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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 325 records · Page 18
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NASA NTRS1980

Mass flow analysis of the ultraviolet spectrum of UW Canis Majoris

The ultraviolet spectrum of the close binary UW CMa, obtained with the Copernicus (OAO-3) and IUE satellites in the wavelength region from 1010 to 1510 A and from 1200 to 3000 A, respectively, is analyzed. The observed P Cygni line profiles are compared with theoretically predicted profiles formed by isotropic and coherent scattering in a spherically symmetric expanding circumstellar envelope. Tables illustrate the identified stellar lines, laboratory wavelengths, and line strengths in terms of peak height for emission or central depth for absorption components, normalized to the local stellar continuum.

Drechsel, H.↗
NASA NTRS1980

Ultraviolet observations of close binary stars

Far ultraviolet observation of three interacting binary stars (HR 2142, HR 7084, and lambda Tauri) made with the Copernicus satellite during 1978-79 are presented. All stars exhibit evidence of a gas stream and extensive mass outflow from the system. Physical parameters, derived for the gas stream in HR 2142, are essentially within the range predicted from theoretical calculations.

Polidan, R. S.↗
NASA NTRS1980

Interstellar gas in the Gum Nebula

A survey of the interstellar gas near the Gum Nebula by optical observation of 67 stars at Ca II, 42 stars at Na I, and 14 stars in the UV with the Copernicus satellite provided radial velocities and column densities for all resolved absorption components. Velocity dispersions for gas in the Gum Nebula are not significantly larger than in the general interstellar medium; the ionization structure is predominantly that of an H II region with moderately high ionization. Denser, more highly ionized clouds are concentrated toward the Gum Nebula; these clouds do not show the anomalously high ionization observed in the Vela remnant clouds.

Wallerstein, G.↗
NASA NTRS1980

Interstellar depletions and far-ultraviolet extinction in the Rho Ophiuchi cloud

Copernicus ultraviolet data on six stars embedded in the well-studied Rho Ophiuchi cloud complex have been analyzed for interstellar abundances, densities, and far-ultraviolet extinction parameters, in an effort to determine how interstellar depletions depend on physical conditions. While there are variations within the cloud in the overall depletions, the pattern of depletions from element to element is constant for all six lines of sight. A picture is suggested in which the cloud core has a small velocity dispersion or is either so strongly depleted or so dense (hence not ionized) that the lines of first ions of heavy elements do not arise there, but rather form in a less-dense or less-depleted outer region. The cloud as a whole has substantial depletions, average to low far-ultraviolet extinction, and a low ratio of molecular to atomic hydrogen.

Snow, T. P., Jr.↗
NASA NTRS1980

The discovery of 'Sco X-1 type' behaviour from the X-ray burster 4U 1735 - 44

A series of Copernicus, Ariel V and optical observations of the X-ray burst source 4U 1735 - 44 (= MXB 1735 - 44) revealed properties very similar to those of the 'Sco X-1 like' sources. During one run, the non-burst X-ray flux varied by a factor of 2 on a time-scale of hours and this was associated with a general hardening of the spectrum. The source was relatively constant throughout the remaining observations. An Ariel V spectrum obtained during a quiescent interval deviated from a simple thermal model in that it showed both a high energy deficiency and a low energy excess. Near simultaneous spectroscopy of the optical counterpart confirmed the general features reported by McClintock et al. Spectra taken on successive nights revealed the H-beta emission to be variable.

White, N. E.↗
NASA NTRS1980

X-ray observations of the OAO1653-40 field

The region of sky containing OAO1653-40 have been observed simultaneously with the Einstein and Copernicus satellites in 1979 August. A best position of RA = 254.318 degrees, Dec = -41.577 degrees (1950) and a period of 38.019 + or - 0.009 sec were obtained for the X-ray pulsar discovered by White and Pravdo. The X-ray spectrum shows considerable photoelectric absorption with an equivalent hydrogen column density of 2.3 x 10 to the 23rd atom per sq cm. An upper limit to any 0.5-3.0 keV flux from V861 Sco of (4 + or - 1) x 10 to the -13th erg /sq cm/sec was also obtained.

Parmar, A. N.↗
NASA NTRS1980

The interstellar material in front of Chi Ophiuchus. II - Ultraviolet observations

The high-resolution UV spectrometer aboard the Copernicus satellite was used to observe the interstellar gas toward the moderately reddened star Chi Oph. The data are consistent with the hypothesis that the material in both the -6 and -12 km/s blend of gas and the -26 km/s cloud could have been affected by shock front activity, though the signatures of that activity are different in each case. These observations of the blend of gas establish that both low and high density neutral material must be present.

Frisch, P. C.↗
NASA NTRS1980

Abundance determinations for interstellar gas

The results of general abundance studies, using the Copernicus satellite are reviewed. The general pattern of depletion of some elements such as Si, Al, Mn, Fe, and Mg, near the sun is described. Techniques for obtaining abundances for various species are discussed, as are the aspects of the analysis which are uncertain. Variations in gas phase abundance from region to region are found for Fe and Si, similar to variations now known to exist for Ca and Ti based on visible spectra. A new generation of space instruments, with higher efficiency and resolution, in particular for 920-1400 A, can provide detailed interstellar line profiles.

York, D. G.↗
NASA NTRS1980

HR 4453 - An anomalously bright UV source

Crawford et al. (1979) reported that HR 4453 has an anomalously large UV flux in the 1350-1600 A band. This paper reports results of the UV spectrophotometry of HR 4453 obtained with the Copernicus satellite. Portions of the spectrum from 1120 to 2660 A were scanned, but no stellar signal was detected in any wavelength interval. This result is consistent with both components of the binary being normal A2A stars. UV variability or a source other than HR 4453 must be invoked to explain the observations of Crawford et al.

Polidan, R. S.↗
NASA NTRS1980

The abundance of CO in diffuse interstellar clouds - An ultraviolet survey

CO was detected in 17 directions and its upper limits were estimated in 21 directions by a UV survey carried out with the Copernicus satellite in the C-X 1088 A and E-X 1076 A lines toward 48 bright stars. The CO column densities range from 10 to the 12th to 10 to the 17th/sq cm and correlate with C I and H2. The tendency of the C I/CO ratio to be about 10 follows the ratio of particular atomic and molecular cross-sections and the physical parameters of interstellar clouds. Finally, the connection between UV observations in diffuse clouds and radio observations of (C-13)O in dark clouds is discussed.

Federman, S. R.↗
NASA NTRS1980

Comparisons of interstellar CH/+/ and H2

Copernicus observations of H2 toward stars in the Pleiades and 23 Orionis have been obtained because of their importance in understanding the formation of interstellar CH(+). No model of CH(+) equilibrium seems to agree very well with these observations; in particular, the suggestions that CH(+) is formed either from collisions between vibrationally excited H2 and C(+) or from radiative association of C(+) and H2 can apparently be excluded. These data do suggest that there is a correlation between the amounts of rotationally excited H2 and CH(+) which are present. Observations of the Pleiades also help interpretations of the reflection nebulae near these stars.

Frisch, P. C.↗
NASA NTRS1980

The interstellar medium on the Gamma Cassiopeiae line of sight

The interstellar medium on the Gamma Cas line of sight is studied through the observations of O I, H2, H I, D I, and Ar I absorption features with the Copernicus satellite. By using the velocity structure of the line of sight previously determined through atomic nitrogen, it is demonstrated that these neutrals are located in the same physical regions and that the O I and Ar I abundances could be solar, on the average, relative to N I in all components. The 1066.660 A Ar I line profile is contaminated by an unidentified line, already detected in the spectrum of Zeta Pup. Furthermore, a peculiar behavior of the Ar I abundance in the different components is reported, possibly associated with high-velocity interstellar gas present on the line of sight. It is concluded that the Gamma Cas line of sight could intercept a dense cloud which has been engulfed and disrupted by a shock.

Ferlet, R.↗
NASA NTRS1981

A study of the Mg II k line in Beta Persei

Spectral scans of the Mg II k line in Beta Per were obtained with Copernicus during two primary eclipses. A brief description of observation in a short frame mode is given. The observed data are compared with computed line profiles based on the eclipse geometry of spherical stars. It is shown that a nonuniform circumstellar envelope, or cloud, probably is present. In one scan, a red-shifted line of P Cygni-type profile appeared, indicating the occurrence of an unusual event in the close binary system.

Chen, K.-Y.↗
NASA NTRS1981

Phase-correlated P Cygni profile variations of the C III multiplet in UW Canis Majoris

The interacting close binary system UW CMa has been observed, in the wavelength range from 1161 to 1188 A, continuously during a complete orbital cycle in 1979 with the Copernicus (OAO-3) U2 spectrometer. The C III multiplet at 1175 A, observed as a P Cygni feature, exhbits a clear dependence on the orbital phase of the binary; the radial velocity variation of this feature lags behind that of the O7 primary component by 0.1 orbital phase, which agrees with the anticipations in an earlier study by the same authors. The radiation-driven matter, flowing out of the binary, originates in the primary component.

Drechsel, H.↗
NASA NTRS1981

Far-ultraviolet spectra and flux distributions of some Orion stars

Far-ultraviolet (950-1800 A) spectra with about 2 A resolution were obtained of a number of stars in Orion during a sounding-rocket flight 1975 December 6. These spectra have been reduced to absolute flux distributions with the aid of preflight calibrations. The derived fluxes are in good agreement with model-atmosphere predictions and previous observations down to about 1200 A. In the 1200-1080 A range, the present results are in good agreement with model predictions but fall above the rocket measurements of Brune, Mount and Feldman. Below 1080 A, our measurements fall below the model predictions, reaching a deviation of a factor of 2 near 1010 A and a factor of 4 near 950 A. The present results are compared with those of Brune et al. via Copernicus U2 observations in this spectral range, and possible sources of discrepancies between the various observations and model-atmosphere predictions are discussed. Other aspects of the spectra, particularly with regard to spectral classification, are briefly discussed.

Carruthers, G. R.↗
NASA NTRS1981

Titan's hydrogen torus

A model of Titan's hydrogen torus, capable of describing its time evolution under the influence of the gravitational fields of both the satellite and the planet, is presented. Estimated lifetimes for hydrogen atoms near Titan's orbit of the order of 10 to the 7th s, based on recent Pioneer 11 measurements, suggest that the torus completely encircles Saturn and is angularly unsymmetric, having an enhanced gas density near the satellite. New model calculations confirm this and provide an explanation for the torus detected by the Copernicus satellite and the UV instrument of Pioneer 11. Agreement between calculated and observed Lyman alpha intensities suggests a hydrogen escape flux between 1 x 10 to the 9th/sq cm-s and 3 x 10 to the 9th/sq cm-s should be operative at Titan. This produces a torus containing some 10 to the 34th hydrogen atoms.

Smyth, W. H.↗
NASA NTRS1981

Observationally determined silicon II oscillator strengths

Si II oscillator strengths for eight resonance lines from the ground state have been determined using a curve-of-growth analysis of interstellar data from the Copernicus and International Ultraviolet Explorer satellites. The oscillator strengths for 1526 A and 1808 A increase by factors of 3.0 and 1.5, respectively, from previously tabulated values; those for 989 A and 1020 A decrease by factors of 0.55 and 0.60, respectively. These new values result in better silicon abundances for interstellar clouds and resolve a long-standing puzzle in the interpretation of quasar absorption line data.

Shull, J. M.↗
NASA NTRS1981

Boron and beryllium in Gamma Geminorum

Observations have been made of the B II resonance line at 1362 A in the A0 IV star Gamma Gem with the Princeton spectrometer on the Copernicus satellite at a spectral resolution of 0.05 A. Complementary ground-based observations of the Be II resonance lines at 3130 and 3131 A have been made at Mauna Kea Observatory with a comparable resolution. A model-atmosphere abundance analysis has been done which includes the effects of the lines that blend with the B II and Be II lines. Previous data on Alpha Lyr and Alpha CMa for B II (which blends with a V III feature) have been reanalyzed with the help of new photographic and Reticon data from Mauna Kea which enable the determination of the V abundance. The results show that Gamma Gem is depleted in B by a factor of 5-10 relative to Alpha Lyr and other normal B stars and depleted in Be by at least a factor of four. By comparison, the hot Am star Alpha CMa is B-deficient by about three orders of magnitude and Be-deficient by at least fifteen times. It is suggested that the abundance deficiencies are due to diffusion, and that Alpha CMa is intrinsically a slow rotator, and Gamma Gem is a slightly evolved slow rotator where some, but not all, of the B and Be has resurfaced.

Boesgaard, A. M.↗