The cooling and condensation of flare coronal plasma

Details The cooling and condensation of flare coronal plasma The cooling and condensation of flare coronal plasma

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981stin...8127029a&link_type=abstract

Unknown

Physics

Chromosphere, Coronal Loops, Isobars (Pressure), Solar Corona, Solar Flares, Mass Flow, Radiative Heat Transfer

Scientific paper

A model is investigated for the decay of flare heated coronal loops in which rapid radiative cooling at the loop base creates strong pressure gradients which, in turn, generate large (supersonic) downward flows. The coronal material cools and 'condenses' onto the flare chromosphere. The features which distinguish this model from previous models of flare cooling are: (1) most of the thermal energy of the coronal plasma may be lost by mass motion rather than by conduction or coronal radiation; (2) flare loops are not isobaric during their decay phase, and large downward velocities are present near the footpoints; (3) the differential emission measure q has a strong temperature dependence.

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