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Shock-heated gas in the outbursts of classical novae

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Abstract

We present a simple model for interactions between the slow and fast phases of mass ejection in classical nova outbursts. A situation develops in which a layer of hot gas sandwiched between two shocks progresses through the slow wind until it ‘blows-out’, expanding and cooling adiabatically. We calculate the X-ray emission from this model and find that the dynamical timescale is at least as important as the radiative cooling time in determining the form of the X-ray light curves. Models of this type may help to explain the origin of X-ray emission in some classical nova outbursts.

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Authors and Affiliations

  1. Computing and Mathematical Sciences, Liverpool John Moores University, Byrom Street, L3 3AF, Liverpool, UK

    T. J. O'Brien

  2. Chemical and Physical Sciences, Liverpool John Moores University, Byrom Street, L3 3AF, Liverpool, UK

    H. M. Lloyd

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  1. T. J. O'Brien
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  2. H. M. Lloyd
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This author is supported by the SERC

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O'Brien, T.J., Lloyd, H.M. Shock-heated gas in the outbursts of classical novae. Astrophys Space Sci 216, 167–172 (1994). https://doi.org/10.1007/BF00982490

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