The Nature of Flare Ribbons in Coronal Null-Point Topology

Abstract

Flare ribbons are commonly attributed to the low-altitude impact, along the footprints of separatrices or quasiseparatrix layers (QSLs), of particle beams accelerated through magnetic reconnection. If reconnection occurs at a three-dimensional coronal magnetic null point, the footprint of the dome-shaped fan surface would map a closed circular ribbon. This paper addresses the following issues: does the entire circular ribbon brighten simultaneously, as expected because all fan field lines pass through the null point? And since the spine separatrices are singular field lines, do spine-related ribbons look like compact kernels? What can we learn from these observations about current sheet formation and magnetic reconnection in a null-point topology? The present study addresses these questions by analyzing Transition Region and Coronal Explorer and Solar and Heliospheric Observatory/Michelson Doppler Imager observations of a confined flare presenting a circular ribbon. Using a potential field extrapolation, we linked the circular shape of the ribbon with the photospheric mapping of the fan field lines originating from a coronal null point. Observations show that the flare ribbon outlining the fan lines brightens sequentially along the counterclockwise direction and that the spine-related ribbons are elongated. Using the potential field extrapolation as initial condition, we conduct a low-β resistive magnetohydrodynamics simulation of this observed event. We drive the coronal evolution by line-tied diverging boundary motions, so as to emulate the observed photospheric flow pattern associated with some magnetic flux emergence. The numerical analysis allows us to explain several observed features of the confined flare. The vorticity induced in the fan by the prescribed motions causes the spines to tear apart along the fan. This leads to formation of a thin current sheet and induces null-point reconnection. We also find that the null point and its associated topological structure is embedded within QSLs, already present in the asymmetric potential field configuration. We find that the QSL footprints correspond to the observed elongated spine ribbons. Finally, we observe that before and after reconnecting at the null point, all field lines undergo slipping and slip-running reconnection within the QSLs. Field lines, and therefore particle impacts, slip or slip-run according to their distance from the spine, in directions and over distances that are compatible with the observed dynamics of the ribbons.

Observations of Multiple Blobs in Homologous Solar Coronal Jets in Closed Loop

“…Sympathetic flares have been extensively reported and investigated in the past decades (e.g. Hanaoka, 1996;Lang & Willson, 1989;Masson et al, 2009;Wang & Liu, 2012;Deng et al, 2013;Sun et al, 2013;Yang et al, 2014;Liu et al, 2015a). The possible agents of energy transported from the source region of energy release to the remote footpoints are nonthermal electrons (Tang & Moore, 1982;Nakajima et al, 1985;Martin & Svestka, 1988), thermal conduction front (Rust et al, 1985;Bastian & Gary , 1992), shock waves (Machado et al , 1988), and reconnection outflows (Hanaoka, 1996;Nishio et al, 1997).…”

A MULTI-INSTRUMENT ANALYSIS OF a C4.1 FLARE OCCURRING IN a Δ SUNSPOT

“…These dynamics are highly reminiscent of the slipping reconnection (Aulanier et al 2006) observed by Masson et al (2009). Analyzing observations of a confined flare presenting a circular ribbon, Masson et al (2009) noted signatures of field lines reconnecting by following a sequential order along a preferential direction.…”

“…The authors deduced the magnetic configuration of the AR during the flare from a potential extrapolation and found that (i) the reconnection initially takes place for field lines closer to a coronal null point, and that (ii) it eventually progresses further toward the direction of this null point. Thus, Masson et al (2009) found that the evolution of the reconnection is induced by the asymmetric magnetic configuration.…”

“…Analyzing observations of a confined flare presenting a circular ribbon, Masson et al (2009) noted signatures of field lines reconnecting by following a sequential order along a preferential direction. The authors deduced the magnetic configuration of the AR during the flare from a potential extrapolation and found that (i) the reconnection initially takes place for field lines closer to a coronal null point, and that (ii) it eventually progresses further toward the direction of this null point.…”

Particle Acceleration Due to Coronal Non-null Magnetic Reconnection

“…Observational examples of nearly circular post-flare loops (e.g. Masson et al, 2009) use potential field extrapolations to map the loop locations to a local separatrix dome formed from the fan plane of an overlying coronal null. Baumann, Haugbølle, and Nordlund (2013) modelled a similar configuration using a novel combination of PIC and magnetohydrodynamic (MHD) approaches and revealed that the underlying particle acceleration was driven by direct acceleration from interaction with the local reconnection electric field.…”