Protostellar evolution. I - The behaviour of the Eddington factor and the accretion shock

Details Protostellar evolution. I - The behaviour of the Eddington factor and the accretion shock Protostellar evolution. I - The behaviour of the Eddington factor and the accretion shock

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...200...58b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 200, no. 1-2, July 1988, p. 58-74.

Astronomy and Astrophysics

Astrophysics

25

Protostars, Stellar Evolution, Stellar Mass Accretion, Pre-Main Sequence Stars, Radiative Transfer, Shock Fronts, Stellar Temperature, Thermodynamic Properties, Time Dependence

Scientific paper

This paper presents a sequence of spherically symmetric models of a collapsing protostellar cloud of 1 solar mass, including realistic thermodynamics and a simultaneous solution of the grey but time-dependent radiation transfer equation (RTE). The initial configuration was chosen, on the basis of the findings of Tscharnuter (1987), to have a constant density of 3.75 x 10 to the -15th g/cu cm. Special attention is given to the behavior of the Eddington factor. Three physical reasons were found for the Eddington factor to drop below 1/3. Late in the accretion phase, the occurrence of shock front instabilities is shown to occur.

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