Resolving spatial and temporal shock structures using LOFAR observations of type II radio bursts

TL;DR

This study uses high-resolution LOFAR radio imaging combined with EUV observations to analyze the structure and origin of multiple type II radio burst lanes caused by coronal shocks, revealing shock expansion and hotspot formation.

Contribution

It provides the first detailed spatial analysis of multiple type II radio burst lanes, linking them to shock expansion and ambient medium structuring using LOFAR data.

Findings

Multiple radio sources correspond to a multi-lane type II burst.

Shock expansion is nearly self-similar with hotspots forming at various times.

Small-scale plasma structuring influences electron acceleration hotspots.

Abstract

Collisionless shocks are one of the most powerful particle accelerators in the Universe. In the heliosphere, type II solar radio bursts are signatures of electrons accelerated by collisionless shocks launched at the Sun. Spectral observations of these bursts show a variety of fine structures often composing multiple type II lanes. The origin of these lanes and structures is not well understood and has been attributed to the inhomogeneous environment around the propagating shock. Here, we aim to determine the large-scale local structures near a coronal shock wave using high-resolution radio imaging observations of a complex type II radio burst observed on 3 October 2023. By using inteferometric imaging from the Low Frequency Array (LOFAR), combined with extreme ultraviolet observations, we investigate the origin of multiple type II lanes at low frequencies (30--80~MHz) relative to the propagating shock wave. We identify at least three radio sources at metric wavelengths corresponding to a multi-lane type II burst. The type II burst sources propagate outwards with a shock driven by a coronal mass ejection. We find a double radio source that exhibits increasing separation over time, consistent with the expansion rate of the global coronal shock. This suggests that the overall shock expansion is nearly self-similar, with acceleration hotspots forming at various times and splitting at a rate proportional to the shock's expansion. Our results show the importance of increased spatial resolution in determining either the small-scale spatial properties in coronal shocks or the structuring of the ambient medium. Possible shock corrugations or structuring of the upstream plasma at the scale of 10$^5$~km can act as hotspots for the acceleration of suprathermal electrons.