Electron Trapping and Precipitation in Asymmetric Solar Flare Loops

Details Electron Trapping and Precipitation in Asymmetric Solar Flare Loops Electron Trapping and Precipitation in Asymmetric Solar Flare Loops

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000iaus..195..375a&link_type=abstract

Highly Energetic Physical Processes and Mechanisms for Emission from Astrophysical Plasmas, Proceedings of IAU Symposium #195, h

Astronomy and Astrophysics

Astrophysics

Scientific paper

Acceleration, propagation, and energy loss of particles energized in solar flares cannot be studied separately because their radiative signatures observed in the form of hard X-ray bremsstrahlung or radio gyrosynchrotron emission represent a convolution of all these processes. We analyze hard X-ray emission from solar flares using a kinematic model that includes free-streaming electrons (having an energy-dependent time-of-flight delay) as well as temporarily trapped electrons (which are pitch-angle scattered by Coulomb collisional scattering) to determine various physical parameters (trapping times, flux asymmetry, loss-cone angles, magnetic mirror ratios) in flare loops with asymmetric magnetic fields.

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