A Unified Code for Acceleration, Transport and Radiation of Electrons in a Solar Flare Loop

Details A Unified Code for Acceleration, Transport and Radiation of Electrons in a Solar Flare Loop A Unified Code for Acceleration, Transport and Radiation of Electrons in a Solar Flare Loop

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0246p&link_type=abstract

American Astronomical Society, SPD Meeting #31, #02.46; Bulletin of the American Astronomical Society, Vol. 32, p.819

Astronomy and Astrophysics

Astronomy

Scientific paper

We have developed a fully relativistic code describing the particle and photon fluxes in a flaring loop during the impulsive phase of a solar flare. Our code includes a stochastic acceleration process at the flare loop-top, a transport equation describing the evolution of particles escaping the acceleration region as well as bremsstrahlung and synchrotron radiation code from both loop-top and foot-point sources. The acceleration process is described by 8 parameters that describe the acceleration region. We include the effects of collisional and synchrotron losses and we use simple empirical approximations of the diffusion coefficients and the escape-time. In describing the transport of energetic electrons from the loop-top to the foot-points, we are able to specify the atmospheric makeup as well as the density and magnetic field variation along the loop. The main processes affecting the transport of electrons are the variations of the magnetic field along the flaring loop (loop convergence), as well as synchrotron and collisional losses. The radiation code includes calculation of bremsstrahlung and synchrotron emission from both the loop-top acceleration region and the foot-point precipitation regions (after modifcation by transport effects). The code will be made available to all iterested solar physicists and is intended for interpretation of the forthcoming HESSI observations. In the future we will expand this code to include more accurate diffusion coefficients and more realistic magnetic field geometries. We also intend to develop similar codes for evaluation of the same processes for protons.

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