MHD wave modes resolved in fine-scale chromospheric magnetic structures

TL;DR

This review discusses recent advances in identifying and analyzing MHD wave modes in fine-scale chromospheric magnetic structures, highlighting their role in solar atmospheric heating and plasma diagnostics.

Contribution

It provides a comprehensive overview of the challenges, methods, and implications of MHD wave mode identification in the chromosphere, including magnetoseismology applications.

Findings

Improved resolution has enabled detailed MHD wave studies in chromospheric structures.

Accurate wave mode identification is crucial for estimating wave energy flux.

Magnetoseismology offers new insights into sub-resolution plasma structuring.

Abstract

Within the last decade, due to significant improvements in the spatial and temporal resolution of chromospheric data, magnetohydrodynamic (MHD) wave studies in this fascinating region of the Sun's atmosphere have risen to the forefront of solar physics research. In this review we begin by reviewing the challenges and debates that have manifested in relation to MHD wave mode identification in fine-scale chromospheric magnetic structures, including spicules, fibrils and mottles. Next we go on to discuss how the process of accurately identifying MHD wave modes also has a crucial role to play in estimating their wave energy flux. This is of cardinal importance for estimating what the possible contribution of MHD waves is to solar atmospheric heating. Finally, we detail how such advances in chromospheric MHD wave studies have also allowed us, for the first time, to implement cutting-edge magnetoseismological techniques that provide new insight into the sub-resolution plasma structuring of the lower solar atmosphere.