Time evolution of the accretion disk radius in a dwarf nova

Statistics – Computation

Scientific paper

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Accretion Disks, Computational Astrophysics, Dwarf Novae, Stellar Evolution, Stellar Mass Accretion, Angular Momentum, Cataclysmic Variables, Finite Difference Theory, Stellar Mass

Scientific paper

The time evolution of the accretion disk radius in the outburst cycle of a dwarf nova has been studied. A numerical scheme for calculating the time evolution of accretion disks is presented, in which both the mass and the angular momentum of the system are exactly conserved during evolution, and in which the tidal torque and tidal dissipation exerted by the secondary star on the accretion disk are taken into account. By using this method, we have examined the time evolution of the disk radius in the dwarf nova outburst cycle based on both the mass transfer burst model and the disk instability model. The disk instability model is able to explain the basic observed features of the disk radius variation; i.e., expansion of the disk during outburst and its gradual shrinkage in quiescence. The mass-transfer burst model gives, at first sight, a similar variation in the disk radius with time. However, if examined closely, it is found that the mass-transfer burst model gives rise to a transient decrease in the disk radius at the onset of an outburst, and very little shrinkage in the disk radius in quiescence; those two features are inconsistent with observations.

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