Return current losses in pulse beam heating of the solar atmosphere

Details Return current losses in pulse beam heating of the solar atmosphere Return current losses in pulse beam heating of the solar atmosphere

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264..679k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 2, p. 679-685.

Astronomy and Astrophysics

Astrophysics

16

Atmospheric Heating, Electron Beams, Plasma Currents, Plasma Dynamics, Solar Atmosphere, Particle Emission, Solar Flares

Scientific paper

A 1D-hybrid code is employed to examine the influence of return current losses on pulse beam heating of the solar atmosphere. While heating of the coronal plasma by the penetrating electron beam is obtained as expected, strong return current losses of beam electrons at the resistivity jump in the transition region are also found. The electron beam energy is deposited at greater heights in the solar atmosphere than in the case of pure collisional losses. At the starting time of the flare, due to a strong return current heating, a very steep transition region is formed where upward and downward plasma flows are generated. The atmosphere is heated and a channel of hot low-resistivity plasma is formed by which the following electron beams can penetrate more easily to deep chromospheric levels where they are then thermalized.

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