  Solar flares are sudden energy release events in the solar corona, resulting
from magnetic reconnection, that accelerates particles and heats the ambient
plasma. During a flare, there are often multiple, temporally and spatially
separated individual energy release episodes that can be difficult to resolve
depending on the observing instrument. We present multi-wavelength imaging and
spectroscopy observations of multiple electron acceleration episodes during a
GOES B1.7-class two-ribbon flare on 2012 February 25, observed simultaneously
with the Karl G. Jansky Very Large Array (VLA) at 1--2 GHz, the Reuven Ramatay
High Energy Solar Spectroscopic Imager (RHESSI) in X-rays, and the Solar
Dynamics Observatory in extreme ultraviolet (EUV). During the initial phase of
the flare, five radio bursts were observed. A nonthermal X-ray source was seen
co-temporal, but not co-spatial, with the first three radio bursts. Their radio
spectra are interpreted as optically thick gyrosynchrotron emission. By fitting
the radio spectra with a gyrosynchrotron model, we derive the magnetic field
strength and nonthermal electron spectral parameters in each acceleration
episode. Notably, the nonthermal parameters derived from X-rays differ
considerably from the nonthermal parameters inferred from the radio. The
observations are indicative of multiple, co-temporal acceleration episodes
during the impulsive phase of a solar microflare. The X-ray and radio burst
sources likely originate from separate electron distributions in different
magnetic loops.
