Computer Science – Numerical Analysis
Scientific paper
Aug 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...200...48w&link_type=abstract
Astrophysical Journal, vol. 200, Aug. 15, 1975, pt. 1, p. 48-60. AEC-sponsored research.
Computer Science
Numerical Analysis
32
Astronomical Models, Protostars, Stellar Evolution, Stellar Motions, Difference Equations, Energy Transfer, Gravitational Collapse, Hydrodynamics, Numerical Analysis
Scientific paper
A numerical scheme is developed in which rapid dynamic motion in one part of a protostar and quasi-static evolution in another part can be calculated simultaneously. Based on this technique, the evolution of spherically symmetric protostars with initial masses between 0.1 and 50 solar masses is investigated. The general evolutionary features are found to be similar to those of previous models, but the final hydrostatic-equilibrium configurations have large radii as compared to Larson's (1973) protostar models. It is found for low-mass protostars that the luminosity remains relatively low until late evolutionary stages and that evolution is very sensitive to the treatment of convective energy transport. For high-mass protostars, it is found that a convective phase never exists and that a fraction of the initial mass is ejected due to heating and radiation pressure in the envelope. Detailed numerical results are given for a protostar with 1 solar mass, and some observational implications of this work are discussed.
Tarter Bruce C.
Westbrook C. K.
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