Transequatorial Filament Eruption and Its Link to a Coronal Mass Ejection

Wang, Jingxiu; Zhou, Guiping; Wen, Yingying; Zhang, Yuzong; Wang, Huaning; Deng, Yuanyong; Zhang, Jun; Harra, L. K.

doi:10.1088/1009-9271/6/2/12

Cited by 37 publications

(33 citation statements)

References 34 publications

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“…According to the properties of magnetic connectivity and the related footpoints, we discern different groups of magnetic-loop systems as magnetic "loops" or magnetic "arcades." The arcade-like structure has been identified in the flare phase with an apparent sheared configuration (Linke, Ioshpa, and Selivanov, 1990;Wang et al, 2006). As shown in Figures 2A and 2B, L is the length occupied by footpoints with the same polarity, and W is the maximum width between positive and negative footpoints of the same group of field lines.…”

Section: Methodsmentioning

confidence: 86%

“…Multi-waveband observations imply that the Bastille Day event was not solely an active-region phenomenon, but rather it involved a large-scale magnetic structure (Andrews, 2001;Chertok and Grechnev, 2005a;Wang et al, 2006). It has been found that the restructuring of large-scale magnetic fields in the corona in connection with the CME was accompanied by the appearance and growth of large-scale dimmings (Chertok and Grechnev, 2005a).…”

Section: The Event Of 14 July 2000mentioning

confidence: 99%

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Coronal Magnetic Connectivity and EUV Dimmings

et al. 2007

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Coronal dimming can be considered to be a disk signature of front-side coronal mass ejections (CMEs) , Geophys. Res. Lett. 27, 1431. The study of the magnetic connectivity associated with coronal dimming can shed new light on the magnetic nature of CMEs. In this study, four major flare-CME events on all halo CMEs associated with major flare activity in complex active regions (ARs) and produced severe space weather consequences. To explore the magnetic connectivity of these CMEs, global potential-field extrapolations based on the composite synoptic magnetograms from the Michelson Doppler Imager onboard the Solar and Heliospheric Observatory are constructed, and their association with coronal dimming is revealed by the Extreme ultraviolet Imaging Telescope. It is found that each flare-CME event involved interaction of more than ten sets of magnetic-loop systems. These loop systems occupied over 50% of all identified loop systems in the visible hemisphere and covered a wide range of solar longitudes and latitudes. We categorize the loop systems as active-region loops (ARLs), AR-interconnecting loops (ARILs) including transequatorial loops (TLs), and long arcades (LAs) straddling filament channels. A recurring pattern, the saddle-field configuration (SFC), consisting of ARILs, is found to be present in all four major flare-CME events. The magnetic connectivity revealed by this work implies that intercoupling and interaction of multiple flux-loop systems are required for a major CME. For comparison, a simple flare-CME event of 12 May 1997 with a relatively simple magnetic configuration is chosen. Even for this simple flare-CME event, we find that multiple flux-loop systems are also present.

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Section: Methodsmentioning

confidence: 86%

Section: The Event Of 14 July 2000mentioning

confidence: 99%

Coronal Magnetic Connectivity and EUV Dimmings

et al. 2007

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“…Zhukov and Veselovsky (2007) suggest a concept of global CMEs to describe observations of widespan CMEs whose source regions are truly global in nature. Activity with large spatial scale have been clearly shown in trans-equatorial magnetic structures (Harra et al 2003Wang et al 2006Wang et al , 2007.…”

Section: Discussionmentioning

confidence: 99%

“…Wang et al (2006) have demonstrated that this major event is not related to only one single AR, but the activation and eruption of a huge transequatorial filament are seen to precede the simultaneous filament eruption and flare in AR 9077, and the full halo-CME in the high corona. Wen et al (2006) illustrate the wide spread of non-thermal radio bursts, i.e., the non-thermal electron sources, based on the NRH (Nancay radio-heliograph) data.…”

Section: On the Bastille Day Event In 2000mentioning

confidence: 92%

Is there more global solar activity on the Sun?

Wang¹,

Zhang²,

Zhou³

et al. 2009

Proc. IAU

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Abstract. There appear indications of more global activity on the Sun which is larger, much beyond the scale of solar active regions (ARs). These indications include formation, flaring and eruption of the trans-equatorial loops seen in EUV and X-rays, formation and eruption of transequatorial filaments, global magnetic connectivity in EUV dimming associated with halo-coronal mass ejections, wide spread of radio burst sources in meter wavelength in the solar corona, and quasi-simultaneous magnetic flux emergence in both hemispheres seen during some major solar events. With examples of a few major events in the last solar cycle we discuss the possibility that there is large or global-scale activity on the Sun. Its spatial scale is many times larger than that of AR and temporal scale is over 10 hours. The exemplified trans-equatorial loops are anchored in ARs and their activity is temporally associated with flares in ARs too. In some sense the flares in ARs appear either as a part of or a precursor of the more global activity. It is likely that the combination of the flares in ARs and the associated global activity is responsible to the major solar-terrestrial events. More efforts in understanding the global activity are undertaken.

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“…This would explain the much lower fluxes observed in the keV ranges. This flare and its associated CME is not related to a single active region according to Wang et al (2006), who reported that the activation and eruption of a huge trans-equatorial filament preceded the flare and CME, and that many tens of halo-CMEs are found to be associated with trans-equatorial filaments and their magnetic environments. According to the authors, this could shed new light on CME magnetism.…”

Section: Bastille Day Event Of 2000-07-14mentioning

confidence: 98%

Temporal Evolution of Solar Energetic Particle Spectra

Doran

Dalla

2016

Sol Phys

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During solar flares and coronal mass ejections, solar energetic particles (SEPs) may be released into the interplanetary medium and near-Earth locations. The energy spectra of SEP events at 1 AU are typically averaged over the entire event or studied in a few snapshots. In this paper we analyze the time evolution of the energy spectra of four large selected SEP events using a large number of snapshots. We use a multi-spacecraft and multi-instrument approach for the observations, obtained over a wide SEP energy range. We find large differences in the spectra at the beginning of the events as measured by different instruments. We show that over time, a wave-like structure is observed traveling through the spectra from the highest energies to the lowest energies, creating an "arch" shape which then straightens into a power law later in the event, after times of the order of 10 hours. We discuss the processes that determine SEP intensities and their role in shaping the spectral time evolution.

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Transequatorial Filament Eruption and Its Link to a Coronal Mass Ejection

Cited by 37 publications

References 34 publications

Coronal Magnetic Connectivity and EUV Dimmings

Coronal Magnetic Connectivity and EUV Dimmings

Is there more global solar activity on the Sun?

Temporal Evolution of Solar Energetic Particle Spectra

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