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Solar flares and coronal mass ejections (CMEs) are responsible for electron acceleration in the corona. The solar corona, however, is too dilute to produce bremsstrahlung X-rays, and radio emission is usually the only tool for diagnostics of non-thermal electrons, especially at distances of a few solar radii. We investigate signatures of energetic electrons in a large-scale loop-like structure associated with a CME. For the first time, a detailed study of the temporal, spatial and frequency evolution of such structure at 1-2 solar radii becomes possible due to the LOw Frequency ARray (LOFAR) observations between 30-70 MHz. A complex frequency structure indicates very non-uniform density distribution within this radio-loop. The observed intensity and frequency maps of the radio emission are consistent with a magnetohydrodynamic model of a kink-unstable coronal loop. This suggests that the electron acceleration in the observed event is likely to be caused by magnetic reconnection in a very large twisted magnetic fluxtube.