Estimating the lateral speed of a fast shock driven by a coronal mass ejection at the location of solar radio emissions

• Published in: Astronomy and astrophysics (Berlin) Vol. 686
• Main Authors: Normo, S., Morosan, D. E., Kilpua, E. K. J., Pomoell, J.
• Format: Journal Article
• Language: English
• Published: Heidelberg EDP Sciences 06.06.2024
• Subjects: Coronal mass ejection; Electromagnetic radiation; Electron acceleration; Observatories; Radio emission; Shock waves; Solar activity; Solar corona; Solar observatories; Solar radio bursts; Ultraviolet imagery; White light
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/202449277

Fast coronal mass ejections (CMEs) can drive shock waves capable of accelerating electrons to high energies. These shock-accelerated electrons act as sources of electromagnetic radiation, often in the form of solar radio bursts. Recent findings suggest that radio imaging of solar radio bursts can provide a means to estimate the lateral expansion of CMEs and associated shocks in the low corona. Our aim is to estimate the expansion speed of a CME-driven shock at the locations of radio emission using 3D reconstructions of the shock wave from multiple viewpoints. In this study, we estimated the 3D location of radio emission using radio imaging from the Nançay Radioheliograph and the 3D location of a CME-driven shock. The 3D shock was reconstructed using white-light and extreme ultraviolet images of the CME from the Solar Terrestrial Relations Observatory, Solar Dynamics Observatory, and the Solar and Heliospheric Observatory. The lateral expansion speed of the CME-driven shock at the electron acceleration locations was then estimated using the approximate 3D locations of the radio emission on the surface of the shock. The radio bursts associated with the CME were found to reside at the flank of the expanding CME-driven shock. We identified two prominent radio sources at two different locations and found that the lateral speed of the shock was between $ $ and $ second $ at these locations. Such a high speed during the early stages of the eruption already indicates the presence of a fast shock in the low corona. We also found a larger ratio between the radial and lateral expansion speed compared to values obtained higher up in the corona. We estimated for the first time the 3D expansion speed of a CME-driven shock at the location of the accompanying radio emission. The high shock speed obtained is indicative of a fast acceleration during the initial stage of the eruption. This acceleration leading to lateral speeds in the range of $ second $ is most likely one of the key parameters contributing to the presence of metric radio emissions, such as type II radio bursts.