The soft X-ray excess in accreting magnetic white dwarfs

Details The soft X-ray excess in accreting magnetic white dwarfs The soft X-ray excess in accreting magnetic white dwarfs

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...193..113f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 193, no. 1-2, March 1988, p. 113-118.

Astronomy and Astrophysics

Astrophysics

82

Magnetic Stars, Stellar Mass Accretion, White Dwarf Stars, X Ray Binaries, Cataclysmic Variables, High Energy Electrons, Magnetohydrodynamic Stability

Scientific paper

The authors re-examine various ideas that have been proposed to account for the excess of soft X-rays in AM Herculis stars and possibly also in intermediate polars. They find that conduction by high velocity electrons in the tail of a thermal distribution at the shock temperature cannot account for the observed excess even if the high opacities appropriate for the gas at the base of the column are invoked. The authors consider inhomogeneous and time-dependent accretion and determine the conditions under which overdense blobs can penetrate deep enough for their energy to be thermalized. These conditions place rather weak constraints on the possible instabilities which give rise to the blobs. It is concluded that inhomogeneities in the accretion stream are a viable explanation for the soft X-ray excess.

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