The equilibria and evolutions of magnetized, rotating, isothermal clouds. V - The effect of the toroidal field

Details The equilibria and evolutions of magnetized, rotating, isothermal clouds. V - The effect of the toroidal field The equilibria and evolutions of magnetized, rotating, isothermal clouds. V - The effect of the toroidal field

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...376..190t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 376, July 20, 1991, p. 190-198.

Other

23

Interstellar Magnetic Fields, Magnetic Field Configurations, Magnetohydrostatics, Molecular Clouds, Star Formation, Equilibrium, Isothermal Processes, Magnetization, Poloidal Flux, Rotation

Scientific paper

The structures of magnetized clouds are studied from a standpoint of magnetohydrostatic equilibrium between the self-gravity and magnetic and thermal pressure forces. Toroidal as well as poloidal magnetic field is taken into account. Poloidal current flowing along the poloidal magnetic field forms a toroidal field which causes the cloud to be pinched toward the symmetric axis. In contrast to the poloidal field, which plays a role in supporting the cloud, the toroidal field has the effect of shrinking the cloud. A cloud that is pinched by the toroidal field but has a low central density often shows a prolate spheroidal shape. With increasing central density the cloud becomes a concaved oblate spheroid. The maximum mass of the cloud supported by magnetic field and thermal pressure decreases with increasing toroidal field strength. Assuming that a cloud encounters a torsional Alfven wave, and the magnetic field begins to be wound up, the cloud begins dynamical collapse if the cloud mass exceeds the marginally supported maximum mass. This indicates a new mode triggering star formation: toroidal field-induced collapse.

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