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

TL;DR

This study investigates unusual moving radio bursts linked to two CMEs, revealing their origin at high altitudes and suggesting CME-CME interaction as a key acceleration mechanism for electrons producing these emissions.

Contribution

The paper identifies a new class of high-altitude moving radio bursts associated with CME flank regions and proposes CME-CME interaction as their origin, expanding understanding beyond traditional shock acceleration models.

Findings

Three high-altitude moving radio bursts identified at CME flanks.

Radio bursts show fine-structured emission with ~1 s durations.

CME-CME interaction likely responsible for observed radio emissions.

Abstract

Context. 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. Aims. 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. Methods. By using radio imaging from the Nan\c{c}ay Radioheliograph, combined with observations from the Solar Dynamics Observatory, Solar and Heliospheric Observatory, and Solar Terrestrial Relations Observatory spacecraft, we investigate the moving radio bursts accompanying two subsequent CMEs on 22 May 2013. We use three-dimensional reconstructions of the two associated CME eruptions to show the possible origin of the observed radio emission. Results. We identified three moving radio bursts at unusually high altitudes in the corona that are located at the northern CME flank and move outwards synchronously with the CME. The radio bursts correspond to fine-structured emission in dynamic spectra with durations of ~1 s, and they may show forward or reverse frequency drifts. Since the CME expands closely following an earlier CME, a low coronal CME-CME interaction is likely responsible for the observed radio emission.