Self-Gravitational Collapse Of A Slowly Rotating Interstellar Gas Cloud

Details Self-Gravitational Collapse Of A Slowly Rotating Interstellar Gas Cloud Self-Gravitational Collapse Of A Slowly Rotating Interstellar Gas Cloud

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20910516w&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #105.16; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

The results of a computer simulation of the self-gravitational collapse of a slowly rotating interstellar gas cloud are presented. The cloud is modeled as axially symetric, and initially of uniform density. In the data presented the cloud is assumed initially to be in "solid body" rotation with the rotation rate bounded by the balance between gravitational and the maximum centrifugal forces. The model includes the effects of viscosity, and pressure in the vicinity of the forming protostar.

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