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Astron. Astrophys. 324, 1046-1058 (1997)

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Radiative shocks in atomic and molecular stellar-like atmospheres

VIII. A self-consistent comprehensive model

E. Huguet and J.-P.J. Lafon

1 Observatoire de Paris, DASGAL/UMR 335 C.N.R.S., F-92195 Meudon Cedex, France

Received 7 June 1996 / Accepted 7 October 1996


This paper is devoted to the modelling of radiative shock waves propagating through a stellar-like atmosphere; that is a collisional atomic and molecular hydrogen gas with temperature and density ranges [FORMULA], and [FORMULA]. Such ambient conditions are typical of those found in inner circumstellar envelopes of cool pulsating evolved stars.

The model describes a one dimensional steady-state radiative shock wave. The radiative coupling between the precursor (pre-shocked gas) and the wake (post-shocked gas) is fully self-consistent. It takes into account three radiations: the Lyman- [FORMULA] line, the Lyman continuum and the Balmer continuum, without any ETL assumption.

The wake is described up to the region in which the Balmer continuum flux is produced at about [FORMULA] behind the shock front.

Although the present paper completes the previous Papers of this series we write it as self-contained as possible in order to give a concise but global view of our investigations on radiative shock waves.

Key words: hydrodynamics – radiative transfer – shock waves – circumstellar matter – stars: mass loss – stars: AGB, post-AGB

Send offprint requests to: E. Huguet


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© European Southern Observatory (ESO) 1997

Online publication: May 5, 1998