Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...393..729w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 393, no. 2, July 10, 1992, p. 729-741. Research supported by University of
Astronomy and Astrophysics
Astrophysics
27
Accretion Disks, Cataclysmic Variables, Eclipsing Binary Stars, Novae, Stellar Magnitude, White Dwarf Stars, Brightness Distribution, Maximum Entropy Method, Optical Thickness, Stellar Rotation
Scientific paper
The surface brightness distribution in the accretion disk of V Per is reconstructed using a maximum entropy technique. The resulting brightness temperature gradient is much less steep than that from a standard steady state, optically thick disk for all reasonable mass accretion rates. A model including a rim which obscures part of the disk does not resolve this discrepancy. However, if the inner disk is disrupted out to about 0.15-0.25RL1 (for example by a magnetic field), the brightness temperature gradient can be very close to Tb varies as R exp -3/4 (1-b(Rin/R)exp 1/2) law. The value of Rin needed to match this steady state distribution depends on the distance to the system, its size and brightness, and the rotation rate of the white dwarf.
Abbott Timothy Mark Cameron
Shafter Allen W.
Wood Janet H.
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