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A Unified Model of Dwarf Nova Outbursts Based on the Disk Instability

Published online by Cambridge University Press:  12 April 2016

Y. Osaki ,
M. Hirose  and
S. Ichikawa
Y. Osaki
Affiliation:
Department of Astronomy, Faculty of Science, The University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
M. Hirose
Affiliation:
Department of Astronomy, Faculty of Science, The University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
S. Ichikawa
Affiliation:
Department of Astronomy, Faculty of Science, The University of Tokyo, Bunkyo-ku, Tokyo 113, Japan

Abstract

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A unified model for outbursts of dwarf novae is proposed based on the disk instability model in cataclysmic variable stars. In this model, two different intrinsic instabilities (i.e., the thermal instability and the tidal instability) within accretion disks are considered in non-magnetic cataclysmic variable stars. It is suggested that all of three sub-classes of dwarf novae (i.e., U Gem-type, Z Cam-type and SU UMa-type dwarf novae) may be explained in terms of two model parameters of the orbital period of the binary and of the mass transfer rate within the framework of the disk instability model.

Type
III. Models
Information
International Astronomical Union Colloquium , Volume 134: Nonlinear Phenomena in Stellar Variability , 1993 , pp. 359 - 360
Copyright
Copyright © Kluwer 1993

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