Abstract
The AM CVn stars are mass transferring, interacting binary, white dwarf systems with orbital periods of 15…45 minutes. Hydrogen is completely lost from these systems, and we observe small helium disks which may show thermal and tidal instabilities if the mass transfer rate is large enough (Osaki 1995). A tidal instability brings the disk into a superoutburst state, and in the light curve we may observe superhumps.
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© 1996 Kluwer Academic Publishers
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Solheim, JE. (1996). Non Circular Disks in AM CVn Systems?. In: Evans, A., Wood, J.H. (eds) Cataclysmic Variables and Related Objects. Astrophysics and Space Science Library, vol 208. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0325-8_40
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DOI: https://doi.org/10.1007/978-94-009-0325-8_40
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-6632-7
Online ISBN: 978-94-009-0325-8
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