Derivation of Stochastic Acceleration Model Characteristics for Solar Flares From RHESSI Hard X-Ray Observations

Abstract

The model of stochastic acceleration of particles by turbulence has been successful in explaining many observed features of solar flares. Here we demonstrate a new method to obtain the accelerated electron spectrum and important acceleration model parameters from the high resolution hard X-ray observations provided by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). In our model, electrons accelerated at or very near the loop top produce thin target bremsstrahlung emission there and then escape downward producing thick target emission at the loop footpoints. Based on the electron flux spectral images obtained by the regularized inversion of the RHESSI count visibilities, we derive several important parameters for the acceleration model. We apply this procedure to the 2003 November 03 solar flare, which shows a loop top source up to 100--150 keV in hard X-ray with a relatively flat spectrum in addition to two footpoint sources. The results imply presence of strong scattering and a high density of turbulence energy with a steep spectrum in the acceleration region.

4 pages, 2 figures; revised manuscript submitted to ApJL

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• Particle acceleration mechanisms
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• Cascade and Damping of Alfvén-Cyclotron Fluctuations: Application to Solar Wind Turbulence Spectrum
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• Impulsive Phase Coronal Hard X-ray Sources in an X3.9 Class Solar Flare
• Hard X-ray footpoint sizes and positions as diagnostics of flare accelerated energetic electrons in the low solar atmosphere
• Turbulent cross-field transport of non-thermal electrons in coronal loops: theory and observations
• A Novel Approach in Constraining Electron Spectra in Blazar Jets: The Case of Markarian 421
• The Relation Between Escape and Scattering Times of Energetic Particles in a Turbulent Magnetized Plasma: Application to Solar Flares
• Flare Induced Photospheric Velocity Diagnostics
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• Determination of Acceleration Mechanism Characteristics Directly and Non-Parametrically from Observations: Application to Supernova Remnants
• Chromospheric Bubbles in Solar Flares
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