Magnetic Reconnection in the Solar Corona

Abstract

Magnetic reconnection, a ubiquitous process in space plasmas, is currently cutting-edge research. This process is usually referred to as the topological reconstruction of the magnetic field in plasmas. Magnetic reconnection in the solar corona has become widely accepted as a key mechanism responsible for the occurrence of solar eruptions such as solar flares and coronal mass ejections. The magnetic energy released in this process is further converted to thermal and kinetic energy which lead to an acceleration of the particles. Hence, research in magnetic reconnection is crucial to better understand the physical mechanisms that trigger solar eruptive events. The present review article particularly focuses on the steady-state MHD theory of slow as well as fast magnetic reconnection and presents observational evidence for magnetic reconnection found in space-based data.

Interactions between Filament Fibrils and a Network Field

“…Dacie et al (2018) analyzed observations of sequential eruptions and argued that the interactions between emerging bipole fields and a quiescent filament were the triggers of the eruptions. Interactions between eruptive filaments and coronal loops are more ubiquitous (Li et al 2017;Kumar & Wang 2019). When an erupting filament encounters the nearby coronal loops, X-type structures usually appear and the magnetic reconnection between the filament and the loops easily leads to changes in the connectivity of filaments (Li et al 2016;Huang et al 2018;Srivastava et al 2019).…”