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The Formation of Preplanetary Disks from the Collapse of Rotating Molecular Cloud CoresSolutions 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.
Document ID
19850015215
Document Type
Other
Authors
Cassen, P.
(NASA Ames Research Center Moffett Field, CA, United States)
Shu, F. H.
(California Univ. Berkeley, United States)
Tereby, S.
(California Univ. Berkeley, United States)
Date Acquired
August 12, 2013
Publication Date
April 1, 1985
Publication Information
Publication: NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984
Subject Category
Lunar And Planetary Exploration
Accession Number
85N23526
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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