Radiative shocks in atomic and molecular stellar atmospheres. IV - Effects of hydrogen recombinations in the precursor

Details Radiative shocks in atomic and molecular stellar atmospheres. IV - Effects of hydrogen recombinations in the precursor Radiative shocks in atomic and molecular stellar atmospheres. IV - Effects of hydrogen recombinations in the precursor

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235..255g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 255-263.

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8

Magnetohydrodynamics, Molecular Clouds, Radiative Transfer, Shock Waves, Stellar Atmospheres, Variable Stars, Computational Astrophysics, Hydrogen Clouds, Ion Recombination, Optical Thickness, Pre-Main Sequence Stars, Shock Fronts, Three Body Problem

Scientific paper

The structure of a radiative precursor of a shock wave propagating in a stellar atmosphere is reexamined. The medium is assumed to be composed only of hydrogen which can be molecular and/or atomic. Both chemical and hydrodynamical processes are taken into account, especially radiative and three-body recombinations of the hydrogen atom. Since this latter is assumed constituted of two levels (fundamental and ionized), only an estimate of the effect of recombinations is possible, although the smallest and largest effects can be exactly computed. Compared to the model without recombinations, recombinations have a fundamental influence on the precursor structure and consequently, on the wake structure, since the whole shock wave structure is given by a self-consistent solution between the precursor and the wake. Thus, precursor recombinations must necessarily be included in a realistic shock wave model when the ionization coefficient at the shock front is around 0.1 depending on the shock front velocity and gas conditions.

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