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

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...254..343a&link_type=abstract

Astrophysical Journal, Part 1, vol. 254, Mar. 1, 1982, p. 343-348.

Astronomy and Astrophysics

Astrophysics

24

Coronal Loops, Magnetohydrodynamic Flow, Plasma Heating, Plasma Temperature, Radiant Cooling, Solar Flares, Temperature Dependence, Equilibrium Flow, Pressure Gradients, Stellar Models, Thermal Energy

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 important features of this model which distinguish it 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 has a strong temperature dependence. These results can account for recent observations of compact flare loops that are not consistent with the previous cooling models.

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