Convective accretion disks and the onset of dwarf nova outbursts

Journal Article · Wed Sep 15 04:00:00 EDT 1982 · Astrophys. J., Lett. Ed.; (United States)

DOI:https://doi.org/10.1086/183875· OSTI ID:6577245

Cannizzo, J K; Ghosh, P; Wheeler, J C

We have constructed vertically integrated, steady state convective models of accretion disks to explore the mechanism of instability in dwarf novae. The models and observations of dwarf novae suggest a picture in which transferred matter piles up in an optically thin torus. The torus eventually becomes optically thick and the resulting convective structure is thermally unstable. Matter then flows inward, and the sudden conversion of gravitational potential energy to radiation is identified as the dwarf nova outburst. At sufficiently high mass accretion rates, the inflow is continuous.

• Research Organization: Department of Astronomy, The University of Texas at Austin
• OSTI ID: 6577245
• Journal Information: Astrophys. J., Lett. Ed.; (United States), Journal Name: Astrophys. J., Lett. Ed.; (United States) Vol. 260:2; ISSN AJLEA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CONVECTION
ERUPTIVE VARIABLE STARS
INSTABILITY
MATHEMATICAL MODELS
NOVAE
STAR ACCRETION
STAR EVOLUTION
STAR MODELS
STARS
STEADY-STATE CONDITIONS
VARIABLE STARS