Interaction between a Fast Rotating Sunspot and Ephemeral Regions as the Origin of the Major Solar Event on 2006 December 13

Zhang, Jun; Li, Leping; Song, Qiao

doi:10.1086/519280

Cited by 109 publications

(104 citation statements)

References 27 publications

(24 reference statements)

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“…[20] The active region NOAA 10930 is well known for the X3.4 class flare on 13 December 2006, which was captured by Hinode satellite soon after its launch, and has been carefully studied by many authors [e.g., Zhang et al, 2007;Moon et al, 2007;Kubo et al, 2007;Su et al, 2007;Yan et al, 2007;Schrijver et al, 2008;Jing et al, 2008;Guo et al, 2008;Su et al, 2008;Wang et al, 2008;Tan et al, 2009;Yan et al, 2009;Magara, 2009;Min and Chae, 2009;Li and Zhang, 2009;Jing et al, 2010]. Dozens of vector magneto-grams of NOAA 10930 were obtained by Hinode/SOT-SP when the active region crossed the Sun's disk during the first half of December 2006 [Matsuzaki et al, 2007].…”

Section: Sot-sp Photospheric Vector Magnetogramsmentioning

confidence: 99%

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

Wang

Yan

2011

J. Geophys. Res.

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[1] The Hinode satellite can obtain high-quality photospheric vector magnetograms of solar active regions and the simultaneous coronal loop images in soft X-ray and extreme ultraviolet (EUV) bands. In this paper, we continue the work of and apply the newly developed upward boundary integration computational scheme for the nonlinear force-free field (NLFFF) extrapolation of the coronal magnetic field to the

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Section: Sot-sp Photospheric Vector Magnetogramsmentioning

confidence: 99%

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

Wang

Yan

2011

J. Geophys. Res.

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“…The flare seems to be induced by a strong shear in the magnetic field associated with a filament eruption, leading to two large ribbons that are twisted but largely horizontal around the filament channel (e.g., Zhang et al 2007;Kosovichev & Sekii 2007). We will compare the orientation of the filament channel with a reconstruction of the associated MC observed in situ (see x 3.1 and Li et al 2007).…”

Section: Cme At the Sunmentioning

confidence: 99%

A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

Liu

Luhmann

Müller‐Mellin

et al. 2008

Astrophysical Journal

141

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The biggest halo coronal mass ejection (CME) since the Halloween storm in 2003, which occurred on 2006 December 13, is studied in terms of its solar source and heliospheric consequences. The CME was accompanied by an X3.4 flare, EUV dimmings, and coronal waves. It generated significant space weather effects such as an interplanetary shock, radio bursts, major solar energetic particle (SEP) events, and a magnetic cloud (MC) that were detected by a fleet of spacecraft including STEREO, ACE, WIND, and Ulysses. Reconstruction of the MC with the Grad-Shafranov (GS) method yields an axis orientation oblique to the flare ribbons. Observations of the SEP intensities and anisotropies show that the particles can be trapped, deflected, and reaccelerated by the large-scale transient structures. The CME-driven shock was observed at both the Earth and Ulysses when they were separated by 74 in latitude and 117 in longitude, which is the largest shock extent ever detected. The ejecta seem to have been missed at Ulysses. The shock arrival time at Ulysses is well predicted by an MHD model that can propagate the 1 AU data outward. The CME /shock is tracked remarkably well from the Sun all the way to Ulysses by coronagraph images, type II frequency drift, in situ measurements, and the MHD model. These results reveal a technique that combines MHD propagation of the solar wind and type II emissions to predict the shock arrival time at the Earth, which is a significant advance for space weather forecasting, especially when in situ data become available from the Solar Orbiter and Solar Sentinels.

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“…The flares associated with coronal mass ejections (CMEs) are termed "eruptive flares" and the eruptive flares usually last for a long period, from tens of minutes to hours (e.g., Zhang et al 2007). Some flares are not accompanied by CMEs in the wake of the eruption (Ji et al 2003), these flares are called confined flares (e.g., Wang & Zhang 2007).…”

Section: Introductionmentioning

confidence: 99%

Are Complex Magnetic Field Structures Responsible for the Confined X-class Flares in Super Active Region 12192?

Zhang

Chen

2017

ApJ

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From 2014 October 19 to 27, six X-class flares occurred in super active region (AR) 12192. They were all confined flares and were not followed by coronal mass ejections (CMEs). To examine the structures of the four flares close to the solar disk center from October 22 to 26, we employ firstly composite tripletime images in each flare process to display the stratified structure of these flare loops. The loop structures of each flare in both lower (171Å) and higher (131Å) temperature channels are complex, e.g., the flare loops rooting at flare ribbons are sheared or twisted (enwound) together, and the complex structures have not been destroyed during the flares. For the first flare, although the flare loop system appears as a spindle shape, we can estimate their structure from observations, with lengths ranging from 130 to 300 Mm, heights from 65 to 150 Mm, widths at the middle part of the spindle from 40 to 100 Mm, and shear angles from 16• to 90• . Moreover, the flare ribbons display irregular movements, such as the left ribbon fragments of the flare on 22 swept a small region repeatedly, and the both ribbons of the flare on 26 moved along the same direction, instead of separating from each other. These irregular movements also imply that the corresponding flare loops are complex, e.g. several sets of flare loops are twisted together. Although previous studies suggest that the background magnetic fields prevent confined flares from erupting, we firstly suggest based on these observations that the complex flare loop structures may be responsible for these confined flares.

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Interaction between a Fast Rotating Sunspot and Ephemeral Regions as the Origin of the Major Solar Event on 2006 December 13

Cited by 109 publications

References 27 publications

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

Nonlinear force-free field extrapolation of the coronal magnetic field using the data obtained by the Hinode satellite

A Comprehensive View of the 2006 December 13 CME: From the Sun to Interplanetary Space

Are Complex Magnetic Field Structures Responsible for the Confined X-class Flares in Super Active Region 12192?

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