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The Dynamics of Eruptive Prominences

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Solar Prominences

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

Abstract

This chapter discusses the dynamical properties of eruptive prominences in relation to coronal mass ejections (CMEs). The fact that eruptive prominences are a part of CMEs is emphasized in terms of their physical association and kinematics. The continued propagation of prominence material into the heliosphere is illustrated using in-situ observations. The solar-cycle variation of eruptive prominence locations is discussed with a particular emphasis on the rush-to-the-pole (RTTP) phenomenon. One of the consequences of the RTTP phenomenon is polar CMEs, which are shown to be similar to the low-latitude CMEs. This similarity is important because it provides important clues to the mechanism by which CMEs erupt. The nonradial motion of CMEs is discussed, including the deflection by coronal holes that have important space weather consequences. Finally, the implications of the presented observations for CME modeling are outlined.

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Acknowledgments

I thank the editors, Oddbjørn Engvold and Jean-Claude Vial, for inviting this contribution. I thank David Webb, Pertti Mäkelä, Sarah Gibson, Ronald Moore, and Alphonse Sterling for helpful comments. I also thank S. Yashiro, S. Akiyama, and P. Mäkelä for their help with the figures. Work supported by NASA’s LWS TR&T program.

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

    Nat Gopalswamy

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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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Gopalswamy, N. (2015). The Dynamics of Eruptive Prominences. 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_15

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