A Solar Eruption Driven by Rapid Sunspot Rotation

Ruan, Guiping; Chen, Yao; Wang, Shuo; Zhang, Hongqi; Li, Gang; Jing, Ju; Su, Jiangtao; Li, Xing; Xu, Haiqing; Du, Guojun; Wang, Haimin

doi:10.1088/0004-637x/784/2/165

Cited by 46 publications

(45 citation statements)

References 50 publications

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“…On the one hand, we did not observe any significant emergence of magnetic field during the period of recurrent flare occurrence, while on the other hand, we detected a peculiar horizontal velocity pattern during our observation time interval. As did Ruan et al (2014), before the X2.1 class flare we noted a clockwise rotation of the main negative sunspot, but we also found a persistent shear motion of the positive and negative polarities along the PIL. However, from the Poynting fluxes computed from the emergence of the magnetic flux and from the shearing of magnetic field lines due to tangential motions on the surface, we found that, even if the energy flux coming from the shearing motions seems to be the main source of energy in the corona during our observation time interval, this energy is lower than the energy released by the M and X flares.…”

Section: Discussionsupporting

confidence: 81%

“…5d) their longitudes differ by about 15 . Moreover, in the same maps it is also possible to recognize the clockwise rotation of the positive spot, already interpreted by Ruan et al (2014) as the main mechanism able to transport a considerable amount of magnetic energy into the corona before the X2.1 flare occurred on September 6.…”

Section: Horizontal Velocity Fieldsmentioning

confidence: 72%

“…The released free energy resulting from their non-linear force-free field model was about 6.4 × 10 31 erg. Ruan et al (2014) showed that the filament and the overlying arcades involved in the flare were partially rooted in a sunspot which rotated at ∼10…”

Section: Ar Evolutionmentioning

confidence: 99%

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Recurrent flares in active region NOAA 11283

Romano

Zuccarello

Guglielmino

et al. 2015

A&A

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Context. Flares and coronal mass ejections (CMEs) are solar phenomena that are not yet fully understood. Several investigations have been performed to single out their related physical parameters that can be used as indices of the magnetic complexity leading to their occurrence. Aims. In order to shed light on the occurrence of recurrent flares and subsequent associated CMEs, we studied the active region NOAA 11283 where recurrent M and X GOES-class flares and CMEs occurred. Methods. We use vector magnetograms taken by HMI/SDO to calculate the horizontal velocity fields of the photospheric magnetic structures, the shear and the dip angles of the magnetic field, the magnetic helicity flux distribution, and the Poynting fluxes across the photosphere due to the emergence and the shearing of the magnetic field. Results. Although we do not observe consistent emerging magnetic flux through the photosphere during the observation time interval, we detected a monotonic increase of the magnetic helicity accumulated in the corona. We found that both the shear and the dip angles have high values along the main polarity inversion line (PIL) before and after all the events. We also note that before the main flare of X2.1 GOES class, the shearing motions seem to inject a more significant energy than the energy injected by the emergence of the magnetic field. Conclusions. We conclude that the very long duration (about 4 days) of the horizontal displacement of the main photospheric magnetic structures along the PIL has a primary role in the energy release during the recurrent flares. This peculiar horizontal velocity field also contributes to the monotonic injection of magnetic helicity into the corona. This process, coupled with the high shear and dip angles along the main PIL, appears to be responsible for the consecutive events of loss of equilibrium leading to the recurrent flares and CMEs.

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Section: Discussionsupporting

confidence: 81%

Section: Horizontal Velocity Fieldsmentioning

confidence: 72%

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Recurrent flares in active region NOAA 11283

Romano

Zuccarello

Guglielmino

et al. 2015

A&A

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“…In Ruan et al (2014), a study focusing on the 6-hr long pre-flare sunspot activity and photospheric magnetic field evolution of the X2.1 event from AR 11283 was presented. It was concluded that the persistent sunspot rotation plays an important role in twisting, energizing, and destabilizing the coronal filament-flux rope system.…”

Section: Introductionmentioning

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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“…The X1.8 flare on 2011 September 7 is notable because of a substantial amount of chromospheric material being ejected. The field evolution around the time of the two X-class flares was described by Ruan et al (2014Ruan et al ( , 2015. These studies note that both major flares were associated with clear sunspot rotation.…”

Section: Ar 11283mentioning

confidence: 90%

The Nonpotentiality of Coronae of Solar Active Regions, the Dynamics of the Surface Magnetic Field, and the Potential for Large Flares

Schrijver

2016

ApJ

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Flares and eruptions from solar active regions (ARs) are associated with atmospheric electrical currents accompanying distortions of the coronal field away from a lowest-energy potential state. In order to better understand the origin of these currents and their role in M-and X-class flares, I review all AR observations made with Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager and SDO/Atmospheric Imaging Assembly from 2010 May through 2014 October within ≈40°from the disk center. I select the roughly 4% of all regions that display a distinctly nonpotential coronal configuration in loops with a length comparable to the scale of the AR, and all that emit GOES X-class flares. The data for 41 regions confirm, with a single exception, that strong-field, high-gradient polarity inversion lines (SHILs) created during emergence of magnetic flux into, and related displacement within, pre-existing ARs are associated with X-class flares. Obvious nonpotentiality in the AR-scale loops occurs in six of ten selected regions with X-class flares, all with relatively long SHILs along their primary polarity inversion line, or with a long internal filament there. Nonpotentiality can exist in ARs well past the flux-emergence phase, often with reduced or absent flaring. I conclude that the dynamics of the flux involved in the compact SHILs is of pre-eminent importance for the large-flare potential of ARs within the next day, but that their associated currents may not reveal themselves in AR-scale nonpotentiality. In contrast, AR-scale nonpotentiality, which can persist for many days, may inform us about the eruption potential other than those from SHILs which is almost never associated with X-class flaring.

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A Solar Eruption Driven by Rapid Sunspot Rotation

Cited by 46 publications

References 50 publications

Recurrent flares in active region NOAA 11283

Recurrent flares in active region NOAA 11283

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

The Nonpotentiality of Coronae of Solar Active Regions, the Dynamics of the Surface Magnetic Field, and the Potential for Large Flares

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