Collapse, outflows and fragmentation of massive, turbulent and magnetized prestellar barotropic cores

TL;DR

This study uses high-resolution MHD simulations to explore how magnetic fields influence the collapse, outflows, and fragmentation of massive, turbulent prestellar cores, revealing significant magnetic effects on star formation processes.

Contribution

It provides new insights into the role of magnetic fields in massive core collapse, including their impact on angular momentum, outflows, and fragmentation, using advanced numerical simulations.

Findings

Magnetic braking reduces angular momentum significantly.

Episodic outflows with velocities up to 40 km/s are launched.

Magnetized clouds show less fragmentation compared to hydrodynamical ones.

Abstract

Stars and more particularly massive stars, have a drastic impact on galaxy evolution. Yet the conditions in which they form and collapse are still not fully understood. In particular, the influence of the magnetic field on the collapse of massive clumps is relatively unexplored, it is thus of great relevance in the context of the formation of massive stars to investigate its impact. We perform high resolution, MHD simulations of the collapse of hundred solar masses, turbulent and magnetized clouds, using the adaptive mesh refinement code RAMSES. We compute various quantities such as mass distribution, magnetic field and angular momentum within the collapsing core and study the episodic outflows and the fragmentation that occurs during the collapse. The magnetic field has a drastic impact on the cloud evolution. We find that magnetic braking is able to substantially reduce the angular momentum in the inner part of the collapsing cloud. Fast and episodic outflows are being launched with typical velocities of the order of 3-5 km s$^{-1}$ although the highest velocities can be as high as 30-40 km s$^{-1}$. The fragmentation in several objects, is reduced in substantially magnetized clouds with respect to hydrodynamical ones by a factor of the order of 1.5-2. We conclude that magnetic fields have a significant impact on the evolution of massive clumps. In combination with radiation, magnetic fields largely determine the outcome of massive core collapse. We stress that numerical convergence of MHD collapse is a challenging issue. In particular, numerical diffusion appears to be important at high density therefore possibly leading to an over-estimation of the number of fragments.