Primary disks and their observational appearance in collapsing magnetic rotating protostellar clouds

Abstract

The collapse of the magnetic rotating protostellar cloud with mass of $10M_{\odot }$ is numerically studied. The initial ratios of the thermal, magnetic, and rotational energies of the cloud to the modulus of its gravitational energy are 0.3, 0.2 and 0.01, respectively. The emphasis is on the evolution and properties of the quasi-magnetostatic primary disk formed at the isothermal stage of the collapse. Simulations show that the primary disk size and mass increase during evolution from $1500$ au to $7400$ au and from $0.3M_{\odot }$ to $5.2M_{\odot }$, respectively. Magnetic field is quasi-radial in the cloud envelope and quasi-uniform within the primary disk. A toroidal magnetic field is generated behind the front of the fast shock MHD wave propagating from the primary disk boundary and in the region of the outflow formed near the first hydrostatic core. The hierarchical structure of collapsing protostellar clouds can be revealed in observations in terms of the magnetic field geometry and the angular momentum distribution.

3 pages, 1 figure, published in Bulletin of the Lebedev Physics Institute

References in corpus (4)

• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• Formation and Evolution of Disks around Young Stellar Objects
• A Pseudodisk Threaded with a Toroidal and Pinched Poloidal Magnetic Field Morphology in the HH 211 Protostellar System
• Simulations of the isothermal collapse of magnetic rotating protostellar clouds