Abstract
Energy of a solar flare, how can it be estimated in a frame of magnetic reconnection theory? We would like to know also the characteristic time of energy accumulation before a flare as well as the characteristic time of energy release during a flare. Another important question is how to relate the dynamical characteristics of a flare with observed changes of magnetic field in the photosphere. These and some other fundamental properties of solar flares, including the particle acceleration process, are considered in this chapter on the basis of the reconnection theory without invoking many detail assumptions.
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Somov, B.V. (2013). Reconnection in Action. In: Plasma Astrophysics, Part II. Astrophysics and Space Science Library, vol 392. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-4295-0_5
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