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- W1489098576 abstract "Since the first soft X-ray and EUV studies of hot DA white dwarfs it has been apparent that the fluxes of white dwarfs in these wavelength ranges are significantly lower than predicted (e.g. Kahn et al. 1984; Petre, Shipman & Canizares 1986; Jordan et al. 1987; Paerels & Heise 1989; Koester 1989). All this work made the simplifying assumption that helium was the sole photospheric opacity source, although the He in these stars was never identified spectroscopically. Moreover, the shape of the EXOSAT spectrum of Feige 24 could only be matched by models including trace abundances of elements heavier than H or He (Vennes et al. 1989). More recent studies combining the soft X-ray and EUV data available from the ROSAT sky survey show that He alone cannot be responsible for absorption in these bands and that most of the hottest stars (T eff > 40, 000K) must have heavier elements in their atmospheres to explain the observed fluxes (Barstow et al. 1993; Wolff et al; 1996, Marsh et al. 1995). In parallel, observational evidence has been acquired by the International Ultraviolet Explorer (IUE) revealing high ionization features attributed to C, N, and Si (e.g. Bruhweiler & Kondo 1981 & 1983). Subsequently, O, Fe and Ni were also directly." @default.
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- W1489098576 date "1997-01-01" @default.
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- W1489098576 title "Heavy Elements in White Dwarf Envelopes" @default.
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- W1489098576 doi "https://doi.org/10.1007/978-94-011-5542-7_33" @default.
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