Abstract
A non-ideal MHD collapse calculation employing the axisymmetric thin-disk approximation is used to resolve cloud core collapse down to the scales of the second (stellar) core. Rotation and a magnetic braking torque are included in the model, and the partial ionization resulting in ambipolar diffusion and Ohmic dissipation is calculated from a detailed chemical network. We find that a centrifugal disk can indeed form in the earliest stage of star formation, due to a shut-off of magnetic braking caused by magnetic field diffusion in the first core region. Thus, there is no catastrophic magnetic braking in a model with realistic non-ideal MHD.
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