Instabilities in dwarf nova accretion disks
The dwarf novae are close binary stars where the Roche lobe filling companion transfers mass to a white dwarf. Due to the high angular momentum of the overflowing material the gas cannot fall directly onto the compact object and an accretion disk is formed. The companion star is usually a low mass main sequence star. These binary systems are very common, well documented by observations in the optical wavelength region since a long time. These objects are therefore particularly well suited to study properties of accretion disks.
KeywordsAccretion Disk White Dwarf Companion Star Stefan Boltzmann Constant High Angular Momentum
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