The behaviour of quiescent accretion discs in dwarf novae

Abstract

We propose a simple explanation for the constant mean brightness observed between outbursts in dwarf novae. Secular changes in the total energy dissipation rate of the accretion disc brought about by variations in surface density, temperature and disc radius can be regulated by the gradual cooling of a small, critically-stable hot inner region. The hypothesis is supported by two-dimensional time-dependent numerical models of dwarf nova accretion discs.

arXiv comment6 pages, 7 figures, accepted for MNRAS

References in corpus (4)

• The disc instability model of dwarf-novae and low-mass X-ray binary transients
• SPH simulations of tidally unstable accretion disks in cataclysmic variables
• Viscosity Mechanisms in Accretion Disks
• The X-ray Spectrum of the Dwarf Nova SS Cyg in quiescence and outburst

Cited by in corpus (6)

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• Transient outburst events from tidally disrupted asteroids near white dwarfs
• ULTRACAM photometry of the eclipsing cataclysmic variables GY Cnc, IR Com and HT Cas
• The steady-state structure of accretion discs in central magnetic fields
• SOAR observations of the high-viscosity accretion disc of the dwarf nova V4140 Sagitarii in quiescence and in outburst
• Long time-scale variability in GRS1915+105