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Astron. Astrophys. 324, 1046-1058

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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

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 1000 K < T <5000 K, 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 100 km 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

© European Southern Observatory (ESO) 1997