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Magnetic Reconnection in the Solar Corona

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. © 2019 BBSCS RN SWS. All rights reserved