Numerical simulations of X-rays and gamma rays from solar flares.

摘要

adiation of energies from 10 keV to greater than 10 MeV has been observed during solar flares, and is interpreted to be due to bremsstrahlung by relativistic electrons. A complete treatment of this problem requires solution of kinetic equation for relativistic electrons and inclusion of synchrotron energy losses. We have solved this equation analytically in some simple limiting cases and numerically for models which have varying densities and magnetic fields using a Fokker-Planck code developed for this purpose. The resulting electron flux distributions are then used to calculate the spectral indices and angular distributions of the radiation and these results are used to compare with HXRBS observations of 30 to 500 keV X-rays and GRS observations of 0.3 to 1 MeV and greater than 10 MeV