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Plasma Structure and Dynamics

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Solar Prominences

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

Abstract

Despite over a century of observations, the physical processes by which prominence plasma forms and evolves remain controversial. In this chapter we review the observational constraints on all mass formation models, review the four leading models—injection, levitation, evaporation–condensation, and magneto-thermal convection, describe the strengths and weaknesses of each model, and point out opportunities for future work. As needed, short tutorials are provided on fundamental physical mechanisms and concepts not covered in other chapters, including magnetic reconnection and energy balance in coronal loops.

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Acknowledgments

JK would like to thank S. Antiochos, T. Berger, C.R. DeVore, S. Guidoni, J. Leake, W. Liu, M. Luna Benassar, and E. Zweibel for their helpful suggestions and comments.

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  1. NASA Goddard Space Flight Center, Code 671, Greenbelt, MD, 20771, USA

    Judith T. Karpen

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  1. Judith T. Karpen
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Correspondence to Judith T. Karpen .

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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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Karpen, J.T. (2015). Plasma Structure and Dynamics. 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_10

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