The equilibria and evolutions of magnetized, rotating, isothermal clouds. I - Basic equations and numerical methods

Abstract

It is shown that the equilibrium structure of a self-gravitating, magnetized, isothermal cloud with rotation can be solved by the self-consistent field method, like that employed in the pioneering work on a magnetized cloud without rotation by Mouschovious. Clouds are assumed to be axisymmetric and are embedded in a stationary external medium. The equilibrium problem is characterized by four free parameters; the central gas density, the total angular momentum, the total mass, and the magnetic flux. Two free functions, the distributions of specific angular momentum and mass within a cloud, should be given. These six quantities characterize each equilibrium model. Several numerical examples are shown.