High Resolution EUV Spectroscopy of Feige 24

Details High Resolution EUV Spectroscopy of Feige 24 High Resolution EUV Spectroscopy of Feige 24

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1273...52k&link_type=abstract

17TH EUROPEAN WHITE DWARF WORKSHOP. AIP Conference Proceedings, Volume 1273, pp. 52-57 (2010).

Physics

White Dwarfs, Photosphere, Stellar Evolution, Interstellar Matter, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Physical Properties

Scientific paper

We report the first high-resolution (R = 4000) spectroscopic observation of the binary DA white dwarf Feige 24 in the extreme-ultraviolet band 220-250A˚. A stellar atmosphere model assuming a homogeneous element distribution yields a best fit to the data that excludes a significant abundance of photospheric helium, a surprising result contrary to predictions by common envelope evolution theory. The upper limit on the photospheric helium abundance is 2.5×10-6 (90% confidence), and the lower limit on the overlying layer of hydrogen is 1.2×10-13 Msolar. An ionized He component (3.9×1017 cm-2) is clearly present along the line-of-sight, which if completely interstellar implies a He ionization fraction of 0.7, considerably higher than is typical of the local interstellar medium.

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