Rapid temporal evolution of radiation from non-thermal electrons in solar flares

Details Rapid temporal evolution of radiation from non-thermal electrons in solar flares Rapid temporal evolution of radiation from non-thermal electrons in solar flares

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987stin...8725982l&link_type=abstract

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Computer Science

Coulomb Collisions, Electron Acceleration, Electron Beams, Fokker-Planck Equation, Solar Flares, Thermal Plasmas, Bremsstrahlung, Energy Distribution, Pitch (Inclination), Plasma Spectra, Solar Corona, X Rays

Scientific paper

Solutions of the time dependent Fokker-Planck equation was found for accelerated electrons undergoing Coulomb collisions in a magnetized, fully ionized plasma. An exact solution was found for arbitrary pitch angle and energy distribution in a uniform background plasma. Then, for an inhomogeneous plasma, a solution was found for particles with small pitch angles. These solutions were used to calculate the temporal evolution of bremsstrahlung x-rays from short bursts of nonthermal electron beams, and these spectra were compared with observed high time resolution spectra of short timescale solar hard x-ray bursts. It is shown that the observed softening in time of the spectra rules out a homogeneous background and therefore the possibility of electrons being confined to the corona either because of converging magnetic field or high densities. The inhomogeneous solution was also applied to a model with constant coronal density and exponentially rising chromospheric density. The spectra are shown to be consistent with that produced by a collimated beam of electrons accelerated in the corona with certain given conditions. These conditions could be violated if large pitch angle electrons are present.

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