Late stages of solar type protostars

Details Late stages of solar type protostars Late stages of solar type protostars

Oct 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978m%26p....19..237w&link_type=abstract

(Conference on Protostars and Planets, Tucson, Ariz., Jan. 3-7, 1978.) Moon and the Planets, vol. 19, Oct. 1978, p. 237-244.

Physics

4

Protostars, Solar System, Stellar Atmospheres, Stellar Evolution, Boundary Value Problems, Convective Flow, Cores, Gravitational Collapse, Magnetohydrodynamics, Radiative Transfer, Stellar Luminosity, Stellar Structure

Scientific paper

A consistent hydrodynamical and radiative-transfer calculation in spherical symmetry for a 1-solar-mass protostar is presented. The calculation starts with Larson's (1969) initial conditions and continues until almost all the material has fallen onto a hydrostatic core with a large outer convection zone. The innermost percent of the mass is partially degenerate. Due to the numerical technique used, the radius of the hydrostatic core is determined with a high degree of accuracy.

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