Equilibrium structures of rotating isothermal gas clouds. II - Dependence on the angular momentum distribution

Details Equilibrium structures of rotating isothermal gas clouds. II - Dependence on the angular momentum distribution Equilibrium structures of rotating isothermal gas clouds. II - Dependence on the angular momentum distribution

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...147...13h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 147, no. 1, June 1985, p. 13-21.

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3

Angular Momentum, Equilibrium Equations, Interstellar Gas, Isothermal Processes, Molecular Clouds, Rotating Fluids, Gas Density, Gravitational Collapse, Stellar Evolution, Stellar Rotation

Scientific paper

Using a thin disk approximation model, the authors have computed equilibrium sequences of rotating isothermal gas clouds with angular momentum distributions jr = (1+ɛ)(J/M){1-(1-Mr/M)1/ɛ}. Here M is the total mass, J the total angular momentum, Mr the mass within the cylindrical radius r, and jr, the specific angular momentum at r. Three cases (ɛ = 2, 1, and 1/2) have been computed (a uniformly rotating homogeneous sphere corresponds to ɛ = 3/2). There are two phases which are stable against the compression mode - a pressure dominant phase and a rotation dominant phase for all angular momentum distributions. When ɛ ≥ 1, there exist equilibria with infinite central density, however, when ɛ = 1/2, a ring structure appears in the rotation dominant phase. When a spherical homogeneous isothermal gas cloud, which is not in equilibrium, is considered, the cloud will begin to collapse.

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