Magnetic Energy Partition Between the Coronal Mass Ejection and Flare From Ar 11283

Li, Feng; Wiegelmann, T.; Su, Yang; Inhester, B.; Li, Y. P.; Sun, Xudong; Gan, Weiqun

doi:10.1088/0004-637x/765/1/37

Cited by 73 publications

(97 citation statements)

References 39 publications

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“…It occurred near disk center at position N14W18. Because of its intensity and its location, the flare has been the object of many studies (Petrie 2012;Wang et al 2012;Feng et al 2013;Jiang et al , 2014aZharkov et al 2013;Gary et al 2014;Liu et al 2014;Yang et al 2014;Xu et al 2014). The flare, as recorded by the Geostationary Orbiting Environmental Satellites (GOES), started at 22:12 UT, peaking around 22:20 UT.…”

Section: The X-class Flare Event Of 6 September 2011mentioning

confidence: 99%

Evolution of flare ribbons, electric currents, and quasi-separatrix layers during an X-class flare

Janvier

Savcheva

Pariat

et al. 2016

A&A

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Context. The standard model for eruptive flares has been extended to three dimensions (3D) in the past few years. This model predicts typical J-shaped photospheric footprints of the coronal current layer, forming at similar locations as the quasi-separatrix layers (QSLs). Such a morphology is also found for flare ribbons observed in the extreme ultraviolet (EUV) band, and in nonlinear force-free field (NLFFF) magnetic field extrapolations and models. Aims. We study the evolution of the photospheric traces of the current density and flare ribbons, both obtained with the Solar Dynamics Observatory instruments. We aim to compare their morphology and their time evolution, before and during the flare, with the topological features found in a NLFFF model. Methods. We investigated the photospheric current evolution during the 06 September 2011 X-class flare (SOL2011-09-06T22:20) occurring in NOAA AR 11283 from observational data of the magnetic field obtained with the Helioseismic and Magnetic Imager aboard the Solar Dynamics Observatory. We compared this evolution with that of the flare ribbons observed in the EUV filters of the Atmospheric Imager Assembly. We also compared the observed electric current density and the flare ribbon morphology with that of the QSLs computed from the flux rope insertion method-NLFFF model.Results. The NLFFF model shows the presence of a fan-spine configuration of overlying field lines, due to the presence of a parasitic polarity, embedding an elongated flux rope that appears in the observations as two parts of a filament. The QSL signatures of the fan configuration appear as a circular flare ribbon that encircles the J-shaped ribbons related to the filament ejection. The QSLs, evolved via a magnetofrictional method, also show similar morphology and evolution as both the current ribbons and the EUV flare ribbons obtained several times during the flare. Conclusions. For the first time, we propose a combined analysis of the photospheric traces of an eruptive flare, in a complex topology, with direct measurements of electric currents and QSLs from observational data and a magnetic field model. The results, obtained by two different and independent approaches 1) confirm previous results of current increase during the impulsive phase of the flare and 2) show how NLFFF models can capture the essential physical signatures of flares even in a complex magnetic field topology.

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Section: The X-class Flare Event Of 6 September 2011mentioning

confidence: 99%

Evolution of flare ribbons, electric currents, and quasi-separatrix layers during an X-class flare

Janvier

Savcheva

Pariat

et al. 2016

A&A

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“…A free energy of ≈10 24 J to ≈10 25 J has been reported prior to weak flaring activity (Bleybel et al 2002;Régnier and Priest 2007;Sun et al 2012a), where "weak" means C-class flares. Moderate to strong (M-to X-class) events tend to occur only when free energies of some 10 25 J to some 10 26 J are present (Régnier et al 2005;Metcalf et al 2005;Thalmann and Wiegelmann 2008;Jing et al 2009;Sun et al 2012a;Feng et al 2013). Note, however, that the buildup of a sufficient amount of energy on its own does not guarantee the occurrence of a subsequent eruption and the release of part of this energy (Gilchrist et al 2012).…”

Section: Relation To Flare Productivitymentioning

confidence: 99%

“…Recent studies, however, do not show a clear tendency, i.e., no clear trend of more energetic events consuming more of the previously stored energy. So far, the estimated upper limits for the decrease of free magnetic energy range from 5 to 50 % Jing et al 2009;Sun et al 2012b;Feng et al 2013). Cases were also reported without a clear decrease (Sun et al 2012a) or even an increasing free energy (Metcalf et al 2005, and references therein).…”

Section: Energy Releasementioning

confidence: 99%

“…Recently, Feng et al (2013) investigated the partition of magnetic energy during an X-class and CME event. The radiative energy release estimated from the recorded flare emission was found to be at least one order of magnitude lower than the upper limit of available free magnetic energy; this also held for the kinetic and potential energy of the associated CME and confirmed the general consensus that by far not all of the free energy is released even during the most energetic events, but that a considerable portion remains available to power successive eruptions (see also Fig.…”

Section: Energy Releasementioning

confidence: 99%

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The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.

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“…As mentioned, it released two X-class flares on September 6 and 7, respectively. The eruption processes of both events have been well studied by many authors (Wang et al 2012;Feng et al 2013;Jiang & Feng 2013;Zharkov et al 2013;Liu et al 2014;Ruan et al 2014;Shen et al 2014). Thus, the details of the overall evolution of this AR will not be repeated here.…”

Section: Observations and The Overall Profile Of The Eventmentioning

confidence: 99%

Gradual Magnetic Evolution of Sunspot Structure and Filament–corona Dynamics Associated With the X1.8 Flare in Ar11283

Ruan

Chen

Wang

2015

ApJ

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In this paper, we present a study of the persistent and gradual penumbral decay and the correlated decline of the photospheric transverse field component 10-20 hr before a major flare (X1.8) eruption on 2011 September 7. This long-term pre-eruption behavior is corroborated by the well-imaged pre-flare filament rising, the consistent expansion of the coronal arcades overlying the filament, and the nonlinear force-free field modeling results in the literature. We suggest that both the long-term pre-flare penumbral decay and the transverse field decline are photospheric manifestations of the gradual rise of the coronal filament-flux rope system. We also suggest that the C3 flare and the subsequent reconnection process preceding the X1.8 flare play an important role in triggering the later major eruption.

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Magnetic Energy Partition Between the Coronal Mass Ejection and Flare From Ar 11283

Cited by 73 publications

References 39 publications

Evolution of flare ribbons, electric currents, and quasi-separatrix layers during an X-class flare

Evolution of flare ribbons, electric currents, and quasi-separatrix layers during an X-class flare

The magnetic field in the solar atmosphere

Gradual Magnetic Evolution of Sunspot Structure and Filament–corona Dynamics Associated With the X1.8 Flare in Ar11283

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