The interstellar medium and the highly ionized species observed in the spectrum of the nearby white dwarf G191-B2B

Details The interstellar medium and the highly ionized species observed in the spectrum of the nearby white dwarf G191-B2B The interstellar medium and the highly ionized species observed in the spectrum of the nearby white dwarf G191-B2B

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...248l.123b&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 248, Sept. 15, 1981, p. L123-L127.

Astronomy and Astrophysics

Astrophysics

64

Interstellar Matter, Ionization, Resonance Lines, Stellar Spectra, Ultraviolet Spectra, White Dwarf Stars, Carbon, Extreme Ultraviolet Radiation, High Resolution, Iue, Nitrogen Ions, Plasma Density, Silicon, Spectrum Analysis, Stellar Envelopes

Scientific paper

High-resolution spectra of the nearby (48 pc) white dwarf G191-B2B, obtained with the International Ultraviolet Explorer, reveal sharp resonance lines of N V, C IV, and Si IV. The origin of these features is most likely linked to the white dwarf, possibly being formed in an expanding halo around the star. Interstellar lines of C II, N I, Mg II, Si II, and Fe II are also seen in the spectrum. Analysis of these features indicates an average neutral hydrogen number density of 0.064 for this line of sight. In combination with the recent EUV and soft X-ray results, this is interpreted to mean that the interstellar medium in the most immediate solar vicinity is of the normal density n approximately equal to 0.1/cu cm of lower ionization, while just beyond it, at least in some directions, is a hot lower density plasma. These results are apparently in conflict with the model of the interstellar medium by McKee and Ostriker (1977) in its present form.

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