MAGNETIC BRAKING DURING STAR FORMATION .2.

A rotating, spherical, uniformly dense cloud of fixed radius R has a frozen-in poloidal magnetic field, symmetric about the rotation axis. The field structure is an idealized version of that resulting from the spherical distortion of a uniform field permeating the uniform infinite medium from which the cloud is supposed to condense. The cloud and its environs are given initial uniform angular velocities Ω and Ω0 respectively. The cloud is also supposed to have an initial toroidal magnetic field of simple structure, chosen so that the magnetic torque on the cloud yields initially a uniform deceleration-Ω. The equations to the interaction between the magnetic and rotation fields are solved, and an expression found for the efflux of angular momentum as a function of (Ω-Ω0), Ω and time. The solution of this set of 'pseudo-problems' provides the tools necessary for attacking the realistic problem of Paper III. © Royal Astronomical Society.