Abstract
A consistent hydrodynamical and radiative transfer calculation in spherical symmetry for a 1M ⊙ protostar is presented. The calculation starts with Larson's 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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Winkler, KH.A. Late stages of solar type protostars. The Moon and the Planets 19, 237–244 (1978). https://doi.org/10.1007/BF00896997
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DOI: https://doi.org/10.1007/BF00896997