Fundamental Physical Processes in Coronae: Waves, Turbulence, Reconnection, and Particle Acceleration

TL;DR

This paper reviews recent observational advances in understanding the fundamental physical processes in the solar corona, including waves, turbulence, reconnection, and particle acceleration, based on space-based observations across multiple wavelengths.

Contribution

It synthesizes key observational findings from various space missions to enhance understanding of coronal physics and related plasma processes.

Findings

Detection of acoustic and MHD waves in the corona

Observation of turbulence-related line broadening

Identification of magnetic configurations associated with reconnection

Abstract

Our understanding of fundamental processes in the solar corona has been greatly progressed based on the space observations of SMM, Yohkoh, Compton GRO, SOHO, TRACE, RHESSI, and STEREO. We observe now acoustic waves, MHD oscillations, turbulence-related line broadening, magnetic configurations related to reconnection processes, and radiation from high-energy particles on a routine basis. We review a number of key observations in EUV, soft X-rays, and hard X-rays that innovated our physical understanding of the solar corona, in terms of hydrodynamics, MHD, plasma heating, and particle acceleration processes.