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Dynamics of the Epsilon Aurigae Ring Model

Published online by Cambridge University Press:  30 March 2016

R.E. Wilson  and
W. Van Hamme
R.E. Wilson
Affiliation:
Dept. of Astronomy, University of Florida
W. Van Hamme
Affiliation:
Dept. of Astronomy, U. of Florida and School of Sciences, University of S. Carolina Coastal Carolina College

Extract

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It has recently been suggested (Lissauer and Backman, 1984; Eggleton and Pringle, 1985) that the secondary mass within the Epsilon Aurigae disk is not a single object but an embedded binary. Lissauer and Backman pointed out that this idea would help greatly to account for its low ratio of luminosity to mass, while Eggleton and Pringle argued in addition that the system’s evolution could be much better understood in terms of such a configuration. They also noted that a central opening in a thin disk, which was proposed by one of us (Wilson, 1971) as a means to produce certain unusual features of the eclipse, can be accounted for quite naturally if the disk has a binary at its center. With such an embedded binary, circular orbits will be impossible for particles inside a critical radius, leading to an effective viscosity which will cause disk material to spiral inward.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 7: Highlights of Astronomy. As presented at the XIXth General Assembly of the IAU, 1985 , 1986 , pp. 205 - 206
Copyright
Copyright © Reidel 1986

References

Eggleton, P.P., and Pringle, J.E. 1985, Astrophys. J. 288, 275.Google Scholar
Huang, S. 1965, Astrophys. J. 141, 976.Google Scholar
Lissauer, J.J., and Backman, D.E. 1984, Astrophys. J. Lett. 286, L39.Google Scholar
van de Kamp, P. 1978, Astron. J. 83, 975.Google Scholar
Wilson, R.E. 1971, Astrophys. J. 170, 529.Google Scholar