Equilibrium structures of rotating isothermal gas clouds. I

Details Equilibrium structures of rotating isothermal gas clouds. I Equilibrium structures of rotating isothermal gas clouds. I

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...143..355h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 143, no. 2, Feb. 1985, p. 355-364.

Statistics

Computation

14

Astronomical Models, Computational Astrophysics, Equilibrium, Interstellar Gas, Protostars, Rotating Matter, Density Distribution, Gravitational Collapse, Newton-Raphson Method

Scientific paper

A disk model is used to describe equilibrium conditions for collapsing gas clouds in order to determine the central density and the mass range of clouds which produce solar-type systems. A Newton-Raphson approach is taken, and it is assumed that a plane-parallel solution is sufficient for the flat cloud and the gravitational force is derivable from planar mass distribution. Rotationally and pressure dominated equilibrium phases are identified, with the central density being infinitely large in the former. The cloud fragments as it collapses, forming a protostar surrounded by a rotating disk, provided certain bounds are extant on the ratio of the thermal to gravitational energy.

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