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Radiation hydrodynamics in solar flares

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Radiation Hydrodynamics in Stars and Compact Objects

Part of the book series: Lecture Notes in Physics ((LNP,volume 255))

Abstract

Solar flares are currently undetstood as the explosive release of energy stored in the form of stressed magnetic fields. In many cases, the released energy seems to take the form of large numbers of electrons accelerated to high energies (the nonthermal electron “thick target” model), or alternatively plasma heated to very high temperatures behind a rapidly moving conduction front (the “thermal” model). The transport of this energy into the remaining portion of the atmosphere results in violent mass motion and strong emission across the electromagnetic spectrum. Radiation processes play a crucial role in determining the ensuing plasma motion.

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Authors and Affiliations

  1. Lawrence Livermore National Laboratory, Institute of Geophysics and Planetary Physics, Mail Code L-413, 94550, Livermore, California, USA

    George H. Fisher

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  1. George H. Fisher
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Editor information

Dimitri Mihalas Karl-Heinz A. Winkler

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© 1986 Springer-Verlag

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Fisher, G.H. (1986). Radiation hydrodynamics in solar flares. In: Mihalas, D., Winkler, KH.A. (eds) Radiation Hydrodynamics in Stars and Compact Objects. Lecture Notes in Physics, vol 255. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-16764-1_5

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  • DOI: https://doi.org/10.1007/3-540-16764-1_5

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  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-540-16764-8

  • Online ISBN: 978-3-540-38739-8

  • eBook Packages: Springer Book Archive

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