X-ray Emission from the Hot White Dwarf KPD 0005+5106: Corona or Accretion?

Details X-ray Emission from the Hot White Dwarf KPD 0005+5106: Corona or Accretion? X-ray Emission from the Hot White Dwarf KPD 0005+5106: Corona or Accretion?

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007cxo..prop.2351c&link_type=abstract

Chandra Proposal ID #09200839

Physics

Chandra Proposal Id #09200839

Scientific paper

X-rays at energies >0.5 keV, not expected from the photosphere of a white dwarf (WD), can be produced only in stellar coronae or from accretion of material onto a WD's surface. KPD 0005+5106 and WD 2226-210 are two outstanding cases of single WDs with X-ray emission at 1 keV. Recent Spitzer observations of WD 2226-210, the central star of the Helix Nebula, reveal excess continuum emission starting at 8 um and peaking at 24-70 um, indicating the existence of a dust disk at 50-100 AU from the star. The dust is most likely produced by collisions among Kuiper Belt-like objects (KBOs). Stray KBOs impacting the WD surface may produce the 1 keV emission. We request Chandra and Spitzer observations of KPD 0005+5106 to search for a similar dust disk and determine the origin of its 1 keV emission.

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