Evidence for the Flare Trigger Site and Three‐Dimensional Reconnection in Multiwavelength Observations of a Solar Flare

Fletcher, L.; Metcalf, Thomas R.; Alexander, David; Brown, D. S.; Ryder, L. A.

doi:10.1086/321377

Cited by 123 publications

(96 citation statements)

References 42 publications

(39 reference statements)

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“…In an embedded bipolar magnetic configuration, a spine links the magnetic null point to infinity (Fletcher et al 2001;Pariat et al 2010;Liu et al 2011;Jiang et al 2013) or to a remote place on the solar surface (Filippov 1999;Masson et al 2009;Wang & Liu 2012;Sun et al 2013). In the latter case, the released thermal energy and accelerated particles during reconnection would be transferred along the magnetic spine to heat the chromosphere and produce brightening at the other footpoint of spine, which has been discovered in flares (Biesecker & Thompson 2000;Wang et al 2001;Moon et al 2002;Brosius & Holman 2007;Su et al 2013).…”

Section: Discussion and Summarymentioning

confidence: 99%

Reciprocatory magnetic reconnection in a coronal bright point

Zhang

Chen

Ding

et al. 2014

A&A

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Context. Coronal bright points (CBPs) are small-scale and long-duration brightenings in the lower solar corona. They are often explained in terms of magnetic reconnection. Aims. We aim to study the substructures of a CBP and clarify the relationship among the brightenings of different patches inside the CBP. Methods. The event was observed by the X-ray Telescope (XRT) aboard the Hinode spacecraft on 2009 August 22−23. Results. The CBP showed repeated brightenings (or CBP flashes). During each of the two successive CBP flashes, that is, weak and strong flashes that were separated by ∼2 hr, the XRT images revealed that the CBP was composed of two chambers, patches A and B. During the weak flash, patch A brightened first, and patch B brightened ∼2 min later. During the transition, the right leg of a large-scale coronal loop drifted from the right side of the CBP to the left side. During the strong flash, patch B brightened first, and patch A brightened ∼2 min later. During the transition, the right leg of the large-scale coronal loop drifted from the left side of the CBP to the right side. In each flash, the rapid change of the connectivity of the large-scale coronal loop is strongly suggestive of the interchange reconnection. Conclusions. For the first time we found reciprocatory reconnection in the CBP, which means that reconnected loops in the outflow region of the first reconnection process serve as the inflow of the second reconnection process.

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Section: Discussion and Summarymentioning

confidence: 99%

Reciprocatory magnetic reconnection in a coronal bright point

Zhang

Chen

Ding

et al. 2014

A&A

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“…They have been found associated with flares (e.g., Gaizauskas et al, 1999;Aulanier et al, 2000;Fletcher et al, 2001) but not in a systematic way (Démoulin, Hénoux, and Mandrini, 1994;. Another piece of evidence for the presence of coronal nulls was given by Filippov (1999).…”

Section: The Small-scale Quadrupolar Eventmentioning

confidence: 96%

Companion Event and Precursor of the X17 Flare on 28 October 2003

et al. 2006

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Abstract.A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October -November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point.

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“…Several models of reconnection include mechanisms for generation of out of plane fields (Shay et al 1998). Threedimensional solar structures have been both observed (Fletcher et al 2001) and simulated (Birn et al 2000). Particle acceleration in reconnection geometries is a subject of intense research (Somov & Kosugi 1997;Aschwanden, Schwartz, & Dennis 1998;de Gouveia Dal Pino & Lazarian 2000).…”

Section: /2 V P B/ (4pr)mentioning

confidence: 99%

Experimental Observation of Energetic Ions Accelerated by Three-dimensional Magnetic Reconnection in a Laboratory Plasma

Brown

Cothran

Landreman

et al. 2002

The Astrophysical Journal

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Magnetic reconnection is widely believed responsible for heating the solar corona as well as for generating X-rays and energetic particles in solar flares. On astrophysical scales, reconnection in the intergalactic plasma is a prime candidate for a local source (!100 Mpc) of cosmic rays exceeding the Greisen-Zatsepin-Kúzmin cutoff (∼10 19 eV). In a laboratory astrophysics experiment, we have made the first observation of particles accelerated by magnetic reconnection events to energies significantly above both the thermal and the characteristic magnetohydrodynamic energies. These particles are correlated temporally and spatially with the formation of threedimensional magnetic structures in the reconnection region.

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Evidence for the Flare Trigger Site and Three‐Dimensional Reconnection in Multiwavelength Observations of a Solar Flare

Cited by 123 publications

References 42 publications

Reciprocatory magnetic reconnection in a coronal bright point

Reciprocatory magnetic reconnection in a coronal bright point

Companion Event and Precursor of the X17 Flare on 28 October 2003

Experimental Observation of Energetic Ions Accelerated by Three-dimensional Magnetic Reconnection in a Laboratory Plasma

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