Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.2524d&link_type=abstract
American Astronomical Society, HEAD meeting #8, #25.24; Bulletin of the American Astronomical Society, Vol. 36, p.958
Astronomy and Astrophysics
Astronomy
Scientific paper
The soft X-ray emission from non-interacting hot white dwarfs (WDs) is the manifestation of the Wein tail of their photospheric spectra. In this context, the ROSAT PSPC pulse height spectrum of the peculiar He-rich hot WD KPD 0005+5106 provided a great surprise when first analysed. It exhibited more short wavelength flux than expected, and defied the best non-LTE modelling attempts in terms of photospheric emission. Instead, Fleming, Werner & Barstow found that a thermal plasma model with a temperature of 2-3× 105 K provided a much better match to the data. KPD 0005+5106 then appeared to be a unique object: it was the only known WD with a corona. However, a high resolution Chandra LETG+HRC-S spectrum of KPD 0005+5106 lacks the spectral shape of thermal bremsstrahlung and narrow lines of H-like and He-like C expected from a coronal plasma. Instead, there is a more continuous broad peak in emission between 40 and 50 Å, in addition to the expected photospheric emission toward longer wavelengths. We show here that the former component does not come from a corona, but arises from photospheric layers that become more transparent at those wavelengths. This flux is highly sensitive to the adopted Fe abundance and provides a rough Fe abundance diagnostic for KPD 005+5106.
Drake Jeremy J.
Werner Kirstin
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