Abstract
The magnetic field is the main, and probably only source of energy for many of nonsteady phenomena in cosmic and laboratory plasmas [200].In particular, events of this type in the solar atmosphere include flares,coronal transients, and plasma ejections into the interplanetary space (e.g.,[335, 280]). At the same time, the magnetic field dissipation in a high-conductivity plasma and the magnetic field energy conversion into other forms constitute a well-known problem of solar physics [94, 281]. The problem has proved to be especially urgent when applied to the so-called ‘hot’ or ‘main’ phase of solar flares. It is in the high-temperature plasma where the bulk of the flare energy is released within the hot phase time [ 167,165].
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© 1992 Springer Science+Business Media Dordrecht
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Somov, B.V. (1992). Magnetic Reconnection and Energy Release in Solar Flares. In: Physical Processes in Solar Flares. Astrophysics and Space Science Library, vol 172. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-2396-9_3
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DOI: https://doi.org/10.1007/978-94-011-2396-9_3
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-5056-2
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