The equilibria of rotating isothermal clouds

Details The equilibria of rotating isothermal clouds The equilibria of rotating isothermal clouds

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..830k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 15, 1987, p. 830-845.

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33

Interstellar Gas, Isothermal Processes, Molecular Clouds, Nebulae, Rotating Fluids, Angular Momentum, Angular Velocity, Gas Density, Velocity Distribution

Scientific paper

The effect of rotation on the equilibrium structure of an axisymmetric isothermal gas cloud embedded in a stationary external medium is investigated by means of numerical simulations. The underlying assumptions, basic equations, input parameters, and numerical approach are explained, and the results are presented in extensive tables and graphs and characterized in detail. The critical central density and rotation energy, beyond which clouds become unstable to global contraction/expansion and ring formation, respectively, are found to be 800 times the boundary-surface density (BSD) and 0.44 times the gravitational energy. Stable rotating clouds are shown to have maximum mass 31 times that of nonrotating clouds, maximum mean rotation velocity 2.7 times the sound speed, and maximum mean density 6 times BSD. An expression for the maximum height of the boundary surface above the equatorial plane is derived.

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