Physics
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pggp.rept..143c&link_type=abstract
In NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984 p 143-145 (SEE N85-23474 13-91)
Physics
Disk Galaxies, Molecular Clouds, Planetary Evolution, Protoplanets, Stellar Evolution, Stellar Mass, Cosmic Dust, Hydrodynamic Equations, Planetary Nebulae, Planetary Rotation
Scientific paper
Solutions that describe the collapse of a molecular cloud core that is initially in unstable equilibrium, embedded within an envelope of uniform density, and rotating at the same rate as the envelope are given. Hydrodynamic equations, including self gravity, are deduced to a set of ordinary differential equations, which are solved by the method of matched asymptotic expansions. Results of these calculations are: (1) the range of stellar masses derived seems to correspond to realistic ranges of observed stellar masses and interstellar cloud parameters, (2) the proper measure of dissipation rate is the ratio of accretion time to viscous diffusion time, and (3) the pressure distribution on the surface of an accreting protostar is nonuniform in a way that favors the channeling of a stellar wind into a bipolar flow directed along the rotation axis.
Cassen Pat
Shu Frank H.
Terebey Susan
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