The solar corona as an active medium for magnetoacoustic waves

TL;DR

This paper explores how thermal misbalance in the solar corona acts as an active medium for magnetoacoustic waves, affecting their damping, amplification, and dispersion, and proposes using wave observations to probe coronal heating mechanisms.

Contribution

It introduces the concept of the corona as an active medium due to thermal misbalance and analyzes its effects on slow-mode magnetoacoustic waves, including damping, amplification, and dispersion.

Findings

Thermal misbalance causes frequency-dependent damping or amplification of slow waves.

The corona's active medium nature affects wave dispersion independently of plasma non-uniformity.

Wave observations can potentially reveal details of the coronal heating function.

Abstract

The presence and interplay of continuous cooling and heating processes maintaining the corona of the Sun at the observed one million K temperature were recently understood to have crucial effects on the dynamics and stability of magnetoacoustic waves. These essentially compressive waves perturb the coronal thermal equilibrium, leading to the phenomenon of a wave-induced thermal misbalance. Representing an additional natural mechanism for the exchange of energy between the plasma and the wave, thermal misbalance makes the corona an active medium for magnetoacoustic waves, so that the wave can not only lose but also gain energy from the coronal heating source (similarly to burning gases, lasers and masers). We review recent achievements in this newly emerging research field, focussing on the effects that slow-mode magnetoacoustic waves experience as a back-reaction of this perturbed coronal thermal equilibrium. The new effects include enhanced frequency-dependent damping or amplification of slow waves, and effective, not associated with the coronal plasma non-uniformity, dispersion. We also discuss the possibility to probe the unknown coronal heating function by observations of slow waves and linear theory of thermal instabilities. The manifold of the new properties that slow waves acquire from a thermodynamically active nature of the solar corona indicate a clear need for accounting for the effects of combined coronal heating/cooling processes not only for traditional problems of the formation and evolution of prominences and coronal rain, but also for an adequate modelling and interpretation of magnetohydrodynamic waves.