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Magnetism and Dynamics of Prominences: MHD Waves

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Solar Prominences

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 415))

Abstract

Quiescent solar prominences are highly dynamic structures which, among other features, display oscillatory motions. The presence of these oscillations has been confirmed by means of ground- and space-based observations, and they have been classified in small and large amplitude oscillations. Since prominences are magnetized structures, the theoretical interpretation of their oscillations has been mostly done in terms of magnetohydrodynamic (MHD) waves. This interpretation has allowed the development of prominence seismology as a tool to determine prominence physical parameters (magnetic field, Alfvén speed, inhomogeneity scale, etc.) which are difficult to measure by direct means.

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Acknowledgements

This chapter is dedicated to the memory of Josip Kleczek who woke up my interest for solar prominences.

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  1. Departament de Física, Universitat de les Illes Balears, E-07122, Palma de Mallorca, Spain

    José Luis Ballester

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Correspondence to José Luis Ballester .

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  1. Université Paris-Sud 11, Institute of Astrophysics Space, Orsay, France

    Jean-Claude Vial

  2. University of Oslo, Blindern, Institute of Theoretical Astrophysics, Oslo, Norway

    Oddbjørn Engvold

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Ballester, J.L. (2015). Magnetism and Dynamics of Prominences: MHD Waves. In: Vial, JC., Engvold, O. (eds) Solar Prominences. Astrophysics and Space Science Library, vol 415. Springer, Cham. https://doi.org/10.1007/978-3-319-10416-4_11

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