Hard X-ray Emission from White Dwarfs

Details Hard X-ray Emission from White Dwarfs Hard X-ray Emission from White Dwarfs

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20111910c&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #119.10; Bulletin of the American Astronomical Society, Vol. 34, p.1301

Astronomy and Astrophysics

Astronomy

Scientific paper

White dwarfs can be soft X-ray (<0.4 keV) sources if their temperatures are high and atmospheric opacities are low. Hard X-ray emission ( ~1 keV) associated with white dwarfs has been attributed to either a late-type companion with coronal activity or accretion of stellar material from a companion onto the surface of a white dwarf. However, using the ROSAT archive we have found hard X-ray emission from a number of apparently single white dwarfs. The most intriguing case is WD 1134+300 (GD 140), whose PSPC spectrum shows distinct hard X-ray emission, but whose 2MASS photometry shows no near-IR excess. Its small distance, 15 pc, helps to rule out the possibility of a hidden stellar-mass companion. New hard X-ray mechanisms are needed for white dwarfs. We are undertaking a thorough search for hard X-ray emission from white dwarfs using the entire ROSAT archive. We will produce a complete catalog of X-ray sources associated with white dwarfs and provide X-ray spectral information.

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