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Previous studies have shown that the energy release mechanism of some solarflares follow the Standard magnetic-reconnection model, but the detailedproperties of high-energy electrons produced in the flare are still not wellunderstood. We conducted a unique, multi-wavelength study that discloses thespatial, temporal and energy distributions of the accelerated electrons in theX2.2 solar flare on 2011, Feb. 15. We studied the source locations of sevendistinct temporal peaks observed in hard X-ray (HXR) and microwave (MW)lightcurves using the Reuven Ramaty High Energy Solar Spectroscopic Imager(RHESSI) in 50 to 75 keV channels and Nobeyama Radioheliograph (NoRH) in 34GHz, respectively. We found that the seven emission peaks did not come fromseven spatially distinct sites in HXR and MW, but rather in HXR we observed asudden change in location only between the second and the third peak, with thesame pattern occurring, but evolving more slowly in MW. Comparison between theHXR lightcurve and the temporal variations in intensity in the two MW sourcekernels also confirmed that the seven peaks came predominantly from twosources, each with multiple temporal peaks. In addition, we studied thepolarization properties of MW sources, and time delay between HXR and MW. Wediscuss our results in the context of the tether-cutting model.

Observation of 2011-02-15 X2.2 flare in Hard X-ray and Microwave