Attenuation of small-amplitude oscillations in a prominence-corona model with a transverse magnetic field

TL;DR

This study investigates how thermal conduction and radiative losses damp small-amplitude magnetoacoustic waves in a prominence-corona system with a transverse magnetic field, revealing different damping efficiencies for slow and fast modes.

Contribution

It provides a detailed numerical analysis of wave damping mechanisms in prominence models with transverse magnetic fields, highlighting the dominant roles of thermal conduction and radiative losses.

Findings

Coronal thermal conduction and radiative losses are key damping mechanisms.

Slow modes are efficiently damped with times matching observations.

Fast modes are less damped, with damping times much longer than observed.

Abstract

Small-amplitude prominence oscillations are usually damped after a few periods. We study the attenuation of non-adiabatic magnetoacoustic waves in a slab prominence embedded in the coronal medium. We assume an equilibrium configuration with a transverse magnetic field to the slab axis and investigate wave damping by thermal conduction and radiative losses. The differential MHD equations that govern linear slow and fast modes are numerically solved to obtain the complex oscillatory frequency and the corresponding eigenfunctions. We find that coronal thermal conduction and radiative losses from the prominence plasma reveal as the most relevant damping mechanisms. Both mechanisms govern together the attenuation of hybrid modes, whereas prominence radiation is responsible for the damping of internal modes and coronal conduction essentially dominates the attenuation of external modes. In addition, the energy transfer between the prominence and the corona caused by thermal conduction has a noticeable effect on the wave stability, radiative losses from the prominence plasma being of paramount importance for the thermal stability of fast modes. We conclude that slow modes are efficiently damped, with damping times compatible with observations. On the contrary, fast modes are less attenuated by non-adiabatic effects and their damping times are several orders of magnitude larger than those observed. The presence of the corona causes a decrease of the damping times with respect to those of an isolated prominence slab, but its effect is still insufficient to obtain damping times of the order of the period in the case of fast modes.