Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2229c&link_type=abstract
American Astronomical Society, SPD meeting #42, #22.29; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
In the model of stochastic acceleration for solar flares, particles undergo simultaneous pitch angle scattering and acceleration by plasma waves or turbulence near the top of the flaring loop. The accelerated electrons produce hard X-ray (HXR) emission mainly at the loop top (LT) and the footpoints (FPs) by bremsstrahlung. As shown in Petrosian & Chen (2010, ApJ Letters, 712, 131), imaging spectroscopic observations of the LT and FP sources can directly give the accelerated electron spectrum, which is determined by the turbulence diffusion and direct acceleration rates, and can constrain some characteristics of turbulence in the coronal LT acceleration region. In particular, we can obtain the escape time, which is related to the pitch angle scattering rate of electrons by turbulence.
We will present results from application of this method to several solar flares observed by the RHESSI satellite using the regularized electron maps. Comparison of electron spectra obtained from solution of the Fokker-Planck equation with the directly observed LT electron spectra allows us to determine whether the required acceleration rate by turbulence is consistent with the scattering rate obtained primarily from the ratio of the LT to FP fluxes.
We will use the escape time obtained from the above analysis to obtain the accelerated electron spectrum from the regularized inversion of the spatially integrated flare HXR spectrum, which can be applied to many more flares as it does not require imaging spectroscopy.
Chen Qingrong
Petrosian Vahe
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