Abstract
Alfvén waves are considered to be viable transporters of the non-thermal energy required to heat the Sun’s quiescent atmosphere. An abundance of recent observations, from state-of-the-art facilities, have reported the existence of Alfvén waves in a range of chromospheric and coronal structures. Here, we review the progress made in disentangling the characteristics of transverse kink and torsional linear magnetohydrodynamic (MHD) waves. We outline the simple, yet powerful theory describing their basic properties in (non-)uniform magnetic structures, which closely resemble the building blocks of the real solar atmosphere.
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Acknowledgements
D.B.J. thanks the Science and Technology Facilities Council (STFC) for a Post-Doctoral Fellowship. R.E. acknowledges M. Kéray for patient encouragement and is grateful to NSF Hungary (OTKA K83133). R.E. also thanks for the hospitality received at the Dept. of Astronomy, Eőtvős University, Budapest, Hungary, where part of his contribution to the review paper was developed. We would like to thank the anonymous referees for their comments and suggestions on the manuscript.
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Mathioudakis, M., Jess, D.B. & Erdélyi, R. Alfvén Waves in the Solar Atmosphere. Space Sci Rev 175, 1–27 (2013). https://doi.org/10.1007/s11214-012-9944-7
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DOI: https://doi.org/10.1007/s11214-012-9944-7