Reconnection Diffusion and Star Formation

TL;DR

This paper discusses how turbulence-induced magnetic reconnection facilitates magnetic field diffusion in astrophysical environments, supporting star formation models by enabling magnetic flux removal from clouds and cores.

Contribution

It provides evidence that reconnection diffusion, driven by turbulence, is a key process in magnetic flux removal during star formation, supported by recent MHD simulations.

Findings

Magnetic reconnection in turbulence enables efficient magnetic flux removal.

Simulations show reconnection diffusion aligns with observed star formation processes.

Supports the concept that turbulence enhances magnetic field diffusion in astrophysics.

Abstract

The diffusion of astrophysical magnetic fields in conducting fluids in the presence of turbulence depends on whether magnetic fields can change their topology or reconnect in highly conducting media. Recent progress in understanding fast magnetic reconnection in the presence of turbulence is reassuring that the magnetic field behavior in computer simulations and turbulent astrophysical environments is similar, as far as the magnetic reconnection is concerned. This makes it meaningful to perform MHD simulations of turbulent flows in order to understand the diffusion of magnetic field in astrophysical environments. These simulations support the concept of reconnection diffusion, which describes the ability of magnetic fields to get removed from magnetized clouds and cores in the process of star formation.