Investigating Energetic X-Shaped Flares on the Outskirts of A Solar Active Region

TL;DR

This study investigates the unique X-shaped solar flares on the outskirts of an active region, revealing their magnetic topology involving hyperbolic flux tubes and current layers, which differ from standard flare models.

Contribution

It uncovers the magnetic topology and reconnection processes responsible for X-shaped flares, emphasizing the role of hyperbolic flux tubes in 3D magnetic reconnection.

Findings

X-shaped ribbons are governed by intersection of quasi-separatrix layers.

Magnetic topology involves hyperbolic flux tubes and embedded separators.

Current layers at the HFT relate to observed X-ray emissions.

Abstract

Typical solar flares display two quasi-parallel, bright ribbons on the chromosphere. In between is the polarity inversion line (PIL) separating concentrated magnetic fluxes of opposite polarity in active regions (ARs). Intriguingly a series of flares exhibiting X-shaped ribbons occurred at the similar location on the outskirts of NOAA AR 11967, where magnetic fluxes were scattered, yet three of them were alarmingly energetic. The X shape, whose center coincided with hard X-ray emission, was similar in UV/EUV, which cannot be accommodated in the standard flare model. Mapping out magnetic connectivities in potential fields, we found that the X morphology was dictated by the intersection of two quasi-separatrix layers, i.e., a hyperbolic flux tube (HFT), within which a separator connecting a double null was embedded. This topology was not purely local but regulated by fluxes and flows over the whole AR. The nonlinear force-free field model suggested the formation of a current layer at the HFT, where the current dissipation can be mapped to the X-shaped ribbons via field-aligned heat conduction. These results highlight the critical role of HFTs in 3D magnetic reconnection and have important implications for astrophysical and laboratory plasmas.