Abstract
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.
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© 1993 Springer Science+Business Media Dordrecht
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Osaki, Y., Hirose, M., Ichikawa, S. (1993). A Unified Model of Dwarf Nova Outbursts Based on the Disk Instability. In: Takeuti, M., Buchler, JR. (eds) Nonlinear Phenomena in Stellar Variability. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1062-4_58
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DOI: https://doi.org/10.1007/978-94-011-1062-4_58
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