Eruption of Solar Magnetic Flux Ropes Caused by Flux Feeding

Zhang, Quanhao; Wang, Yuming; Liu, Rui; Zhang, Jie; Hu, Yaozhong; Wang, Wensi; Zhuang, Bin; Li, Xiaolei

doi:10.3847/2041-8213/aba1f3

Cited by 16 publications

(10 citation statements)

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“…We note that the same conclusion was drawn by Patsourakos et al (2013) from the investigation of another hot channel observed continuously between a CME and its preceding confined eruption. Flux rope formation by reconnection in the corona has been suggested by a number of recent investigations, but several of them did not clearly establish the association with a confined flare (Liu et al 2010;Zhang et al 2014Zhang et al , 2020James et al 2017;Yan et al 2018;Gou et al 2019). Even more recently (while this paper was being revised), several authors pointed out the role of confined flares in forming or significantly enhancing a flux rope prior to a CME (Liu et al 2018;Wang et al 2019;Nindos et al 2020;James et al 2020).…”

Section: A General Picture Of Flux Rope Formation By Confined Eruptionsmentioning

confidence: 84%

Nonequilibrium Flux Rope Formation by Confined Flares Preceding a Solar Coronal Mass Ejection

Kliem

Lee

et al. 2021

ApJ

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We present evidence that a magnetic flux rope was formed before a coronal mass ejection (CME) and its associated long-duration flare during a pair of preceding confined eruptions and associated impulsive flares in a compound event in NOAA Active Region 12371. Extreme-ultraviolet images and the extrapolated nonlinear force-free field show that the first two (impulsive) flares, SOL2015-06-21T01:42, result from the confined eruption of highly sheared low-lying flux, presumably a seed flux rope. The eruption spawns a vertical current sheet, where magnetic reconnection creates flare ribbons and loops, a nonthermal microwave source, and a sigmoidal hot channel that can only be interpreted as a magnetic flux rope. Until the subsequent long-duration flare, SOL2015-06-21T02:36, the sigmoid’s elbows expand, while its center remains stationary, suggesting nonequilibrium but not yet instability. The “flare reconnection” during the confined eruptions acts like “tether-cutting reconnection” whose flux feeding of the rope leads to instability. The subsequent full eruption is seen as an accelerated rise of the entire hot channel, seamlessly evolving into the fast halo CME. Both the confined and ejective eruptions are consistent with the onset of the torus instability in the dipped decay index profile that results from the region’s two-scale magnetic structure. We suggest that the formation or enhancement of a nonequilibrium but stable flux rope by confined eruptions is a generic process occurring prior to many CMEs.

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Section: A General Picture Of Flux Rope Formation By Confined Eruptionsmentioning

confidence: 84%

Nonequilibrium Flux Rope Formation by Confined Flares Preceding a Solar Coronal Mass Ejection

Kliem

Lee

et al. 2021

ApJ

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“…In our simulation, the quantities at the lower boundary are fixed, indicating that it corresponds to the photosphere; increment equivalent extrapolation is used at the other boundaries (e.g., Zhang et al 2020):…”

Section: Simulating Proceduresmentioning

confidence: 99%

“…variable method (e.g., Zhang et al 2020) to construct the partially open bipolar background field, which can be cast in the complex variable form…”

mentioning

confidence: 99%

“…Starting from the initial condition and the background configuration, equations (A1) to (A5) are simulated by the multi-step implicit scheme (Hu 1989). With similar simulating procedures to those in Zhang et al (2020), we let a flux rope emerge from the lower base at a constant speed. The emergence begins at t = 0 and ends at t = τ E = 174 s, so that at time t (0 t τ e ), the emerged part of the rope is within −x E x x E at the lower base,…”

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confidence: 99%

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Confined and eruptive catastrophes of solar magnetic flux ropes caused by mass loading and unloading

Zhang,

Liu,

Wang

et al. 2021

Preprint

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It is widely accepted that coronal magnetic flux ropes are the core structures of large-scale solar eruptive activities, which inflict dramatic impacts on the solarterrestrial system. Previous studies have demonstrated that varying magnetic properties of a coronal flux rope system could result in a catastrophe of the rope, which may trigger solar eruptive activities. Since the total mass of a flux rope also plays an important role in stabilizing the rope, we use 2.5-dimensional magnetohydrodynamic (MHD) numerical simulations in this letter to investigate how a flux rope evolves as its total mass varies. It is found that an unloading process that decreases the total mass of the rope could result in an upward (eruptive) catastrophe in the flux rope system, during which the rope jumps upward and the magnetic energy is released. This indicates that mass unloading processes could initiate the eruption of the flux rope. Moreover, when the system is not too diffusive, there is also a downward (confined) catastrophe that could be caused by mass loading processes, via which the total mass accumulates. The magnetic energy, however, is increased during the downward catastrophe, indicating that mass loading processes could cause confined activities that may contribute to the storage of energy before the onset of coronal eruptions.

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“…Since there lacks accurate measurement of the local conditions in the corona, the physical essence of flux feeding mechanism is unclear based on observational results alone. To solve this, Zhang et al (2020) (hereafter Paper I) carried out numerical simulations to investigate the scenario of the flux feeding mechanism in BPS configurations. In their simulations, the rising chromospheric fibril is represented by a small flux rope emerging from below a pre-existing coronal magnetic flux rope with a BPS configuration.…”

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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Eruption of Solar Magnetic Flux Ropes Caused by Flux Feeding

Cited by 16 publications

References 50 publications

Nonequilibrium Flux Rope Formation by Confined Flares Preceding a Solar Coronal Mass Ejection

Nonequilibrium Flux Rope Formation by Confined Flares Preceding a Solar Coronal Mass Ejection

Confined and eruptive catastrophes of solar magnetic flux ropes caused by mass loading and unloading

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

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