Photospheric, circumstellar, and interstellar features of He, C, N. O, and Si in the HST spectra of four hot white dwarf stars

Details Photospheric, circumstellar, and interstellar features of He, C, N. O, and Si in the HST spectra of four hot white dwarf stars Photospheric, circumstellar, and interstellar features of He, C, N. O, and Si in the HST spectra of four hot white dwarf stars

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109.1220s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 109, no. 3, p. 1220-1230

Other

12

Absorption Spectra, Abundance, Emission Spectra, Stellar Atmospheres, Stellar Envelopes, Stellar Winds, Ultraviolet Spectra, White Dwarf Stars, Carbon, Helium, Hubble Space Telescope, Lyman Alpha Radiation, Nitrogen, Oxygen, Signal To Noise Ratios, Silicon, Spectrum Analysis

Scientific paper

This paper reports on the observations of four hot white dwarf stars with the spectrographs on the Hubble Space Telescope (HST). The higher resolving power and higher signal/noise, in comparison with IUE, reveals a very rich phenomomenology, including photospheric features from heavy elements, circumstellar features, and the first direct detection of accretion onto the white dwarf component of a binary system. Specific results include the following: Our observations of the ultrahot degenerate H1504+65 confirm that it has a photosphere which is depleted in both H and He, and reveals features of C IV and O VI. The spectrum fits previously published models extremely well. The intermediate-temperature DO star PG 1034+001 has an ultraviolet spectrum showing complex profiles of the well-known resonance doublets of C IV, N v, and Si IV. The O V 1371 line shows a clear separation into a photospheric and a circumstellar component, and it is likely that the same two components can explain the other lines as well. The cooler DA star GD 394 has an extensive system of heavy-element features, but their radial velocity is such that it is highly unlikely that they are formed in the stellar photosphere. Time-resolved spectra of the accreting white dwarf in the V 471 Tau binary system are briefly presented here; they do show the presence of C IV, Si IV, and He II. However, the C IV and He II lines are in emission, rather than in aborption as had been expected.

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