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Even small solar flares can display a surprising level of complexityregarding their morphology and temporal evolution. Many of their properties,such as energy release and electron acceleration can be studied using highlycomplementary observations at X-ray and radio wavelengths. We present X-rayobservations from the Reuven Ramaty High Energy Solar Spectroscopic Imager(RHESSI) and radio observations from the Karl G. Jansky Very Large Array (VLA)of a series of GOES A3.4 to B1.6 class flares observed on 2013 April 23. Theflares, as seen in X-ray and extreme ultraviolet (EUV), originated frommultiple locations within active region NOAA 11726. A veritable zoo ofdifferent radio emissions between 1 GHz and 2 GHz was observed co-temporallywith the X-ray flares. In addition to broad-band continuum emission, broad-bandshort-lived bursts and narrow-band spikes, indicative of accelerated electrons,were observed. However, these sources were located up to 150 arcsec away fromthe flaring X-ray sources but only some of these emissions could be explainedas signatures of electrons that were accelerated near the main flare site. Forother sources, no obvious magnetic connection to the main flare site could befound. These emissions likely originate from secondary acceleration sitestriggered by the flare, but may be due to reconnection and accelerationcompletely unrelated to the co-temporally observed flare. Thanks to theextremely high sensitivity of the VLA, not achieved with current X-rayinstrumentation, it is shown that particle acceleration happens frequently andat multiple locations within a flaring active region.

Multiple electron acceleration instances during a series of solar microflares observed simultaneously at X-rays and microwaves