High-resolution wave dynamics in the lower solar atmosphere

TL;DR

This paper reviews recent advances in understanding high-resolution wave dynamics in the lower solar atmosphere, emphasizing observational and modeling challenges, and discusses future prospects with new technologies.

Contribution

It compiles recent research efforts and discusses challenges and future directions in studying wave phenomena in the Sun's lower atmosphere.

Findings

Insights into wave propagation in the chromosphere

Challenges in spectropolarimetry and radiative transfer

Implications for next-generation solar observations

Abstract

The magnetic and convective nature of the Sun's photosphere provides a unique platform from which generated waves can be modelled, observed, and interpreted across a wide breadth of spatial and temporal scales. As oscillations are generated in-situ or emerge through the photospheric layers, the interplay between the rapidly evolving densities, temperatures, and magnetic field strengths provides dynamic evolution of the embedded wave modes as they propagate into the tenuous solar chromosphere. A focused science team was assembled to discuss the current challenges faced in wave studies in the lower solar atmosphere, including those related to spectropolarimetry and radiative transfer in the optically thick regions. Following the Theo Murphy international scientific meeting held at Chicheley Hall during February 2020, the scientific team worked collaboratively to produce 15 independent publications for the current Special Issue, which are introduced here. Implications from the current research efforts are discussed in terms of upcoming next-generation observing and high performance computing facilities.