MHD turbulence-Star Formation Connection: from pc to kpc scales

TL;DR

This paper reviews how MHD turbulence and turbulent magnetic reconnection facilitate magnetic flux transport in star-forming regions, potentially surpassing ambipolar diffusion in efficiency, with implications across various astrophysical scales.

Contribution

It highlights the role of turbulent reconnection in magnetic flux diffusion during star formation, supported by recent 3D simulations, offering a new perspective beyond traditional ambipolar diffusion.

Findings

Turbulent reconnection efficiently diffuses magnetic fields in star-forming clouds.

Simulations show magnetic flux transport is faster with turbulence than with ambipolar diffusion.

The turbulence-star formation connection extends from galactic to cluster scales.

Abstract

The transport of magnetic flux to outside of collapsing molecular clouds is a required step to allow the formation of stars. Although ambipolar diffusion is often regarded as a key mechanism for that, it has been recently argued that it may not be efficient enough. In this review, we discuss the role that MHD turbulence plays in the transport of magnetic flux in star forming flows. In particular, based on recent advances in the theory of fast magnetic reconnection in turbulent flows, we will show results of three-dimensional numerical simulations that indicate that the diffusion of magnetic field induced by turbulent reconnection can be a very efficient mechanism, especially in the early stages of cloud collapse and star formation. To conclude, we will also briefly discuss the turbulence-star formation connection and feedback in different astrophysical environments: from galactic to cluster of galaxy scales.