Ion-rich acceleration during an eruptive flux rope event in a multiple null-point configuration

TL;DR

This paper investigates gamma-ray emissions during a solar flare, revealing two distinct acceleration mechanisms with the second likely involving ion acceleration in a complex magnetic null-point topology.

Contribution

It provides new insights into ion acceleration processes in solar flares by linking gamma-ray emission features to magnetic null-point configurations and flux tube trapping.

Findings

Double-peaked gamma-ray emission indicates two separate acceleration mechanisms.

The second peak is dominated by ion acceleration in a null-point magnetic topology.

Delayed gamma-ray emission suggests ion trapping and gradual escape in flux tubes.

Abstract

We report on the $\gamma$-ray emission above 100~MeV from the GOES M3.3 flare SOL2012-06-03. The hard X-ray (HXR) and microwave emissions have typical time profiles with a fast rise to a well-defined peak followed by a slower decay. The $>$100~MeV emission during the prompt phase displayed a double-peaked temporal structure with the first peak following the HXR and microwaves, and the second one, about three times stronger, occurring $17 \pm 2$ seconds later. The time profiles seem to indicate two separate acceleration mechanisms at work, where the second $\gamma$-ray peak reveals a potentially pure or at least largely dominant ion acceleration. The Atmospheric Imaging Assembly imaging shows a bright elliptical ribbon and a transient brightening in the north-western (NW) region. Nonlinear force-free extrapolations at the time of the impulsive peaks show closed field lines connecting the NW region to the south-eastern part of the ribbon and the magnetic topology revealed clusters of nulls. These observations suggest a spine-and-fan geometry, and based on these observations we interpret the second $\gamma$-ray peak as being due to the predominant acceleration of ions in a region with multiple null points. The $>$100 MeV emission from this flare also exhibits a delayed phase with an exponential decay of roughly 350 seconds. We find that the delayed emission is consistent with ions being trapped in a closed flux tube with gradual escape via their loss cone to the chromosphere.