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Solar flares are sudden energy release events in the solar corona, resultingfrom magnetic reconnection, that accelerates particles and heats the ambientplasma. During a flare, there are often multiple, temporally and spatiallyseparated individual energy release episodes that can be difficult to resolvedepending on the observing instrument. We present multi-wavelength imaging andspectroscopy observations of multiple electron acceleration episodes during aGOES B1.7-class two-ribbon flare on 2012 February 25, observed simultaneouslywith the Karl G. Jansky Very Large Array (VLA) at 1--2 GHz, the Reuven RamatayHigh Energy Solar Spectroscopic Imager (RHESSI) in X-rays, and the SolarDynamics Observatory in extreme ultraviolet (EUV). During the initial phase ofthe flare, five radio bursts were observed. A nonthermal X-ray source was seenco-temporal, but not co-spatial, with the first three radio bursts. Their radiospectra are interpreted as optically thick gyrosynchrotron emission. By fittingthe radio spectra with a gyrosynchrotron model, we derive the magnetic fieldstrength and nonthermal electron spectral parameters in each accelerationepisode. Notably, the nonthermal parameters derived from X-rays differconsiderably from the nonthermal parameters inferred from the radio. Theobservations are indicative of multiple, co-temporal acceleration episodesduring the impulsive phase of a solar microflare. The X-ray and radio burstsources likely originate from separate electron distributions in differentmagnetic loops.

Radio and X-ray Observations of Short-lived Episodes of Electron Acceleration in a Solar Microflare