Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption

Liu, Rui

doi:10.48550/arxiv.2007.11363

Cited by 3 publications

(3 citation statements)

References 418 publications

(610 reference statements)

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“…Large-scale solar eruptions include prominence/filament eruptions, flares, and coronal mass ejections (CMEs) (Benz 2008;Chen 2011;Parenti 2014;Liu 2020). They are capable of inflicting huge impacts on the solar-terrestrial system (Švestka 2001;Cheng et al 2014;Shen et al 2014;Lugaz et al 2017;Gopalswamy et al 2018).…”

Section: Introductionmentioning

confidence: 99%

How flux feeding causes eruptions of solar magnetic flux ropes with the hyperbolic flux tube configuration?

Zhang,

Liu,

Wang

et al. 2021

Preprint

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Coronal magnetic flux ropes are generally considered to be the core structure of large-scale solar eruptions. Recent observations found that solar eruptions could be initiated by a sequence of "flux feeding," during which chromospheric fibrils rise upward from below, and merge with a pre-existing prominence. Further theoretical study has confirmed that the flux feeding mechanism is efficient in causing the eruption of flux ropes that are wrapped by bald patch separatrix surfaces. But it is unclear how flux feeding influences coronal flux ropes that are wrapped by hyperbolic flux tubes (HFT), and whether it is able to cause the flux-rope eruption. In this paper, we use a 2.5-dimensional magnetohydrodynamic model to simulate the flux feeding processes in HFT configurations. It is found that flux feeding injects axial magnetic flux into the flux rope, whereas the poloidal flux of the rope is reduced after flux feeding. Flux feeding is able to cause the flux rope to erupt, provided that the injected axial flux is large enough so that the critical axial flux of the rope is reached. Otherwise, the flux rope system evolves to a stable equilibrium state after flux feeding, which might be even farther away from the onset of the eruption, indicating that flux feeding could stabilize the rope system with the HFT configuration in this circumstance.

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Section: Introductionmentioning

confidence: 99%

How flux feeding causes eruptions of solar magnetic flux ropes with the hyperbolic flux tube configuration?

Zhang,

Liu,

Wang

et al. 2021

Preprint

Self Cite

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“…The results of our discussions form the core of this manuscript. We do not attempt to provide a comprehensive review of CME initiation and formation processes since there exist several recent excellent reviews on the matter (Chen, 2011;Cheng et al, 2017;Manchester et al, 2017;Green et al, 2018;Archontis and Syntelis, 2019;Georgoulis et al, 2019;Liu, 2020). We focus on three key questions: (1) what constitutes an MFR or SMA?…”

Section: Introductionmentioning

confidence: 99%

Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections

Patsourakos,

Vourlidas,

Török

et al. 2020

Preprint

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A clear understanding of the nature of the pre-eruptive magnetic field configurations of Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting solar eruptions. Only two, but seemingly disparate, magnetic configurations are considered viable; namely, sheared magnetic arcades (SMA) and magnetic flux ropes (MFR). They can form via three physical mechanisms (flux emergence, flux cancellation, helicity condensation). Whether the CME culprit is an SMA or an MFR, however, has been strongly debated for thirty years. We formed an International Space Science Institute (ISSI) team to address and resolve this issue and report the outcome here. We review the status of the field across modeling and observations, identify the open and closed issues, compile lists of SMA and MFR observables to be tested against observations and outline research activities to close the gaps in our current understanding. We propose that the combination of multi-viewpoint multi-thermal coronal observations and multiheight vector magnetic field measurements is the optimal approach for resolving

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“…On the other hand, the ideal MHD instabilities, mainly the helical kink instability (KI, Hood & Priest 1981;Török et al 2004Török et al , 2010Török & Kliem 2005) and the torus instability (TI, Bateman 1978;Kliem & Török 2006) are developed based on magnetic flux rope (MFR, Kuperus & Raadu 1974;Chen 1989;Titov & Démoulin 1999;Liu 2020), which is a coherent group of twisted magnetic flux winding around a common axis. In the MFR-based models, it is assumed that MFR exists in the corona prior to eruption.…”

Section: Introductionmentioning

confidence: 99%

Variation of Magnetic Flux Ropes Through Major Solar Flares

Duan,

Jiang,

Zhou

et al. 2020

Preprint

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It remains unclear how solar flares are triggered and in what conditions they can be eruptive with coronal mass ejections. Magnetic flux ropes (MFRs) has been suggested as the central magnetic structure of solar eruptions, and their ideal instabilities including mainly the kink instability (KI) and torus instability (TI) provide important candidates for triggering mechanisms. Here using magnetic field extrapolations from observed photospheric magnetograms, we systematically studied the variation of coronal magnetic fields, focusing on MFRs, through major flares including 29 eruptive and 16 confined events. We found that nearly 90% events possess MFR before flare and 70% have MFR even after flare. We calculated the controlling parameters of KI and TI, including the MFR's maximum twist number and the decay index of its strapping field. Using the KI and TI thresholds empirically derived from solely the pre-flare MFRs, two distinct different regimes are shown in the variation of the MFR controlling parameters through flares. For the events with both parameters below their thresholds before flare, we found no systematic change of the parameters after the flares, in either the eruptive or confined events. In contrast, for the events with any of the two parameters exceeding their threshold before flare (most of them are eruptive), there is systematic decrease in the parameters to below their thresholds after flares. These results provide a strong constraint for the values of the instability thresholds and also stress the necessity of exploring other eruption mechanisms in addition to the ideal instabilities.

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Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption

Cited by 3 publications

References 418 publications

How flux feeding causes eruptions of solar magnetic flux ropes with the hyperbolic flux tube configuration?

How flux feeding causes eruptions of solar magnetic flux ropes with the hyperbolic flux tube configuration?

Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections

Variation of Magnetic Flux Ropes Through Major Solar Flares

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