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At least 91 records · Page 5

Ultraviolet spectroscopy of the nova-like variable V3885 Sagittarii /= CD -42 deg 14462/

Low-dispersion long and short wavelength IUE spectra of the nova-like system V3885 Sgr were obtained on 1979 August 24 UT. The UV spectrum exhibits strong, high-temperature absorption lines of C III, C IV, He II, N IV, N V, and Si IV which all have relatively large negative velocities of 600-1000 km/s at their line centers. The C IV (1550 A) features shows a P Cygni-type profile with a blueshifted absorption line; the presence of the P Cygni-type feature strongly suggests a significant mass outflow from the system in the form of a hot stellar wind. The observed continuum fluxes are fitted with theoretical accretion disk model fluxes, and a tentative physical interpretation of the observed spectral properties is presented.

Guinan, E. F.↗

Luminosities and masses for three central stars of planetary nebulae in the Magellanic Clouds from ultraviolet spectroscopy with the IUE

Physical parameters of the central stars of the planetary nebulae (PN) P40, N2, and N5 are determined from UV observations by the IUE spacecraft and emission line-data. The observations took place on May 23 and 26, 1981. Derived properties, such as the H-beta, color excess, nebular hydrogen emission, helium emission, and stellar continuum emission, the stellar radius, surface gravity, Zanstra temperature, luminosity, absolute bolometric magnitude, apparent visual magnitude, mass, and Zanstra parameter for the three PN central stars are presented. All the masses were over one solar mass, suggesting a specific PN nuclei mass. The finding was corroborated by all luminosities exceeding the Eddington luminosity for a 0.6 solar mass star, which has previously been calculated for the white dwarf core of a PN.

Stecher, T. P.↗

Ultraviolet spectroscopy of the zodiacal light

The results of observations of the zodiacal light at 25 A resolution from two different viewing angles are reported. Airglow emission from both NO and O II were identified spectroscopically and according to altitude variation. The UV spectrometer was rocket-borne, and functioned in the wavelengths from 1700-3150 A. The solar spectrum was matched at wavelengths higher than 2600 A. Using the smaller elongation angle, an upper limit for the zodiacal light was determined to be 190 millionth erg/sq cm per sec per A/sr at 1800 A, i.e., four times the solar brightness at the same wavelength. It was found that the zodiacal light dependence on elongation was the same in the UV as in the visible. The color ratios for 2100-2400 A is discussed.

Cebula, R. P.↗

Ultraviolet spectroscopy of selected astronomical sources

The birth rates of various kinds of white dwarf progenitors are estimated and the spectra of two very hot O-type white dwarfs are analyzed. The effective temperature of LSE 21 was found to be in excess of 100,000 K. The abundance of iron in the atmospheres of two central stars and numerous very hot O-type subdwarfs was found to be strongly variable. Results obtained by high resolution optical spectroscopy, UBV photometry, and low resolution IUE spectrophotometry for LSS 2018, the central star of the planetary nebulae DS1, are summarized. A planetary nebula surrounding the very hot subdwarf LSS 1362 was discovered. Analysis of results obtained by high resolution optical spectra shows agreement with an effective temperature of 110,000 K derived using low resolution IUE observations.

Drilling, J. S.↗

Ultraviolet spectroscopy of the 'jetlike' condensations of NGC 4151

The spectrometers aboard the IUE are used to obtain UV spectroscopy of the jetlike condensations seen extending 18 arcsec from the nucleus of the nearby Seyfert 1 galaxy NGC 4151. New data reduction techniques are used to detect, delineate, and measure weak nebular emission in IUE spectra. Spatially resolved extended emission is seen in both semiforbidden C III 1909 A and C IV 1549 A. The deduced integrated fluxes in the jet are 10 to the 14th and 4 x 10 to the 14th ergs/sq cm/s for C III and C IV, respectively. The observed fluxes are compared with predictions based upon a central source photoionization model. The implied high C IV/C III flux ratio is shown to be inconsistent with this model and suggests an additional source of ionization for the jet.

Bruhweiler, F. C.↗

Spatially resolved ultraviolet spectroscopy of the liner NGC 3998

Results of IUE observations of the Liner NGC 3998 are reported. Spatial structure in the long wavelength emission is apparent; the spatial profiles from the LWP line-by-line images show a two-component structure, with an unresolved central component superimposed on extended underlying emission. The LWP emission was separated into component spectra. The unresolved component spectrum is considerably flatter than the extended component spectrum, which is dominated by fairly late type stars (late F to early G). The unresolved component also shows strong C II) 2326 A and broad Mg II 2800 A emission.The width of the Mg II emission is 8600 km/sec, and its profile agrees quite well with the broad wings of the H alpha emission. The results support the idea that NGC 3998 may contain a dwarf Seyfert nucleus.

Reichert, G. A.↗

Far-ultraviolet spectroscopy of the quasar UM 675 with the faint object spectrograph on the Hubble Space Telescope

To investigate the far-UV spectral properties of a QSO and to look for evidence of He I 584 A emission and absorption the Faint Object Spectrograph aboard the HST was used to observed UM 675. Light is detected down to 520 A in the object in the rest frame and limits are set to He I emission, the He I Gunn-Peterson effect at z = 2.148, and Ly-alpha absorption at z roughly 0.5.

Beaver, E. A.↗

Spatially resolved ultraviolet spectroscopy of the LINER galaxy NGC 3998

Results of recent IUE observations of the LINER galaxy NGC 3998 are reported. Spatial structure in the LW emission is apparent; the spatial profiles in the longwave primary (LWP) images show a two-component structure, with an unresolved central component superposed on extended underlying emission. New software, which exploits a knowledge of the LWP point spread function and its variation with wavelength, is used to model the spatial profiles and to separate the LWP emission into component spectra. The unresolved component spectrum is found to be considerably flatter than the spectrum of the extended component, which is dominated by fairly late-type stars. The unresolved component exhibits strong semiforbidden C II 2326 and broad Mg II 2800 emission. The width of the Mg II emission is about 8000 km/s, and its profile agrees quite well with the broad wings of the H-alpha emission.

Reichert, G. A.↗

Extreme ultraviolet spectroscopy of G191-B2B - Direct observation of ionization edges

We present the first spectrum of the hot, DA white dwarf G191-B2B (wd 0501 + 527) between 200 and 330 A. The spectrum, which has about 2 A resolution, was obtained with a sounding rocket-borne, grazing incidence spectrograph. The spectrum shows no evidence of He II, the expected primary opacity source in this wavelength region. Three ionization edges and one absorption feature were observed and are suggestive of O III existing in the photosphere of G191-B2B. Also noted is a broad spectral depression that may result from Fe VI in the photosphere.

Wilkinson, Erik↗

Airglow studies using an all-reflection interferometer for extreme ultraviolet spectroscopy (ARIES)

Ultrahigh resolution line studies can deepen insight into the excitation processes and structures of the upper atmosphere; attention is presently given to the possibility of a study of terrestrial atomic oxygen in the thermosphere through measurements of the O I 1304 A solar and terrestrial airglow emissions from a sounding rocket. These line profile studies of the airglow yield a relative contribution of the two main excitation mechanisms (photoelectron impact and solar-resonance scattering), as well as a verification of cross section and branching ratios.

Cotton, D. M.↗

Long-slit ultraviolet spectroscopy of Comet Austin (1990 V)

The spatial distributions of the brightest features in the far-UV spectrum of Comet Austin were measured, and it is found that they are generally similar to those found for Comet Halley during two rocket observations in 1986. As in Halley, the CO profile can be fit to a radial outflow profile for a source whose size is smaller than the instrumental spatial resolution. Neither the shape nor the magnitude of the extended atomic carbon profiles, however, can be satisfactorily explained by the photodissociation of CO. No evidence is found for an extended source of CO in the coma; thus, suggestions that the additional carbon can come directly from grains are difficult to accept since Austin is a low-dust comet. The presence of the O I 1356 A feature implies that there is a photoelectron excitation source in the coma. The measured O I 1304 A distribution is consistent with H2O being the dominant source of oxygen in the coma. The atomic sulfur profile matches that expected for a daughter product of relatively short-lived parents.

Sahnow, David J.↗

Hubble Space Telescope ultraviolet spectroscopy of the highly polarized but quiescent quasar OI 287

The quasar OI 287 has a unique combination of properties, including a high and constant optical polarization oriented parallel to the radio axis, a quiescent optical flux, and a lobe-dominant radio source. Previous studies have led to the picture of an edge-on thin dusty torus occulting a featureless continuum (FC) source and a broad line region (BLR) in this object. The FC source and the BLR are seen only in reflected (polarized) light. In the unified models, this makes OI 287 a 'quasar 2', analogous to the type 2 Seyfert galaxies and the narrow-line radio galaxies. Our UV spectrum adds two bits of information consistent with the above ideas. First, the spectrum neither turns up in the UV, as expected for optically thin dust scattering, nor turns down as expected for polarization by dust transmission. It is consistent with reflection by free electrons or optically thick dust. Second, there are in fact blueshifted absorption troughs associated with the C IV 1549 A line, supporting the analogy with BALs, as well as the idea that the BALs are objects which present a nearly edge-on view of a disk structure.

Antonucci, Robert↗

Far-ultraviolet Spectroscopy of O+o Binaries in the Magellanic Clouds

We report FUSE observations in 2006 of three O-type, double-lined spectroscopic binaries in the Magellanic Clouds. Their binary nature was discovered only in the past several years. The systems have very short periods (1.4 - 2.25 days), represent rare, young evolutionary stages of massive stars and binaries, and provide a unique glimpse at some of the most massive systems that form in dense clusters of massive stars. The systems are: LH54-425 in the LMC (O3IIIf + O6V, P=2.25 days, approx. 100+50 Mo), J053441-693139 in the LMC (O2-31f + O6V, P=1.4 days, 41+27 Mo), and Hodge 53-47 in the SMC (O6V + O4-5IIIf, P=2.2 days, 24+14 Mo, where the O4 star appears to be less massive than the O6 star). These represent some of the most massive binaries known. Their short periods indicates that wind interaction and mass transfer are likely important factors in their evolution. The spectra provide quantitative and systematic studies of phase-dependent stellar wind properties, wind collision effects in O+O binaries at lower metallicities, improved radial velocity curves, and FUV spectrophotometric changes as a function of orbital phase.

Sonneborn, George↗

The Mariner Mars 1971 orbiter.

The Mariner Mars 1971 (MM '71) orbiter spacecraft, launched toward Mars in the spring of 1971, was designed to offer the first opportunity for sustained observations in the near vicinity of another planet of our solar system. The MM '71 spacecraft, like its predecessors, is fully attitude stabilized about three axes, using the sun and Canopus as references, an orientation which allows use of photovoltaic solar panels for primary power and permits two-way communication to the earth through a high-gain directional antenna. Midcourse and orbit insertion maneuvers use the sun-Canopus orientation as a reference direction for initiating commanded turns. Scientific instruments employed during Mars orbital operations are mounted on a two-degree-of-freedom platform controlled by commands from the central computer and sequencer. Science measurements to be obtained by the MM '71 spacecraft include television visual imaging, infrared radiometry, infrared spectroscopy, ultraviolet spectroscopy, S-band radio occultation, and celestial mechanics.

Scull, J. R.↗

Electrochemical Corrosion and Catalysis Dynamics of Tin Oxide during Water Oxidation

Metal oxide corrosion severely limits anodic electrocatalysis, particularly at high potentials in acidic environments, where degradation pathways remain poorly defined. This study establishes explicit connections between corrosion and electrocatalysis on tin oxide during water oxidation by examining the roles of lattice defects, reactive oxygen species, interfacial pH variations, and speciation of corroded tin in acid. We first demonstrate the presence of structural defects such as oxygen vacancies and substoichiometric Sn(II) species by integrating electron paramagnetic resonance spectroscopy, ultraviolet photoelectron spectroscopy, and Mott–Schottky analysis. Kohn–Sham density functional theory calculations reveal that explicit water structures thermodynamically stabilize reaction intermediates and lower reaction overpotentials. Moreover, we propose that water dissociation leads to hydrogen-bonding networks formed by H* and OH* intermediates, which may span the entire catalyst surface and decrease the interfacial pH to drive corrosion. In contrast, the electrochemical generation of reactive oxygen species is shown to play a minor role in catalyst corrosion during water oxidation using inductively coupled plasma mass spectrometry coupled with selective chemical scavengers. Square-wave voltammetry combined with rotating ring-disk electrodes is used to reveal that under open-circuit conditions, only Sn(IV) cations chemically dissolve from tin oxide, while both Sn(IV) and Sn(II) species electrochemically corrode during water oxidation. Our results unveil a dynamic and complicated interplay between corrosive and catalytic pathways on metal oxide electrocatalysts: a decrease in interfacial pH due to water oxidation exacerbates Sn(II)/Sn(IV) corrosion. Subsequently, the electrochemical corrosion of Sn(II)/Sn(IV) facilitates product formation from lattice oxygen, while the redeposition of corroded Sn(II) as Sn(IV) can enable oxygen exchange with water. By elucidating the roles of defects and interfacial chemistry, this work provides a roadmap for engineering improved electrocatalysts that balance activity and stability, a critical step toward scalable and durable energy technologies.

36 MATERIALS SCIENCE↗

Integrated material-surface analyzer

These 10 surface-analysis tests can be run without breaking vacuum: secondary-ion mass spectroscopy, ion-scattering spectroscopy, electron-stimulated desorption, residual-gas analysis, auger electron spectroscopy, x-ray photoelectron spectroscopy, ultraviolet photoelectron spectroscopy, characteristic-electron energy-loss spectroscopy, scanning electron microscope, scanning low-energy electron probe. Quadruple mass spectrometer, used in first 4 tests, serves as electron transfer lens in last 6 tests.

Grunthaner, F. J.↗

Ultraviolet slit spectroscopy in the core of 30 Doradus with the International Ultraviolet Explorer

Low resolution (about 7 A) IUE observations of the core of the 30 Doradus Nebula in the Large Magellanic Cloud are presented. Data were obtained through the large entrance aperture at 11 different positions in both the long wavelength (1900-3200 A) and short wavelength (1150-2000 A) cameras. The aperture was stepped in 10-arcsec intervals, in the direction of the long axis of the aperture, effectively yielding a 2-arcmin long slit with the central object, R136, close to the center. The brightness distribution is strongly peaked at the position of R136, but it is found that the far-ultraviolet fluxes are dominated by luminous early-type stars at any position along the slit. The behavior of the ultraviolet colors along the slit implies that the core of 30 Dor lies behind a cloud of dust extending over at least 2 arcmin = 30 pc and suggests that the reddening law changes with distance from R136.

Koornneef, J.↗