On radiative shocks in atomic and molecular stellar atmospheres. II - The precursor structure

Details On radiative shocks in atomic and molecular stellar atmospheres. II - The precursor structure On radiative shocks in atomic and molecular stellar atmospheres. II - The precursor structure

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139..401g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 2, Oct. 1984, p. 401-410. Research supported by the European Southern

Astronomy and Astrophysics

Astrophysics

16

Protostars, Shock Wave Propagation, Stellar Atmospheres, Stellar Models, Atmospheric Models, Hydrogen, Photodissociation, Photoionization, Stellar Temperature

Scientific paper

This paper deals with the problem of determining the structure of the radiative shock precursor in dense (1015-1021 particles per m3), cool (500 - 5000K) atomic and molecular media such as protostars and cool pulsating stars. The medium is assumed to consist of hydrogen only. A one-photon and one-temperature precursor model, taking into account cooling by dissociation and ionization and heating by incident photon flux, is presented. An analytical solution in Lagrangian space is given for chemical and transfer equations. It is shown that the heating clearly dominates the cooling. The variation of the mass density is only of a few per cent whereas the temperature can be multiplied by a factor of a few units.

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