On the Seismicity of September 7, 2011 X1.8-class Flare

Zharkov, S.; Green, L.M.; Matthews, Sarah; Zharkova, V. V.

doi:10.1088/1742-6596/440/1/012046

Cited by 10 publications

(20 citation statements)

References 16 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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“…Times and locations of the seismically active solar flares found in this survey. Some of these have been reported by other authors before, e.g., Kosovichev (2011Kosovichev ( , 2014; Zharkov et al (2013a); Sharykin, Kosovichev, and Zimovets (2014). Peak times and positions were taken from the RHESSI flare list.…”

Section: Helioseismic Holographymentioning

confidence: 99%

A Statistical Correlation of Sunquakes Based on Their Seismic and White-Light Emission

et al. 2015

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Several mechanisms have been proposed to explain the transient seismic emission, i.e., "sunquakes," from some solar flares. Some theories associate high-energy electrons and/or white-light emission with sunquakes. High-energy charged particles and their subsequent heating of the photosphere and/or chromosphere could induce acoustic waves in the solar interior. We carried out a correlative study of solar flares with emission in hard-X rays (HXRs), enhanced continuum emission at 6173Å, and transient seismic emission. We selected those flares observed by RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Imager) with a considerable flux above 50 keV between January 1, 2010 and June 26, 2014. We then used data from the Helioseismic and Magnetic Imager onboard the Solar Dynamic Observatory (SDO/HMI) to search for excess visible continuum emission and new sunquakes not previously reported. We found a total of 18 sunquakes out of 75 investigated. All of the sunquakes were associated with a enhancement of the visible continuum during the flare time. Finally, we calculated a coefficient of correlation for a set of dichotomic variables related to these observations. We found a strong correlation between two of the standard helioseismic detection techniques, and between sunquakes and visible continuum enhancements. We discuss the phenomenological connectivity between these physical quantities and the observational difficulties of detecting seismic signals and excess continuum radiation.

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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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On the Seismicity of September 7, 2011 X1.8-class Flare

Cited by 10 publications

References 16 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

A Statistical Correlation of Sunquakes Based on Their Seismic and White-Light Emission

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

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