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Resonant Absorption of Axisymmetric Modes in Twisted Magnetic Flux Tubes

Research paper by Ioannis Giagkiozis, Marcel Goossens, Gary Verth, Viktor Fedun, Tom Van Doorsselaere

Indexed on: 29 Jun '17Published on: 29 Jun '17Published in: arXiv - Astrophysics - Solar and Stellar Astrophysics



Abstract

It has been shown recently that magnetic twist and axisymmetric MHD modes are ubiquitous in the solar atmosphere and therefore, the study of resonant absorption for these modes have become a pressing issue as it can have important consequences for heating magnetic flux tubes in the solar atmosphere and the observed damping. In this investigation, for the first time, we calculate the damping rate for axisymmetric MHD waves in weakly twisted magnetic flux tubes. Our aim is to investigate the impact of resonant damping of these modes for solar atmospheric conditions. This analytical study is based on an idealized configuration of a straight magnetic flux tube with a weak magnetic twist inside as well as outside the tube. By implementing the conservation laws derived by \cite{Sakurai:1991aa} and the analytic solutions for weakly twisted flux tubes obtained recently by \cite{Giagkiozis:2015apj}, we derive a dispersion relation for resonantly damped axisymmetric modes in the spectrum of the Alfv\'{e}n continuum. We also obtain an insightful analytical expression for the damping rate in the long wavelength limit. Furthermore, it shown that both the longitudinal magnetic field and the density, which are allowed to vary continuously in the inhomogeneous layer, have a significant impact on the damping time. Given the conditions in the solar atmosphere, resonantly damped axisymmetric modes are highly likely to be ubiquitous and play an important role in energy dissipation. We also suggest that given the character of these waves, it is likely that they have already been observed in the guise of Alfv\'{e}n waves.