Propagation and dispersion of sausage wave trains in magnetic flux tubes

TL;DR

This paper investigates how localized perturbations generate dispersive sausage wave trains in magnetic flux tubes, analyzing the effects of physical properties and initial conditions on wave propagation and dispersion.

Contribution

It extends previous work by examining axisymmetric perturbations and highlights how initial perturbation length and density ratios influence wave train characteristics.

Findings

Long initial perturbations produce low amplitude wave packets.

Higher density ratios result in longer wave trains.

Wave dispersion depends on group velocity and physical properties.

Abstract

A localized perturbation of a magnetic flux tube produces a pair of wave trains that propagate in opposite directions along the tube. These wave packets disperse as they propagate, where the extent of dispersion depends on the physical properties of the magnetic structure, on the length of the initial excitation, and on its nature (e.g., transverse or axisymmetric). In Oliver et al. (2014) we considered a transverse initial perturbation, whereas the temporal evolution of an axisymmetric one is examined here. In both papers we use a method based on Fourier integrals to solve the initial value problem. Previous studies on wave propagation in magnetic wave guides have emphasized that the wave train dispersion is influenced by the particular dependence of the group velocity on the longitudinal wavenumber. Here we also find that long initial perturbations result in low amplitude wave packets and that large values of the magnetic tube to environment density ratio yield longer wave trains. To test the detectability of propagating transverse or axisymmetric wave packets in magnetic tubes of the solar atmosphere (e.g., coronal loops, spicules, or prominence threads) a forward modelling of the perturbations must be carried out. This is left for a future work.