Solutions for the equilibrium of static isothermal gas clouds with poloidal magnetic fields

Details Solutions for the equilibrium of static isothermal gas clouds with poloidal magnetic fields Solutions for the equilibrium of static isothermal gas clouds with poloidal magnetic fields

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...225..405b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 225, no. 2, Nov. 1989, p. 405-410.

Statistics

Computation

9

Computational Astrophysics, Equilibrium Equations, Interstellar Gas, Interstellar Magnetic Fields, Magnetohydrodynamics, Molecular Clouds, Astronomical Models, Density Distribution, Differential Equations, Poloidal Flux

Scientific paper

A family of semi-analytical solutions for the equilibrium of magnetic self-gravitating gas clouds is presented. The configurations are isothermal and axially symmetric; the frozen-in magnetic field is poloidal. Formulating the equilibrium equations of such gas clouds in spherical polar coordinates, a separation of these equations provides simple representative solutions. The radial part of the density distribution is given by the characteristic inverse square of the radial coordinate. The angular parts are governed by a system of nonlinear ordinary differential equations which is solved numerically. The nonmagnetic limit is the isothermal gas sphere with infinite central density. With increasing field strength the configurations flatten. Besides the isothermal sound velocity the value of the magnetic field in the midplane is a free continuous parameter. In the limit of extremely strong fields a thin disk forms. The existence of bounded solutions is discussed, and the models are compared with configurations presented by other authors.

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