Abstract
A novel numerical simulation scheme designed to calculate compressible gas-flows in accretion discs is described. This is then applied to the study of accretion disc behaviour in the wake of a mass-transfer burst in a dwarf nova system. The disc is predicted to be dominated by tidal forces throughout much of the outburst–quiescent cycle. These results are, however, found to be incompatible with the observations of the dwarf novae SS Cygni and U Geminorum in outburst. This is interpreted as evidence against the simple mass-transfer burst model of dwarf novae outbursts and instead as indirect evidence for the variation in viscosity between quiescence and outburst.
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