  Solar coronal radio bursts are enhanced radio emission excited by energetic
electrons accelerated during solar eruptions, studies on which are important
for investigating the origin and physical mechanism of energetic particles and
further diagnosing coronal parameters. Earlier studies suffered from a lack of
simultaneous high-quality imaging data of the radio burst and the eruptive
structure in the inner corona. Here we present a study on a complex solar radio
eruption consisting of a type II and three reversely-drifting type III bursts,
using simultaneous EUV and radio imaging data. It is found that the type II
burst is closely associated with a propagating and evolving CME-driven EUV
shock structure, originated initially at the northern shock flank and later
transferred to the top part of the shock. This source transfer is co-incident
with the presence of shock decay and enhancing signatures observed at the
corresponding side of the EUV front. The electron energy accelerated by the
shock at the flank is estimated to be $\sim$ 0.3 c by examining the imaging
data of the fast-drifting herringbone structure of the type II burst. The
reversely-drifting type III sources are found to be within the ejecta and
correlated with a likely reconnection event therein. Implications on further
observational studies and relevant space-weather forecasting techniques are
discussed.
