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

Authors: Morosan, D. E., Palmerio, E., Räsänen, J. E., Kilpua, E. K. J., Magdalenic, J., Lynch, B. J., Kumari, A., Pomoell, J. & Palmroth, M.

Coronal mass ejections (CMEs) are large eruptions of magnetised plasma from the Sun that are often accompanied by solar radio bursts produced by accelerated electrons. A powerful source for accelerating electron beams are CME-driven shocks, however, there are other mechanisms capable of accelerating electrons during a CME eruption. So far, studies have relied on the traditional classification of solar radio bursts into five groups (Type I-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 CME that do not fit into the present classification of the solar radio emission.

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Recommended citation: Morosan, D. E., et al., “Electron acceleration and radio emission following the early interaction of two coronal mass ejections”, Astronomy and Astrophysics, vol. 642, 2020. doi:10.1051/0004-6361/202038801.