 Numerical Calculations of the Dynamics of a Collapsing Proto-Star by Richard B. Larson

The primary numerical study follows spherical protostellar collapse. A small central core forms before most of the envelope reaches it and subsequently grows by accretion. The abstract also describes infrared reprocessing by the dusty envelope. Spherical symmetry and the chosen radiative and thermodynamic treatment are model assumptions; rotation, magnetic fields and non-spherical accretion require additional physics.