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The Nature of GQ Mus As Depicted From Photoionization Models of the Shell

Published online by Cambridge University Press:  12 April 2016

D. Péquignot  and
C. Morisset
D. Péquignot
Affiliation:
Observatoire de Paris-Meudon, F-92195 Meudon Principal Cedex, France
C. Morisset
Affiliation:
Observatoire de Paris-Meudon, F-92195 Meudon Principal Cedex, France

Extract

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Consequences of a detailed photoionization model study of the shell ejected by Nova Mus 1983 (GQ Mus) are presented for the period from early 1983 to 1990 (Morisset & Péquignot 1996).

The drastic time variation of the emission line spectrum, including the transition from a nebular to a coronal stage in 1986, can be quantitatively understood in terms of a smooth evolution of both the expanding shell and the hot thermal source. This transition is due to a decrease of the shell density with time, and not to an increase of the source effective temperature.

The model shell comprises two components so that not all directions become optically thin to ionizing radiation simultaneously. The range of density and geometrical thickness of the emitting material is of the order of a factor 2.

Type
Novae & Symbiotic Stars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 305 - 306
Copyright
Copyright © Kluwer 1996

References

Morisset, C., Péquignot, D., 1996, A&A, in press.Google Scholar