Multiwavelength studies of MHD waves in the solar chromosphere: An overview of recent results

TL;DR

This paper reviews recent high-resolution observations and theoretical advances in understanding MHD waves in the solar chromosphere, highlighting their role in energy transfer and heating of the solar atmosphere.

Contribution

It provides a comprehensive overview of recent observational and theoretical progress in characterizing MHD waves and their energetics in the solar chromosphere.

Findings

High-resolution observations reveal diverse oscillatory phenomena.

Advances in MHD wave theory enhance understanding of energy transfer.

Waves significantly contribute to chromospheric and coronal heating.

Abstract

The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool photosphere and the intensely heated transition region and corona. Compressible and incompressible waves propagating through the chromosphere can supply significant amounts of energy to the interface region and corona. In recent years an abundance of high-resolution observations from state-of-the-art facilities have provided new and exciting ways of disentangling the characteristics of oscillatory phenomena propagating through the dynamic chromosphere. Coupled with rapid advancements in magnetohydrodynamic wave theory, we are now in an ideal position to thoroughly investigate the role waves play in supplying energy to sustain chromospheric and coronal heating. Here, we review the recent progress made in characterising, categorising and interpreting oscillations manifesting in the solar chromosphere, with an impetus placed on their intrinsic energetics.