Influence of magnetic field structure on the conduction cooling of flare loops

Details Influence of magnetic field structure on the conduction cooling of flare loops Influence of magnetic field structure on the conduction cooling of flare loops

Aug 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976soph...49..359a&link_type=abstract

Solar Physics, vol. 49, Aug. 1976, p. 359-367.

Physics

60

Magnetic Field Configurations, Solar Corona, Solar Flares, Solar Magnetic Field, Solar Temperature, Solar Wind, Stellar Models, Chromosphere, Evaporative Cooling, Heat Flux, Plasma Radiation, Plasma Temperature, Radiant Cooling, Thermal Plasmas

Scientific paper

A simple model facilitates calculation of the influence of magnetic-field configuration on the conduction cooling rate of a hot post-flare coronal plasma. The magnetic field is taken to be that produced by a line dipole or point dipole at an arbitrary depth below the chromosphere. For the high temperatures (at least 10 million K) produced by flares, the plasma may remain static and isobaric. The influence of the field is such as to increase the heat flux (per unit area) into the chromosphere, but to decrease the total conduction cooling of the flare plasma. This leads to a significant enhancement of the total energy radiated by the flare plasma.

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