MHD Waves in open coronal structures

TL;DR

This review discusses recent advances in the detection, origin, damping, and seismological applications of MHD waves in open coronal structures, highlighting their relevance to coronal heating and solar wind acceleration.

Contribution

It provides a comprehensive overview of recent progress in understanding MHD waves in open coronal structures, including observational, theoretical, and seismological insights.

Findings

Detection of propagating slow magnetoacoustic and kink waves in open coronal structures.

Insights into wave damping mechanisms and their implications for coronal heating.

Potential role of Alfvénic waves in solar wind acceleration.

Abstract

Modern observatories have revealed the ubiquitous presence of magnetohydrodynamic waves in the solar corona. The propagating waves (in contrast to the standing waves) are usually originated in the lower solar atmosphere which makes them particularly relevant to coronal heating. Furthermore, open coronal structures are believed to be the source regions of solar wind, therefore, the detection of MHD waves in these structures is also pertinent to the acceleration of solar wind. Besides, the advanced capabilities of the current generation telescopes have allowed us to extract important coronal properties through MHD seismology. The recent progress made in the detection, origin, and damping of both propagating slow mangetoacoustic waves and kink (Alfv\'{e}nic) waves is presented in this review article especially in the context of open coronal structures. Where appropriate, we give an overview on associated theoretical modelling studies. A few of the important seismological applications of these waves are discussed. The possible role of Aflv\'{e}nic waves in the acceleration of solar wind is also touched upon.