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

TL;DR

This study numerically investigates the formation and evolution of primary disks in collapsing magnetic rotating protostellar clouds, highlighting magnetic field configurations and observable features during early star formation stages.

Contribution

It provides detailed simulations of primary disk development, magnetic field structures, and their observational signatures in collapsing protostellar clouds.

Findings

Primary disk size increases from 1500 au to 7400 au.

Magnetic field is quasi-radial in the envelope and quasi-uniform in the disk.

A toroidal magnetic field forms behind the shock front.

Abstract

The collapse of the magnetic rotating protostellar cloud with mass of $10\,M_{\odot}$ 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 $0.3\,M_{\odot}$ to $5.2\,M_{\odot}$, 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.