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X-rays from the magnetic white dwarf PG 1658 + 441
Pravdo, S. H.; Marshall, F. E.; White, N. E.; Giommi, P.
AA(California Institute of Technology, Jet Propulsion Laboratory, Pasadena), AB(NASA, Goddard Space Flight Center, Greenbelt, MD), AC(EXOSAT Observatory, Darmstadt, Germany), AD(EXOSAT Observatory, Darmstadt, Germany)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 300, Jan. 15, 1986, p. 819-823. NASA-supported research. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Magnetic Stars, White Dwarf Stars, X Ray Sources, X Ray Spectra, Stellar Atmospheres, Stellar Composition, Stellar Spectra, Stellar Temperature
Bibliographic Code:


X-ray emission has been detected from PG 1658 + 441, a hot, isolated, magnetic white dwarf. The source was first detected in an Einstein IPC observation and was later identified in an Exosat channel multiplier array observation. Both imaging observations were motivated by an attempt to find the optical counterpart to the HEAO 1 soft X-ray source H1659 + 44. Spectral analysis, however, indicates that H1659 + 44 and PG 1658 + 441 are unrelated. The broad-band spectrum of this DA white dwarf can be explained as emission from a homogeneous, high-gravity, pure hydrogen atmosphere with a temperature near 28,000 K. The observations of PG 1658 + 441 support the suggestion that a correlation exists between temperature and helium abundance in white dwarf atmospheres.

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