Abstract
A model is proposed for the interpretation of the extended phase of soft X-ray emission observed for Nova GQ Muscae 1983. It is argued that such a phase is a forced consequence of the evolution of classical novae in outburst (MacDonald, Fujimoto, & Truran 1985). The early appearance of the soft X-ray emission (Ögelman, Krautter, & Beuermann 1987) is interpreted to be a consequence of common envelope (CE) driven mass loss, occurring over the first few hundred days of the nova outburst. The subsequent turn-off of GQ Muscae as a soft X-ray source occurred between early 1992 and late 1993. The approximately 10 year phase of soft X-ray emission thus defined is found to be consistent with the nuclear burning timescale for the exhaustion of the residual (post common envelope phase) hydrogen envelope on a 1 M ⊙ white dwarf, in a binary system of period 85.5 s (Diaz & Steiner 1989).
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Truran, J.W., Glasner, S.A. (1995). On the Nature of the Soft X-Ray Emission from Nova GQ Muscae 1983. In: Bianchini, A., Valle, M.D., Orio, M. (eds) Cataclysmic Variables. Astrophysics and Space Science Library, vol 205. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0335-0_123
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DOI: https://doi.org/10.1007/978-94-011-0335-0_123
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