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Based on detailed analysis of radio and X-ray observations of a flare on 2002April 11 augmented by realistic 3D modeling, we have identified a radioemission component produced directly at the flare acceleration region. Thisacceleration region radio component has distinctly different (i) spectrum, (ii)light curves, (iii) spatial location, and, thus, (iv) physical parameters fromthose of the separately identified, trapped or precipitating electroncomponents. To derive evolution of physical parameters of the radio sources weapply forward fitting of the radio spectrum time sequence with thegyrosynchrotron source function with 5 to 6 free parameters. At the stage whenthe contribution from the acceleration region dominates the radio spectrum, theX-ray- and radio- derived electron energy spectral indices agree well with eachother. During this time the maximum energy of the accelerated electron spectrumdisplays a monotonic increase with time from ~ 300 keV to ~ 2 MeV over roughlyone minute duration indicative of an acceleration process in the form of growthof the power-law tail; the fast electron residence time in the accelerationregion is about 2 - 4 s, which is much longer than the time of flight and sorequires a strong diffusion mode there to inhibit free-streaming propagation.The acceleration region has a relatively strong magnetic field, B ~ 120 G, anda low thermal density, less than 2x10^9 cm^-3. These acceleration regionproperties are consistent with a stochastic acceleration mechanism.

Probing Dynamics of Electron Acceleration with Radio and X-ray Spectroscopy, Imaging, and Timing in the 2002 Apr 11 Solar Flare