NUMERICAL SIMULATION OF PRIMARY PROTOSTELLAR DISK FORMATION

The formation of primary disks during the collapse of magnetized ro-tating cores of molecular clouds (protostellar clouds) is investigated us-ing numerical magnetohasodynamic (MHD) modeling. Primary disks are optically thin end are in state of quasi-magnetostatic equilibrium. They form at the initial stages of isothermal collapse mainly along the magnetic field lines. The sizes, masses and angular momentums of primary disks are determined. Calculations show that, at the time of formation of an optically opaque protostellar disk, the size of the primary disk is 5 000—19 000 AU, and the mass is about 1 % of the initial mass of the cloud.