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Context. Coronal mass ejections (CMEs) are large eruptions of magnetisedplasma from the Sun that are often accompanied by solar radio bursts producedby accelerated electrons. Aims. A powerful source for accelerating electronbeams are CME-driven shocks, however, there are other mechanisms capable ofaccelerating electrons during a CME eruption. So far, studies have relied onthe traditional classification of solar radio bursts into five groups (TypeI-V) based mainly on their shapes and characteristics in dynamic spectra. Here,we aim to determine the origin of moving radio bursts associated with a CMEthat do not fit into the present classification of the solar radio emission.Methods. By using radio imaging from the Nan\c{c}ay Radioheliograph, combinedwith observations from the Solar Dynamics Observatory, Solar and HeliosphericObservatory, and Solar Terrestrial Relations Observatory spacecraft, weinvestigate the moving radio bursts accompanying two subsequent CMEs on 22 May2013. We use three-dimensional reconstructions of the two associated CMEeruptions to show the possible origin of the observed radio emission. Results.We identified three moving radio bursts at unusually high altitudes in thecorona that are located at the northern CME flank and move outwardssynchronously with the CME. The radio bursts correspond to fine-structuredemission in dynamic spectra with durations of ~1 s, and they may show forwardor reverse frequency drifts. Since the CME expands closely following an earlierCME, a low coronal CME-CME interaction is likely responsible for the observedradio emission.

Electron acceleration and radio emission following the early interaction of two coronal mass ejections