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Possible X-Ray Flares in a Recurrent Nova

Published online by Cambridge University Press:  12 April 2016

Izumi Hachisu  and
Hiroshi Itoh
Izumi Hachisu
Affiliation:
Department of Aeronautical Engineering, Kyoto University, Kyoto 606, Japan
Hiroshi Itoh
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606, Japan

Abstract:

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The dynamical evolution and nonequilibrium X-ray emission of recurrent nova remnants have been investigated by using a spherically symmetric hydrodynamic code. We assume that the nova ejecta expand into a wind from a red-giant companion. The wind material is blast-shocked, and emits copious X-rays. The blast shock soon breaks out of the wind region and the X-ray emission declines drastically. The blast shock eventually catches up with the relatively slow ejecta of the previous outbursts. The X-ray emission may then be rejuvenated in both luminosity and spectral shape.

Type
4. Related Objects
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 427 - 428
Copyright
Copyright © Springer-Verlag 1990

References

Bode, M.F., and Kahn, F.D. 1985, M. N. R. A. S., 217, 205.CrossRefGoogle Scholar
Itoh, H., and Hachisu, I. 1989, Ap.J., submitted.Google Scholar
Mason, K.O., Córdova, F.A., Bode, M.F., and Ban, P. 1987, in RS Ophiuchi (1985) and the Recurrent Nova Phenomenon, ed. Bode, M.F. (Utrecht: VNU Science Press), p. 167.Google Scholar