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Fatima Rubio da Costa   Submitted: 2015-05-20 12:15

Solar flares involve complex processes that are coupled together and span a wide range of temporal, spatial, and energy scales. Modeling such processes self-consistently has been a challenge in the past. Here we present such a model to simulate the coupling of high-energy particle kinetics with hydrodynamics of the atmospheric plasma. We combine the Stanford unified Fokker-Planck code that models particle acceleration, transport, and bremsstrahlung radiation with the RADYN hydrodynamic code that models the atmospheric response to collisional heating by non-thermal electrons through detailed radiative transfer calculations. We perform simulations using different injection electron spectra, including an ad hoc power law and more realistic spectra predicted by the stochastic acceleration model due to turbulence or plasma waves. Surprisingly, stochastically accelerated electrons, even with energy flux 1010 (erg/s/cm2), cause "explosive" chromospheric evaporation and drive stronger up- and downflows (and hydrodynamic shocks). We synthesize emission line profiles covering different heights in the lower atmosphere, including Hα 6563 A, He II 304 Å, Ca II K 3934 A and Si IV 1393 A. One interesting result is the unusual high temperature (up to a few 105K) of the formation site of He II 304 Å, which is expected due to photonionization-recombination under flare conditions, compared to those in the quiet Sun dominated by collisional excitation. When compared with observations, our results can constrain the properties of non-thermal electrons and thus the poorly understood particle acceleration mechanism.

Authors: Fatima Rubio da Costa, Wei Liu, Vahé Petrosian, Mats Carlsson
Projects: Other

Publication Status: submitted
Last Modified: 2015-05-25 09:30
Go to main E-Print page  Solar prominences: 'double, double . . . boil and bubble'  Temperature of the Source Plasma for Impulsive Solar Energetic Particles  Edit Entry  Download Preprint  Delete Entry 

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