The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Flare and of a Coronal Mass Ejection

Yan, Xiaoli; Jiang, Chaowei; Xue, Zhike; Wang, J. C.; Priest, E. R.; Yang, Liheng; Kong, D. F.; Cao, Wenda; Ji, Haisheng

doi:10.3847/1538-4357/aa7e29

Cited by 43 publications

(37 citation statements)

References 116 publications

(176 reference statements)

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“…About twenty minutes after the first flare, the main C5.0 occurred on the eastern side of the sunspots. This flare was associated with the eruption of a filament in AIA 304Å images (see the white arrow in Figure 1 During the eruption process of the filament, a loop-like hot magnetic structure is observed in the hot AIA 131 and 94Å observations (see the arrows in Figure 1 (e) and (f)), which should be a hot flux rope structure as reported in previous studies (e.g., Zhang et al 2012;Cheng et al 2013;Yan et al 2015Yan et al , 2017. The flux rope also erupted along with the eruption of the filament, and their eruption directly caused the observed halo CME in the LASCO coronagraphs.…”

Section: Observational Resultssupporting

confidence: 76%

A Quasi-periodic Fast-propagating Magnetosonic Wave Associated with the Eruption of a Magnetic Flux Rope

Shen¹,

Liu²,

Song³

et al. 2018

ApJ

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Using high temporal and high spatial resolution observations taken by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, we present the detailed observational analysis of a high quality quasi-periodic fastpropagating (QFP) magnetosonic wave that was associated with the eruption of a magnetic flux rope and a GOES C5.0 flare. For the first time, we find that the QFP wave lasted during the entire flare lifetime rather than only the rising phase of the accompanying flare as reported in previous studies. In addition, the propagation of the different parts of the wave train showed different kinematics and morphologies. For the southern (northern) part, the speed, duration, intensity variation are about 875 ± 29 (1485 ± 233) km s −1 , 45 (60) minutes, and 4% (2%), and the pronounced periods of them are 106 ± 12 and 160 ± 18 (75 ± 10 and 120 ± 16) seconds, respectively. It is interesting that the northern part of the wave train showed obvious refraction effect when they pass through a region of strong magnetic field. Periodicity analysis result indicates that all the periods of the QFP wave can be found in the period spectrum of the accompanying flare, suggesting their common physical origin. We propose that the quasi-periodic nonlinear magnetohydrodynamics process in the magnetic reconnection that produces the accompanying flare should be important for exciting of QFP wave, and the different magnetic distribution along different paths can account for the different speeds and morphology evolution of the wave fronts.

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Section: Observational Resultssupporting

confidence: 76%

A Quasi-periodic Fast-propagating Magnetosonic Wave Associated with the Eruption of a Magnetic Flux Rope

Shen¹,

Liu²,

Song³

et al. 2018

ApJ

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“…Importantly, high-resolution observations are powerful in disclosing the complete dynamic evolution of magnetic flux ropes related to the initiation of flares/CMEs. Using BBSO/GST Hα data, Yan et al (2017) presented that a smallscale flux rope (Figures 2d-h), with its footpoints showing a rotational motion, emerges near a large sunspot and subsequently erupts, driving an M1.0 flare and a CME. The presence of the flux rope was evidenced by both optimization NLFFF (Figure 2i) and data-driven magnetohydrodynamic modeling.…”

Section: Chromospheric Signatures Of Flux Ropesmentioning

confidence: 99%

Signatures of Magnetic Flux Ropes in the Low Solar Atmosphere Observed in High Resolution

Wang

Liu

2019

Front. Astron. Space Sci.

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Magnetic flux ropes (MFRs) are important physical features closely related to solar eruptive activities with potential space weather consequences. Studying MFRs in the low solar atmosphere can shed light on their origin and subsequent magnetic structural evolution. In recent years, observations of solar photosphere and chromosphere reached a spatial resolution of 0.1 to 0.2 arcsec with the operation of meter class ground-based telescopes, such as the 1.6 m Goode Solar Telescope at Big Bear Solar Observatory and the 1 m New Vacuum Solar Telescope at Yunnan Observatory. The obtained chromospheric Hα filtergrams with the highest resolution thus far have revealed detailed properties of MFRs before and during eruptions, and the observed pre-eruption structures of MFRs are well consistent with those demonstrated by non-linear force-free field extrapolations. There is also evidence that MFRs may exist in the photosphere. The magnetic channel structure, with multiple polarity inversions and only discernible in high-resolution magnetograph observations, may be a signature of photospheric MFRs. These MFRs are likely formed below the surface due to motions in the convection zone and appear in the photosphere through flux emergence. Triggering of some solar eruptions is associated with an enhancing twist in the low-atmospheric MFRs.

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“…The observational sunspots and active regions (ARs) are thought to be born of the emerging magnetic flux, which is the concentration of the magnetic fields (van Driel-Gesztelyi & Green 2015). On the other hand, many solar activities are triggered by newly emerging magnetic flux, such as coronal mass ejections (CMEs), flares, formations or eruptions of the filaments, jets, and small-scale bursts (e.g., Feynman & Martin 1995;Chen & Shibata 2000;Isobe et al 2007;Yan et al 2017;Chen et al 2018;Wang et al 2018Wang et al , 2019Young et al 2018;Tian et al 2018). Such an emerging magnetic field not only plays a vital role in understanding active regions and sunspots, but it also has a great influence on many of the activities in taking place in the solar atmosphere.…”

Section: Introductionmentioning

confidence: 99%

Naked emergence of an anti-Hale active region I. Overall evolution and magnetic properties

Wang,

Yan,

Kong

et al. 2021

Preprint

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Context.Aims. In order to understand the emergence of the active region, we investigate the emerging process and magnetic properties of a naked anti-Hale active region during the period between August 24 to 25, 2018. Methods. Using the data from Helioseismic and Magnetic Imager on board the Soar Dynamic Observatory and the New Vacuum Solar Telescope, we calculated different evolving parameters (such as pole separation, tilt angle) and magnetic parameters (such as vertical electric current, force-free parameter, relative magnetic helicity) during the emergence of the active region. With these calculated parameters and some reasonable assumptions, we use two different methods to estimate the twist of the active region. Results. The magnetic flux and pole separation continue increasing while the tilt angle exhibits a decreasing pattern during the emergence of the active region. The increase of the pole separation is mainly contributed as a result of the enhancement in the longitude direction. A power-law relationship between pole separation and total flux is found during the emergence of the active region. On the other hand, it is found that both the positive and negative electric currents increased equivalently and the average flux-weighted force-free parameter α remains almost consistently positive, on the order of ∼ 10 −8 m −1 . The relative magnetic helicity is mainly contributed by the shear term, while the relative magnetic helicity injection flux of the shear term changes its sign at the latter stage of the emergence. The twist number of the whole active region remains on the order of 10 −1 turns during the emergence of the active region. Conclusions. We find that the magnetic flux tube with low twist also could emerge into the solar atmosphere.

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The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Flare and of a Coronal Mass Ejection

Cited by 43 publications

References 116 publications

A Quasi-periodic Fast-propagating Magnetosonic Wave Associated with the Eruption of a Magnetic Flux Rope

A Quasi-periodic Fast-propagating Magnetosonic Wave Associated with the Eruption of a Magnetic Flux Rope

Signatures of Magnetic Flux Ropes in the Low Solar Atmosphere Observed in High Resolution

Naked emergence of an anti-Hale active region I. Overall evolution and magnetic properties

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