Flare Generated Shock Wave Propagation Through Solar Coronal Arcade Loops and Associated Type II Radio Burst

TL;DR

This study investigates a flare-generated shock wave in the solar corona, analyzing its propagation through coronal loops and its association with a type II radio burst, revealing insights into solar flare dynamics without a CME.

Contribution

It provides detailed multiwavelength observations of a flare-induced shock wave and links it to magnetic topology and EUV wave behavior, highlighting the role of breakout reconnection.

Findings

EUV wave propagated at ~800-1490 km/s through coronal loops.

Shock wave closely matched the type II radio burst.

Breakout reconnection triggered the EUV wave and shock.

Abstract

This paper presents multiwavelength observations of a flare-generated type II radio burst. The kinematics of the shock derived from the type II closely match a fast EUV wave seen propagating through coronal arcade loops. The EUV wave was closely associated with an impulsive M1.0 flare without a related coronal mass ejection, and was triggered at one of the footpoints of the arcade loops in active region NOAA 12035. It was initially observed in the AIA 335 \AA\ images with a speed of ~800 km/s and accelerated to ~1490 km/s after passing through the arcade loops. A fan-spine magnetic topology was revealed at the flare site. A small, confined filament eruption (~340 km/s) was also observed moving in the opposite direction to the EUV wave. We suggest that breakout reconnection in the fan-spine topology triggered the flare and associated EUV wave that propagated as a fast shock through the arcade loops.