The equilibria of rotating, isothermal clouds. I - Method of solution.

Details The equilibria of rotating, isothermal clouds. I - Method of solution. The equilibria of rotating, isothermal clouds. I - Method of solution.

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...268..155s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 268, May 1, 1983, p. 155-184.

Other

30

Gravitational Collapse, Nebulae, Plasma Equilibrium, Protostars, Rotating Fluids, Stellar Evolution, Gravitational Fields, Hydrodynamics, Isothermal Processes, Molecular Clouds, Rotating Spheres, Self Consistent Fields, Toroidal Plasmas, Virial Theorem

Scientific paper

The problem of the axisymmetric collapse of rotating protostellar clouds is considered by investigating the end-product of that collapse, presenting the method for computing isothermal equilibria. The clouds are assumed to have the angular momentum distribution of rigidly rotating, uniform-density spheres of the same mass; magnetic and viscous effects are neglected. The mathematical formulation involves nondimensionalizing the problem in terms of boundary pressure, internal sound speed, and the gravitational constant. The equilibrium configuration is found by solving the equation for momentum balance together with Poisson's equation for the gravitational potential. The computational method is a modified version of the self-consistent field method of Ostriker and Mark (1968). The equilibria can be characterized by two parameters: a dimensionless mass M and the rotational parameter beta. The detailed properties of the equilibria throughout the M-beta plane are given, dynamical stability is discussed, and numerical results for the marginally unstable eigenmodes are presented.

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