Pre-flare activity and magnetic reconnection during the evolutionary stages of energy release in a solar eruptive flare

TL;DR

This study analyzes a solar eruptive flare using multi-wavelength observations, revealing pre-flare magnetic activities and reconnection processes that trigger the main flare, advancing understanding of solar eruption mechanisms.

Contribution

It provides detailed insights into pre-flare magnetic reorganization and reconnection, linking these processes to the initiation of the eruptive flare.

Findings

Pre-flare activities include localized brightenings and magnetic reconnection.

X-ray precursor phase shows plasma heating and electron acceleration.

Post-impulsive phase features high-energy looptop sources with non-thermal emissions.

Abstract

In this paper, we present a multi-wavelength analysis of an eruptive white-light M3.2 flare which occurred in active region NOAA 10486 on November 1, 2003. Excellent set of high resolution observations made by RHESSI and TRACE provide clear evidence of significant pre-flare activities for ~9 minutes in the form of an initiation phase observed at EUV/UV wavelengths followed by the X-ray precursor phase. During the initiation phase, we observed localized brightenings in the highly sheared core region close to the filament and interactions among short EUV loops overlying the filament which led to the opening of magnetic field lines. The X-ray precursor phase is manifested in RHESSI measurements below ~30 keV and coincided with the beginning of flux emergence at the flaring location along with early signatures of the eruption. From the RHESSI observations, we conclude that both plasma heating and electron acceleration occurred during the precursor phase. The main flare is consistent with the standard flare model. However, after the impulsive phase, intense HXR looptop source was observed without significant footpoint emission. More intriguingly, for a brief period the looptop source exhibited strong HXR emission with energies up to 100 keV and significant non-thermal characteristics. The present study indicates a causal relation between the activities in the preflare and main flare. We also conclude that pre-flare activities, occurred in the form of subtle magnetic reorganization along with localized magnetic reconnection, played a crucial role in destabilizing the active region filament leading to solar eruptive flare and associated large-scale phenomena.