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Astron. Astrophys. 328, 247-252


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Evaporation of the accretion disk in dwarf novae during quiescence

B.F. Liu1,2, F. Meyer1, and E. Meyer-Hofmeister1

1Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, D-85740 Garching, Germany
2Yunnan Observatory, Academia Sinica, P.O. Box 110, Kunming 650011, China

Received 22 April 1997 / Accepted 4 July 1997

Abstract

We investigate the evolution of the accretion disk in dwarf nova systems during quiescence. This is the phase of accumulation of matter in the disk. We employ the evaporation model of Meyer $\&$ Meyer-Hofmeister (1994) in which above the cool inert disk, a self-sustained coronal layer is built up, fed by matter evaporating from the disk underneath. Conservation of mass and angular momentum governs the evolution of the coexisting cool disk and corona. We compute the evolution and show how the onset of the next outburst is influenced by the evaporation process.

Key words: accretion, accretion disk - cataclysmic variables - stars: white dwarfs - stars: coronae


© European Southern Observatory (ESO) 1997

Online publication: October 30, 1997
Last change: March 24, 1998
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