Computer Science
Scientific paper
Apr 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phdt.........8w&link_type=abstract
Ph.D. Thesis Oxford Univ. (England).
Computer Science
8
Accretion Disks, Dwarf Novae, Gas Flow, Mass Flow, Stellar Mass Accretion, Computerized Simulation, Kinematics, Mass Ratios, Mass Transfer, Tides, Variable Stars, Viscosity
Scientific paper
The problem of mass flow between the members of cataclysmic variable stars is addressed with particular emphasis to the U Geminorum and SU Ursae Majoris classes of dwarf novae. A new, two dimensional particle based numerical simulation of the kinematics of this gas flow was developed. This is used to determine constraints on the postulated mechanisms for dwarf nova eruptions. The observed outbursts were found inconsistent with the simple, constant viscosity mass transfer models which have been published to date. Instead the results suggests that the disc switches from a state of high viscosity in outburst to low viscosity in quiescence, as proposed by disc instability models. The tidal forces imposed by the companion stars upon the accretion flow are discovered to be important; with two classes of possible disc behavior in outbursts: a tidally stable disc and a tidally unstable disc. The tidally stable disc exists in those systems where the primary is less than four times as massive as the secondary; the unstable disc occurs in outbursts of systems with more extreme mass ratios. This division corresponds to the observed distinction between the SU Ursae Majoris and U Geminorum classes of dwarf novae.
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