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MHD Equilibria and Triggers for Prominence Eruption

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Solar Prominences

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

Abstract

Magneto-hydrodynamic (MHD) simulations of the emergence of twisted magnetic flux tubes from the solar interior into the corona are discussed to illustrate how twisted and sheared coronal magnetic structures (with free magnetic energy), capable of driving filament eruptions, can form in the corona in emerging active regions. Several basic mechanisms that can disrupt the quasi-equilibrium coronal structures and trigger the release of the stored free magnetic energy are discussed. These include both ideal processes such as the onset of the helical kink instability and the torus instability of a twisted coronal flux rope structure and the non-ideal process of the onset of fast magnetic reconnections in current sheets. Representative MHD simulations of the non-linear evolution involving these mechanisms are presented.

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Acknowledgements

The author would like to thank Fang Fang, Terry Forbes, Judy Karpen, Zoran Mikic, Slava Titov, and Tibor Török for granting permission to reprint Figures from their original publications. The National Center for Atmospheric Research is sponsored by the National Science Foundation.

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  1. National Center for Atmospheric Research, 3080 Center Green Dr., Boulder, CO, 80301, USA

    Yuhong Fan

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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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Fan, Y. (2015). MHD Equilibria and Triggers for Prominence Eruption. 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_12

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