Evolution of electron and proton temperatures in a flaring loop. I - A case of thermal heating of electrons

Details Evolution of electron and proton temperatures in a flaring loop. I - A case of thermal heating of electrons Evolution of electron and proton temperatures in a flaring loop. I - A case of thermal heating of electrons

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...84..271n&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 84, April 1983, p. 271-283.

Physics

5

Coronal Loops, Solar Electrons, Solar Flares, Solar Protons, Atmospheric Models, Electron Energy, Proton Energy, Solar Temperature, Velocity Distribution

Scientific paper

A temperature difference between electrons and protons produced in a flaring loop was investigated experimentally by adopting a one-fluid, two-temperature model instead of a single-temperature model. Consideration was given to the case in which flare energy is released in the form of heating of electrons located in the top part of the loop. In this case, a large temperature difference appears in the corona in the energy-input phase of the flare. When the material evaporated from the chromosphere fills the corona, the temperature difference in the loop begins to shrink rapidly from below. Eventually, in the loop apex, the proton temperature exceeds the electron temperature mainly due to cooling of the electrons by conduction down the loop and heating of the protons by compression of the ascending material. In the late phase of the flare (about 15 min from the flare onset), the temperature difference becomes less than 2 pct of the mean temperature of electrons and protons at every point in the loop.

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