X-ray emission from non-magnetic cataclysmic variables

Details X-ray emission from non-magnetic cataclysmic variables X-ray emission from non-magnetic cataclysmic variables

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.308..519k&link_type=abstract

Nature (ISSN 0028-0836), vol. 308, April 5, 1984, p. 519-521.

Physics

52

Binary Stars, Stellar Radiation, Variable Stars, White Dwarf Stars, X Ray Sources, Boundary Layer Flow, Stellar Coronas, Stellar Mass Accretion

Scientific paper

It is argued that at sufficiently low accretion rates a thermal instability in the accretion flow in cataclysmic variables leads to the formation of a hard X-ray emitting corona around the white dwarf. The corona is relatively superseded at higher accretion rates. It is shown that the cooling of such a corona gives the observed correlation between X-ray temperature and luminosity, and that hard X-ray production may be rather inefficient because of transport processes. These can give rise to soft X-ray emission from most of the white dwarf surface, with a correspondingly low effective temperature.

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