Abstract
Most flares may be regarded as either simple-loop (or compact) flares or two-ribbon flares. In the former, a single loop brightens and decays without moving, whereas the two-ribbon type involves the eruption of a magnetic arcade. The object of the present talk is simply to describe the basic MHD instabilities that may be responsible, but, first of all, a summary of some basic theoretical concepts is given. These include the tearing-mode instability, magnetic reconnection and the energy method.
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Hood, A.W., Priest, E.R. (1981). Solar Flares: Magnetohydrodynamic Instabilities. In: Bonnet, R.M., Dupree, A.K. (eds) Solar Phenomena in Stars and Stellar Systems. NATO Advanced Study Institutes Series, vol 68. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-8479-0_28
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