Hard X-rays from accretion disk boundary layers

Details Hard X-rays from accretion disk boundary layers Hard X-rays from accretion disk boundary layers

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993natur.362..820n&link_type=abstract

Nature (ISSN 0028-0836), vol. 362, no. 6423, p. 820-822.

Computer Science

119

Accretion Disks, Boundary Layer Flow, Luminosity, White Dwarf Stars, X Ray Spectra, Cataclysmic Variables, Self Consistent Fields, Stellar Mass Accretion, Temperature Distribution

Scientific paper

Numerical solutions are presented for a model of thin accretion disks around a white dwarf which encompasses a self-consistent description of the boundary layer. For a high accretion rate M, there emerge optically thick boundary layers whose radial width and peak temperature decrease with decreasing M; when M falls below a critical value, however, the boundary layer becomes optically thin while width and temperature dramatically increase. These results account for the hard X-rays observed in cataclysmic variables, especially at low M.

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