Theory of magnetic reconnection in solar and astrophysical plasmas

TL;DR

This paper reviews the current understanding of magnetic reconnection in solar and astrophysical plasmas, covering theoretical models, 3D effects, kinetic and MHD regimes, and observational evidence.

Contribution

It provides a comprehensive overview of recent advances in modeling and understanding magnetic reconnection in complex 3D and kinetic frameworks, highlighting new regimes and observational support.

Findings

Identification of new 3D reconnection regimes

Evidence from solar system plasma observations

Theoretical distinctions between 2D and 3D reconnection

Abstract

Magnetic reconnection is a fundamental process in a plasma that facilitates the release of energy stored in the magnetic field by permitting a change in the magnetic topology. In this article we present a review of the current state of understanding of magnetic reconnection. We discuss theoretical results regarding the formation of current sheets in complex 3D magnetic fields, and describe the fundamental differences between reconnection in two and three dimensions. We go on to outline recent developments in modelling of reconnection with kinetic theory, as well as in the MHD framework where a number of new 3D reconnection regimes have been identified. We discuss evidence from observations and simulations of solar system plasmas that support this theory, and summarise some prominent locations in which this new reconnection theory is relevant in astrophysical plasmas.