Abstract
The heating of postflare loops by slow MHD shocks is considered. Although such loops were once thought to represent the dying remnant of a two-ribbon flare, it is now realized that they are the main part of such an event and begin very early on. It is shown that, if the local temperature of a loop, its local angle of inclination to the vertical, and ambient coronal conditions are known from observations, then simple analytical formulae give the rise speed of the shocks and the magnitude of the evaporative flow incident upon them. The formulae are applied as an example to the 1973 July 29 and 1980 May 21 two-ribbon flares, and reasonable agreement with rise-speed observations is found. It is therefore claimed that shock heating is a viable method for heating postflare loops for the long times observed.
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