned for continued irradiation. This experiment extends the range of neutron-irradiation-induced resistivity by a factor of five over the previous experiments. A simple model is developed which reproduces the magnetoresistance results of all the experiments to an accuracy of 2.5%. (orig.)
Radiation effects limits on superconducting magnets: data base for copper stabilizers
1986-01-01
The objective of this work is to quantify the changes which occur in the magnetoresistivity of coppers (having various purities and pretreatments) at fields up to 12T during the course of sequential neutron irradiations at 4K and anneals to room temperature. In conjunction with work by Klabunde and Coltman at ORNL, the results should lead to engineering design data for the stabilizers of superconducting magnets in fusion reactors. These magnets are expected to be irradiated during reactor operation and warmed to room temperature periodically during maintenance. Two of eight differently prepared copper stabilizer samples, previously irradiated in the RTNS-II at LLNL, the IPNS-1 at ANL, and the BSR at ONRL, have been irradiated to a fluence of 1.33 x 1022 n/m2 at RNTS-II. During the course of the irradiation the samples were periodically removed ...
Fusion materials irradiations in reactors, T(d,n), and Be(d,n) neutron sources currently require accurate flux and spectral measurements to characterize the irradiation in terms of displacement damage and gas production. The multiple-foil activation technique is described with emphasis on routinely obtainable accuracy as well as the most outstanding problems and nuclear data needs.
1979-01-01
Fusion materials irradiations in reactors, T(d,n), and Be(d,n) neutron sources currently require accurate flux and spectral measurements to characterize the irradiation in terms of displacement damage and gas production. The multiple-foil activation technique is described with emphasis on routinely obtainable accuracy as well as the most outstanding problems and nuclear data needs.
EFFECTS OF SUBLETHAL RADIATION DOSES ON THE CYCLE AND ESTRUS OF WHITE LABORATORY MICE. PART II
Investigations concerning duration of the estrous cycle of the white laboratory mouse after 200 r total body x-ray irradiation showed that no discernible changes in the duration of the estrous cycle could be observed if mature animals were irradiated. Prolonged cycles were observed in those mature female mice that were irradiated with 200 r in utero at the 15th day of pregnancy. (auth)
Effects of gamma irradiation on cobalt hexacyanoferrate(II) ion exchangers
1994-03-01
Study was made of the effects of [gamma] irradiation doses of 2.1 and 5.0 MGy on the structure and cesium ion exchange properties of potassium cobalt hexacyanoferrate(II) and a composite ion exchanger, sodium cobalt hexacyanoferrate(II) in a chelating ion exchange resin. In the case of the potassium cobalt hexacyanoferrate only a slight increase in crystal size was observed. The composite exchanger withstood the lower dose, but at the higher dose the organic resin decomposed, leaving a residue of sodium cobalt hexacyanoferrate. (author).
In order to determine the presence of HLA antigens on human uveal melanomas, we tested anti-HLA monoclonal antibodies on tissue sections of these tumors. A great variety in expression of HLA class I and II antigens was present. A significantly lower expression of HLA class II antigens was present on uveal melanomas that had been irradiated before enucleation. These tumors lacked a lymphocytic infiltrate in comparison with nonirradiated tumors. These data suggest that radiotherapy affects expression of histocompatibility antigens on tumors.
1988-01-15
In order to determine the presence of HLA antigens on human uveal melanomas, we tested anti-HLA monoclonal antibodies on tissue sections of these tumors. A great variety in expression of HLA class I and II antigens was present. A significantly lower expression of HLA class II antigens was present on uveal melanomas that had been irradiated before enucleation. These tumors lacked a lymphocytic infiltrate in comparison with nonirradiated tumors. These data suggest that radiotherapy affects expression of histocompatibility antigens on tumors.
Time-Dependent Models of Accretion Disks Formed from Compact Object Mergers
2008-05-30
We present time-dependent models of the accretion disks created during compact object mergers, focusing on the energy available from accretion at late times and the composition of the disk and its outflows. We calculate the dynamics near the outer edge of the disk, which contains the majority of the mass and sets the accretion rate onto the central black hole. This allows us to follow the evolution over much longer timescales than current hydrodynamic simulations. At late times the disk becomes advective and its properties asymptote to self-similar solutions with accretion rate dM/dt ~ t^(-4/3) (neglecting outflows). This late-time accretion can in principle provide sufficient energy to power the late-time activity observed from some short-duration gamma-ray bursts (GRBs). However, because outflows during the advective phase unbind the majority of the remaining mass, it is difficult for the remnant disk alone to produce significant accretion power well beyond the onset of the advective phase. Unless the viscosity is quite low (alpha ~1e-3), this occurs before the start of observed flaring at ~ 30 s; continued mass inflow thus appears required to explain the late-time activity from short GRBs. We show that the composition of the disk freezes-out relatively neutron-rich (electron fraction Ye ~ 0.3). Roughly 1e-2 Msun of this neutron-rich material is ejected by winds at late times. During earlier, neutrino-cooled phases of accreti on, neutrino irradiation of the disk produces a wind with Ye ~ 0.5, which synthesizes at most ~ 1e-3 Msun of Ni56. We highlight what conditions are favorable for Ni56 production and predict, in the best cases, optical and infrared transients peaking ~ 0.5-2 days after the burst, with fluxes a factor of ~ 10 below the current observational limits.
2010-06-18
We perform multi-dimensional radiative transfer simulations to compute spectra for a hydrodynamical simulation of a line-driven accretion disk wind from an active galactic nucleus. The synthetic spectra confirm expectations from parameterized models that a disk wind can imprint a wide variety of spectroscopic signatures including narrow absorption lines, broad emission lines and a Compton hump. The formation of these features is complex with contributions originating from many of the different structures present in the hydrodynamical simulation. In particular, spectral features are shaped both by gas in a successfully launched outflow and in complex flows where material is lifted out of the disk plane but ultimately falls back. We also confirm that the strong Fe Kalpha line can develop a weak, red-skewed line wing as a result of Compton scattering in the outflow. In addition, we demonstrate that X-ray radiation scattered and reprocessed in the flow has a pivotal part in both the spectrum formation and determining the ionization conditions in the wind. We find that scattered radiation is rather effective in ionizing gas which is shielded from direct irradiation from the central source. This effect likely makes the successful launching of a massive disk wind somewhat more challenging and should be considered in future wind simulations.
The Temperature Dependence of Solar Active Region Outflows
2010-08-17
Spectroscopic observations with the EUV Imaging Spectrometer (EIS) on Hinode have revealed large areas of high speed outflows at the periphery of many solar active regions. These outflows are of interest because they may connect to the heliosphere and contribute to the solar wind. In this Letter we use slit rasters from EIS in combination with narrow band slot imaging to study the temperature dependence of an active region outflow and show that it is more complicated than previously thought. Outflows are observed primarily in emission lines from Fe XI - Fe XV. Observations at lower temperatures (Si VII), in contrast, show bright fan-like structures that are dominated by downflows. The morphology of the outflows is also different than that of the fans. This suggests that the fan loops, which often show apparent outflows in imaging data, are contained on closed field lines and are not directly related to the active region outflows.
Multiple Component Outflows in an Active Region Observed with the EUV Imaging Spectrometer on Hinode
2010-04-29
We have used the Extreme Ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft to observe large areas of outflow near an active region. These outflows are seen to persist for at least 6 days. The emission line profiles suggest that the outflow region is composed of multiple outflowing components, Doppler-shifted with respect to each other. We have modeled this scenario by imposing a double-Gaussian fit to the line profiles. These fits represent the profile markedly better than a single Gaussian fit for Fe XII and XIII emission lines. For the fastest outflowing components, we find velocities as high as 200 km/s. However, there remains a correlation between the fitted line velocities and widths, suggesting that the outflows are not fully resolved by the double-Gaussian fit and that the outflow may be comprised of further components.
Estimate of total reflectance from the Orinoco River outflow
The Orinoco River Delta was photographed by Apollo astronauts. The photographs show discrete water color zones that reflect the mixing of the sediment laden Orinoco outflow with the water of the tropical ...
2007-09-04
CONTEXT: The chemistry in the inner few thousand AU of accreting envelopes around young stellar objects is predicted to vary greatly with far-UV and X-ray irradiation by the central star. Aim We search for molecular tracers of high-energy irradiation by the protostar in the hot inner envelope. METHODS: The Submillimeter Array (SMA) has observed the high-mass star forming region AFGL 2591 in lines of CS, SO, HCN, HCN(v2=1), and HC15N with 0.6" resolution at 350 GHz probing radial scales of 600-3500 AU for an assumed distance of 1 kpc. The SMA observations are compared with the predictions of a chemical model fitted to previous single-dish observations. RESULTS: The CS and SO main peaks are extended in space at the FWHM level, as predicted in the model assuming protostellar X-rays. However, the main peak sizes are found smaller than modeled by nearly a factor of 2. On the other hand, the lines of CS, HCN, and HC15N, but not SO and HCN(v2=1), show pedestal emissions at radii of about 3500 AU that are not predicted. All lines except SO show a secondary peak within the approaching outflow cone. A dip or null in the visibilities caused by a sharp decrease in abundance with increasing radius is not observed in CS and only tentatively in SO. CONCLUSIONS: The emission of protostellar X-rays is supported by the good fit of the modeled SO and CS amplitude visibilities including an extended main peak in CS. The broad pedestals can be inter preted by far-UV irradiation in a spherically non-symmetric geometry, possibly comprising outflow walls on scales of 3500 -- 7000 AU. The extended CS and SO main peaks suggest sulfur evaporation near the 100 K temperature radius.
The Water Vapor Abundance in Orion KL Outflows
2006-08-16
We present the detection and modeling of more than 70 far-IR pure rotational lines of water vapor, including the 18O and 17O isotopologues, towards Orion KL. Observations were performed with the Long Wavelength Spectrometer Fabry-Perot (LWS/FP; R~6800-9700) on board the Infrared Space Observatory (ISO) between ~43 and ~197 um. The water line profiles evolve from P-Cygni type profiles (even for the H2O18 lines) to pure emission at wavelengths above ~100 um. We find that most of the water emission/absorption arises from an extended flow of gas expanding at 25+-5 kms^-1. Non-local radiative transfer models show that much of the water excitation and line profile formation is driven by the dust continuum emission. The derived beam averaged water abundance is 2-3x10^-5. The inferred gas temperature Tk=80-100 K suggests that: (i) water could have been formed in the "plateau" by gas phase neutral-neutral reactions with activation barriers if the gas was previously heated (e.g. by shocks) to >500 K and/or (ii) H2O formation in the outflow is dominated by in-situ evaporation of grain water-ice mantles and/or (iii) H2O was formed in the innermost and warmer regions (e.g. the hot core) and was swept up in ~1000 yr, the dynamical timescale of the outflow.
The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. III. Perseus Observed with IRAC
2006-03-21
We present observations of 3.86 sq. deg. of the Perseus molecular cloud complex with the Spitzer Space Telescope Infrared Array Camera (IRAC). The maps show strong extended emission arising from shocked H2 in outflows in the region and from polycyclic aromatic hydrocarbon features. More than 120,000 sources are extracted toward the cloud. Based on their IRAC colors and comparison to off-cloud and extragalactic fields, we identify 400 candidate young stellar objects. About two thirds of these are associated with the young clusters IC348 and NGC1333, while the last third is distributed over the remaining cloud. We classify the young stellar objects according to the traditional scheme based on the slope of their spectral energy distributions. Significant differences are found for the numbers of embedded Class I objects relative to more evolved Class II objects in IC348, NGC1333 and the remaining cloud with the embedded Class I and "flat spectrum" YSOs constituting 14%, 36% and 47% of the total number of YSOs identified in each of these regions. The high number of Class I objects in the extended cloud (61% of the Class I objects in the entire cloud) suggests that a significant fraction of the current star formation is occuring outside the two main clusters. Finally we discuss a number of outflows and identify their driving sources, including the known deeply embedded Class 0 sources outside the two major clusters. The Class 0 objects are found to be detected by Spitzer and have very red [3.6]-[4.5] colors but do not show similarly red [5.8]-[8.0] colors. The Class 0 objects are easily identifiable in color-color diagrams plotting these two colors but are problematic to extract automatically due to the extended emission from shocked gas or scattered light in cavities related to the associated outflows.
The 2008 outburst in the young stellar system Z CMa: the first detection of twin jets
2010-01-01
The Z CMa binary is understood to undergo both FU Orionis (FUOR) and EX Orionis (EXOR) type outbursts. While the SE component has been spectroscopically classified as an FUOR, the NW component, a Herbig Be star, is the source of the EXOR outbursts. The system has been identified as the source of a large outflow; however, previous studies have failed to identify the driver. Here, we present adaptive optics assisted [Fe II ] spectro-images which reveal for the first time the presence of two small-scale jets. Observations made using OSIRIS at the Keck Observatory show the Herbig Be star to be the source of the parsec-scale outflow, which within 2" of the source shows signs of wiggling and the FUOR to be driving a ~0"4 jet. The wiggling of the Herbig Be star's jet is evidence for an additional companion which could in fact be generating the EXOR outbursts, the last of which began in 2008. Indeed, the dynamical scale of the wiggling corresponds to a timescale of 4-8 years which is in agreement with the timescale of these outbursts. The spectro-images also show a bow-shock-shaped feature and possible associated knots. The origin of this structure is as of yet unclear. Finally, interesting low velocity structure is also observed. One possibility is that it originates in a wide-angle outflow launched from a circumbinary disk. Publisher: Institute of Physics Publishing Contributor: Swinburne University of Technology. Faculty of Information and Communication Technologies. Centre for Astrophysics and Supercomputing Other identifier: swin:18753 Language: English Source: Astrophysical Journal Letters, Vol. 720, no. 1 (Sep 2010), p. L119 Rights: Copyright © 2010 The American Astronomical Society. All rights reserved. The American Astronomical Society does not allow institutions to archive either the accepted manuscript or the published version of the article. However, you can find an earlier version of the full text here: http://arxiv.org/abs/1008.0111.
The 2008 Outburst in the Young Stellar System Z CMa: The First Detection of Twin Jets
2010-08-03
The Z CMa binary is understood to undergo both FU Orionis (FUOR) and EX Orionis (EXOR) type outbursts. While the SE component has been spectro- scopically identified as an FUOR, the NW component, a Herbig Be star, is the source of the EXOR outbursts. The system has been identified as the source of a large outflow, however, previous studies have failed to identify the driver. Here we present adaptive optics (AO) assisted [FeII] spectro-images which reveal for the first time the presence of two jets. Observations made using OSIRIS at the Keck Observatory show the Herbig Be star to be the source of the parsec-scale outflow, which within 2'' of the source shows signs of wiggling and the FUOR to '' be driving a ~ 0.4 jet. The wiggling of the Herbig Be star's jet is evidence for an additional companion which could in fact be generating the EXOR outbursts, the last of which began in 2008 (Grankin & Artemenko 2009). Indeed the dy- namical scale of the wiggling corresponds to a time-scale of 4-8 years which is in agreement with the time-scale of these outbursts. The spectro-images also show a bow-shock shaped feature and possible associated knots. The origin of this structure is as of yet unclear. Finally interesting low velocity structure is also observed. One possibility is that it originates in a wide-angle outflow launched from a circumbinary disk.
1988-12-15
During a period starting in 1983 and ending in April 1984 radionuclide ventriculography was performed in 26 patients subjected to surgical correction of Fallot's tetralogy after having reached adulthood. They were divided into two groups according to the surgical methods used. Patients showing no right-ventricular outflow patch were assigned to group I, while group II was made up of individuals that had received outflow tract patches of Dacron or Teflon for pressure reduction in the right ventricle. The parameters registered during radionuclide ventriculography, in which the tracer substance TC 99m was administered into a peripheral vein, included the endiastolic volume, endsystolic volume, stroke volume, global ejection fraction and cardiac index. For resting patients, these values were calculated using the first-pass technique, the determinations during exercise on the ergometer were based on equilibrium radionuclide ventriculography. It could be concluded from the results obtained here that non-invasive endocardial scintigraphy is a sensitive method that can be used both at rest and during exercise on the ergometer to detect function disorders of the right and left ventricles. (orig./MG).
On the exclusion of intra-cluster plasma from AGN-blown bubbles
2010-01-12
Simple arguments suggest that magnetic fields should be aligned tangentially to the surface of an AGN-blown bubble. If this is the case, charged particles from the fully ionised intra-cluster medium (ICM) will be prevented, ordinarily, from crossing the boundary by the Lorentz force. However, recent observations indicate that thermal material may occupy up to 50% of the volume of some bubbles. Given the effect of the Lorentz force, the thermal content must then be attributed to one, or a combination, of the following processes: i) the entrainment of thermal gas into the AGN outflow that inflated the bubble; ii) rapid diffusion across the magnetic field lines at the ICM/bubble interface; iii) magnetic reconnection events which transfer thermal material across the ICM/bubble boundary. Unless the AGN outflow behaves as a magnetic tower jet, entrainment may be significant and could explain the observed thermal content of bubbles. Alternatively, the cross-field diffusion coefficient required for the ICM to fill a typical bubble is roughly 10^16 cm^2 s^-1, which is anomalously high compared to predictions from turbulent diffusion models. Finally, the mass transfer rate due to magnetic reconnection is uncertain, but significant for plausible reconnection rates. We conclude that entrainment into the outflow and mass transfer due to magnetic reconnection events are probably the most significant sources of thermal content in AGN-blown bu bbles.
Observations of spatial and velocity structure in the Orion Molecular Cloud
2005-11-08
Observations are reported of H2 IR emission in the S(1) v=1-0 line at 2.121 microns in the Orion Molecular Cloud, OMC1, using the GriF instrument on the Canada-France-Hawaii Telescope. GriF is a combination of adaptive optics and Fabry-Perot interferometry, yielding a spatial resolution of 0.15" to 0.18" and a velocity discrimination as high as 1 km/s. Thanks to the high spatial and velocity resolution of the GriF data, 193 bright H2 emission regions can be identified in OMC1. The general characteristics of these features are described in terms of radial velocities, brightness and spatial displacement of maxima of velocity and brightness, the latter to yield the orientation of flows in the plane of the sky. Strong spatial correlation between velocity and bright H2 emission is found and serves to identify many features as shocks. Important results are: (i) velocities of the excited gas illustrate the presence of a zone to the south of BN-IRc2 and Peak 1, and the west of Peak 2, where there is a powerful blue-shifted outflow with an average velocity of -18 km/s. This is shown to be the NIR counterpart of an outflow identified in the radio from source I, a very young O-star. (ii) There is a band of weak velocity features (<5 km/s) in Peak 1 which may share a common origin through an explosive event, in the BN-IRc2 region, with the fast-moving fingers (or bullets) to the NW of OMC1. (iii) A proportion of the flows are likely to represent sites of low mass star formation and several regions show multiple outflows, probably indicative of multiple star formation within OMC1. The high spatial and velocity resolution of the GriF data show these and other features in more detail than has previously been possible.
A precise understanding of neural circuits controlling lipid mobilization and thermogenesis remains to be determined. We have been studying the sympathetic nervous system (SNS) contributions to white adipose tissue (WAT) lipolysis largely in Siberian hamsters. Central melanocortins are implicated in the control of the sympathetic outflow to WAT, and, moreover, the melanocortin 4 receptors (MC4-R) appear to be principally involved. We previously found that acute third ventricular melanotan II (MTII; an MC3/4-R agonist) injections increase sympathetic drive (norepinephrine turnover) to interscapular brown adipose tissue (IBAT) and IBAT temperature. Here we tested whether MC4-R mRNA is expressed in IBAT SNS outflow neurons using in situ hybridization for the former and injections of the transneuronal viral retrograde tract tracer, pseudorabies virus (PRV) into IBAT, for the latter. Significant numbers of double-labeled cells for PRV and MC4-R mRNA were found across the neuroaxis (mean of all brain sites ∼60%), including the hypothalamic paraventricular nucleus (PVH; ∼80%). Acute parenchymal MTII microinjections into the PVH of awake, freely-moving hamsters, using doses below those able to increase IBAT temperature when injected into the third ventricle, increased IBAT temperature for as long as 4 h, as measured by temperature transponders implanted below the tissue. Collectively, these data add significant support to the view that central melanocortins are important in controlling IBAT thermogenesis via the SNS innervation of this tissue, likely through the MC4-Rs.
2009-10-15
Results of the long-term (11 years, from 1996 to 2006) H$\\alpha$ and H$\\beta$ line variations of the active galactic nucleus of NGC 4151 are presented. High quality spectra (S/N>50 and R~8A) of H$\\alpha$ and H$\\beta$ were investigated. We analyzed line profile variations during monitoring period. Comparing the line profiles of H$\\alpha$ and H$\\beta$, we studied different details (bumps, absorption features) in the line profiles. The variations of the different H$\\alpha$ and H$\\beta$ line profile segments have been investigated. Also, we analyzed the Balmer decrement for whole line and for line segments. We found that the line profiles were strongly changing during the monitoring period, showing blue and red asymmetries. This indicates a complex BLR geometry of NGC 4151 with, at least, three kinematically distinct regions: one that contributes to the blue line wing, one to the line core and one to the red line wing. Such variation can be caused by an accelerating outflow starting very close to the black hole, where the red part may come from the region { closer to the black hole than the blue part, which is coming} from the region having the highest outflow velocities. Taking into account the fact that the BLR of NGC 4151 has a complex geometry (probably affected by an outflow) and that a portion of the broad line emission seems to have not a pure photoionization origin, one can ask the question whether the study of the BLR by r everberation mapping may be valid in the case of this galaxy.
Hydrodynamics and stability of galactic cooling flows
Using numerical techniques we studied the global stability of cooling flows in giant elliptical galaxies. As an initial equilibrium state we choose the hydrostatic gas recycling model (Kritsuk 1996). Non-equilibrium radiative cooling, stellar mass loss, heating by type Ia supernovae, distributed mass deposition, and thermal conductivity are included. Although the recycling model reproduces the basic X-ray observables, it appears to be unstable with respect to the development of inflow or outflow. In spherically symmetry the inflows are subject to a central cooling catastrophe, while the outflows saturate in a form of a subsonic galactic wind. Two-dimensional axisymmetric random velocity perturbations of the equilibrium model trigger the onset of a cooling catastrophe, which develops in an essentially non-spherical way. The simulations show a patchy pattern of mass deposition and the formation of hollow gas jets, which penetrate through the outflow down to the galaxy core. The X-ray observables of such a hybrid gas flow mimic those of the equilibrium recycling model, but the gas temperature exhibits a central depression. The mass deposition rate M_dot consists of two contributions of similar size: (i) a hydrostatic one resembling that of the equilibrium model, and (ii) a dynamical one which is related to the jets and is more concentrated to the centre. For a model galaxy, like NGC 4472, our 2D simulations predict M_dot = 2 M_sun/yr within the cooling radius for the advanced non-linear stage of the instability. We discuss the implications of these results to H_alpha nebulae and star formation in cooling flow galaxies and emphasize the need for high-resolution 3D simulations.
Feeding versus Feedback in NGC4151 probed with Gemini NIFS. II. Kinematics
2009-11-12
We have used the Gemini NIFS to map the gas kinematics of the inner 200x500pc of the Seyfert galaxy NGC4151 in the Z, J, H and K bands at a resolving power 5000 and spatial resolution of 8pc. The ionised gas emission is most extended along the known ionisation bi-cone at position angle PA=60-240deg, but is observed also along its equatorial plane. This indicates that the AGN ionizes gas beyond the borders of the bi-cone, within a sphere with 1arcsec radius around the nucleus. The ionised gas has three kinematic components: (1) one observed at the systemic velocity and interpreted as originating in the galaxy disk; (2) one outflowing along the bi-cone, with line-of-sight velocities between -600 and 600 km/s and strongest emission at +/-(100-300)km/s; (3) and another component due to the interaction of the radio jet with ambient gas. The mass outflow rate, estimated to be 1 M_Sun/yr along each cone, exceeds the inferred black hole accretion rate by a factor of 100. There is no evidence in our data for the gradual acceleration followed by gradual deceleration proposed by previous modelling of the [OIII] emitting gas. The molecular gas exhiibits distinct kinematics relative to the ionised gas. Its emission arises in extended regions approximately perpendicular to the axis of the bi-cone and along the axis of the galaxy's stellar bar, avoiding the innermost ionised regions. It does not show an outflowing component, being observed on ly at velocities very close to systemic, and is thus consistent with an origin in the galaxy plane. This hot molecular gas may only be the tracer of a larger reservoir of colder gas which represents the AGN feeding.
Acceleration and Substructure Constraints in a Quasar Outflow
2007-05-01
We present observations of probable line-of-sight acceleration of a broad absorption trough of C IV in the quasar SDSS J024221.87+004912.6. We also discuss how the velocity overlap of two other outflowing systems in the same object constrains the properties of the outflows. The Si IV doublet in each system has one unblended transition and one transition which overlaps with absorption from the other system. The residual flux in the overlapping trough is well fit by the product of the residual fluxes in the unblended troughs. For these optically thick systems to yield such a result, at least one of them must consist of individual subunits rather than being a single structure with velocity-dependent coverage of the source. If these subunits are identical, opaque, spherical clouds, we estimate the cloud radius to be r = 3.9 10^15 cm. If they are identical, opaque, linear filaments, we estimate their width to be w = 6.5 10^14 cm. These subunits are observed to cover the Mg II broad emission line region of the quasar, at which distance from the black hole the above filament width is equal to the predicted scale height of the outer atmosphere of a thin accretion disk. Insofar as that scale height is a natural size scale for structures originating in an accretion disk, these observations are evidence that the accretion disk can be a source of quasar absorption systems. Based on data from ESO program 075.B-0190(A).
Ion-induced spike effects on metal surfaces.
1999-01-01
The effects of single Xe ion impacts on the surfaces of Au, Ag, In and Pb have been studied using in-situ transmission electron microscopy. Individual ion impacts produce surface craters with associated expelled material. The cratering efficiency scales with the density of the irradiated metal. Calculation indicates that, when collision cascades occur near surfaces (within about 5 nm) with energy densities sufficient to cause local melting, craters will occur. Crater formation occurs as a result of the explosive outflow of material from the hot molten core of the cascade. This would appear to indicate that, although the number of atoms in a spike is small and its duration short, it is reasonable to use macroscopic concepts such as vibrational temperature, melting and flow to describe spike effects.
2010-05-06
Gas-phase complex organic molecules have been detected toward a range of high- and low-mass star-forming regions at abundances which cannot be explained by any known gas-phase chemistry. Recent laboratory experiments show that UV irradiation of CH3OH-rich ices may be an important mechanism for producing complex molecules and releasing them into the gas-phase. To test this ice formation scenario we mapped the B1-b dust core and nearby protostar in CH3OH gas using the IRAM 30m telescope to identify locations of efficient non-thermal ice desorption. We find three CH3OH abundance peaks tracing two outflows and a quiescent region on the side of the core facing the protostar. The CH3OH gas has a rotational temperature of ~10 K at all locations. The quiescent CH3OH abundance peak and one outflow position were searched for complex molecules. Narrow, 0.6-0.8 km s-1 wide, HCOOCH3 and CH3CHO lines originating in cold gas are clearly detected, CH3OCH3 is tentatively detected and C2H5OH and HOCH2CHO are undetected toward the quiescent core, while no complex molecular lines were found toward the outflow. The core abundances with respect to CH3OH are ~2.3% and 1.1% for HCOOCH3 and CH3CHO, respectively, and the upper limits are 0.7-1.1%, which is similar to most other low-mass sources. The observed complex molecule characteristics toward B1-b and the pre-dominance of HCO-bearing species suggest a cold ice (below 25 K, the sublimation temperatu re of CO) formation pathway followed by non-thermal desorption through e.g. UV photons traveling through outflow cavities. The observed complex gas composition together with the lack of any evidence of warm gas-phase chemistry provide clear evidence of efficient complex molecule formation in cold interstellar ices.
1976-06-01
Radiation degradation of cellulose fibers was investigated by gel permeation chromatography (GPC). Scoured cotton of Mexican variety (cellulose I), Polynosic rayon (cellulose II), and their microcrystalline celluloses obtained by hydrolysis of the original fibers were irradiated by Co-60 ..gamma..-rays under vacuum or humid conditions. The irradiated samples were then nitrated under nondegradative conditions. The molecular weights and molecular weight distributions were measured by GPC using tetrahydrofuran as solvent. The relationship between molecular weight and elution count was obtained with cellulose trinitrate standards fractionated by preparative GPC. The degree of polymerization of the fibers decreased with increasing irradiation dose, but their microcrystalline celluloses were only slightly degraded by irradiation, especially in microcrystalline cellulose from cellulose I. Degradation of the fibers irradiated under humid conditions was less than that irradiated under vacuum. It was found that the G-values for main-chain scission for the irradiated cellulose I, cellulose II, microcrystalline cellulose I, and microcrystalline cellulose II were 2.8, 2.9, less than 1, and 2.9, respectively, but the G-value for main-chain scission for the irradiated cellulose II was increased to 11.2 at irradiation doses above 3 Mrad. Consequently, it is inferred that cellulose molecules in the amorphous regions are degraded more readily, and the well-aligned molecules in crystalline regions are not as easily degraded by irradiation.
A Widely-Separated, Highly-Occluded Companion to the Nearby Low-Mass T Tauri Star TWA 30
2010-08-26
We report the discovery of TWA 30B, a wide (~3400 AU), co-moving M dwarf companion to the nearby (~42 pc) young star TWA 30. Companionship is confirmed from their statistically consistent proper motions and radial velocities, as well as a chance alignment probability of only 0.08%. Like TWA 30A, the spectrum of TWA 30B shows signatures of an actively accreting disk (H I and alkali line emission) and forbidden emission lines tracing outflowing material ([O I], [O II], [O III], [S II], and [N II]). We have also detected [C I] emission in the optical data, marking the first such detection of this line in a pre-main sequence star. Negligible radial velocity shifts in the emission lines relative to the stellar frame of rest (Delta V < 30 km/s) indicate that the outflows are viewed in the plane of the sky and that the corresponding circumstellar disk is viewed edge-on. Indeed, TWA 30B appears to be heavily obscured by its disk, given that it is 5 magnitudes fainter than TWA 30A at K-band despite having a slightly earlier spectral type (M4 versus M5). The near-infrared spectrum of TWA 30B also evinces an excess that varies on day timescales, with colors that follow classical T Tauri tracks as opposed to variable reddening (as is the case for TWA 30A). Multi-epoch data show this excess to be well-modeled by a blackbody component with temperatures ranging from 630 to 880 K and emitting areas that scale inversely with the temperature. Th e variable excess may arise from disk structure such as a rim or a warp at the inner disk edge located at a radial distance of ~3-5 R_sun. As the second and third closest actively accreting and outflowing stars to the Sun (after TWA 3), TWA 30AB presents an ideal system for detailed study of star and planetary formation processes at the low-mass end of the hydrogen-burning spectrum.
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