Flare particle acceleration in the interaction of twisted coronal flux ropes

TL;DR

This study models non-thermal particle acceleration in 3D MHD simulations of unstable coronal loops, revealing how reconnection and resistivity influence particle energization during solar flares.

Contribution

It introduces a relativistic guiding centre scheme applied to high-resolution MHD simulations to analyze particle acceleration in multi-threaded coronal loops, highlighting the effects of different resistivity models.

Findings

Particle energy gains vary with loop destabilization stages.

Resistivity type influences particle acceleration efficiency.

Particles are accelerated during reconnection events in unstable loops.

Abstract

The aim of this work is to investigate and characterise non-thermal particle behaviour in a three-dimensional (3D) magnetohydrodynamical (MHD) model of unstable multi-threaded flaring coronal loops. We have used a numerical scheme which solves the relativistic guiding centre approximation to study the motion of electrons and protons. The scheme uses snapshots from high resolution numerical MHD simulations of coronal loops containing two threads, where a single thread becomes unstable and (in one case) destabilises and merges with an additional thread. The particle responses to the reconnection and fragmentation in MHD simulations of two loop threads are examined in detail. We illustrate the role played by uniform background resistivity and distinguish this from the role of anomalous resistivity using orbits in an MHD simulation where only one thread becomes unstable without destabilising further loop threads. We examine the (scalable) orbit energy gains and final positions recovered at different stages of a second MHD simulation wherein a secondary loop thread is destabilised by (and merges with) the first thread. We compare these results with other theoretical particle acceleration models in the context of observed energetic particle populations during solar flares.