Quantifying the Toroidal Flux of Preexisting Flux Ropes of Coronal Mass Ejections

Xing, C.; Cheng, X.; Qiu, Jiong; Hu, Qiang; Priest, E. R.; Ding, M. D.

doi:10.3847/1538-4357/ab6321

Cited by 11 publications

(8 citation statements)

References 92 publications

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“…The lower estimate for the toroidal flux from the dimming method than the estimate for the poloidal flux from the flare ribbon method found in this study is in agreement with the result obtained from the statistical study by Sindhuja and Gopalswamy (2020). Some studies have however also indicated a significant increase in toroidal flux due to flare reconnection during the CME eruption (e.g., Xing et al, 2020). The temporal evolution of axial/poloidal fluxes and twist in flux ropes, and determination of those from the simulation data, are complicated research questions that require more extensive future investigations.…”

Section: Summary and Discussionsupporting

confidence: 89%

Estimating the Magnetic Structure of an Erupting CME Flux Rope From AR12158 Using Data-Driven Modeling

Kilpua

Pomoell

Price³

et al. 2021

Front. Astron. Space Sci.

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We investigate here the magnetic properties of a large-scale magnetic flux rope related to a coronal mass ejection (CME) that erupted from the Sun on September 12, 2014 and produced a well-defined flux rope in interplanetary space on September 14–15, 2014. We apply a fully data-driven and time-dependent magnetofrictional method (TMFM) using Solar Dynamics Observatory (SDO) magnetograms as the lower boundary condition. The simulation self-consistently produces a coherent flux rope and its ejection from the simulation domain. This paper describes the identification of the flux rope from the simulation data and defining its key parameters (e.g., twist and magnetic flux). We define the axial magnetic flux of the flux rope and the magnetic field time series from at the apex and at different distances from the apex of the flux rope. Our analysis shows that TMFM yields axial magnetic flux values that are in agreement with several observational proxies. The extracted magnetic field time series do not match well with in-situ components in direct comparison presumably due to interplanetary evolution and northward propagation of the CME. The study emphasizes also that magnetic field time-series are strongly dependent on how the flux rope is intercepted which presents a challenge for space weather forecasting.

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Section: Summary and Discussionsupporting

confidence: 89%

Estimating the Magnetic Structure of an Erupting CME Flux Rope From AR12158 Using Data-Driven Modeling

Kilpua

Pomoell

Price³

et al. 2021

Front. Astron. Space Sci.

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“…It was found that most (80%) of the MCs have a twist larger than 1.25 turns per AU, and some of the MCs have a twist larger than 10 turns per AU. Two factors are attributed to the high twist, one is the initial flux in the source region before eruption (Xing et al 2020), and the other is magnetic reconnection during eruption, which converts the ambient magnetic field to the MFR flux (Longcope & Beveridge 2007;Qiu 2009;Aulanier et al 2012;Wang et al 2017). According to our results, quiescent filaments are generally more twisted than active-region filaments before eruption.…”

Section: Origin Of Twists In Interplanetary Magnetic Cloudssupporting

confidence: 52%

Magnetic Twists of Solar Filaments

Guo,

Ni,

Qiu

et al. 2021

Preprint

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Solar filaments are cold and dense materials situated in magnetic dips, which show distinct radiation characteristics compared to the surrounding coronal plasma. They are associated with coronal sheared and twisted magnetic field lines. However, the exact magnetic configuration supporting a filament material is not easy to be ascertained because of the absence of routine observations of the magnetic field inside filaments.Since many filaments lie above weak-field regions, it is nearly impossible to extrapolate their coronal magnetic structures by applying the traditional methods to noisy photospheric magnetograms, in particular the horizontal components. In this paper, we construct magnetic structures for some filaments with the regularized Biot-Savart laws and calculate their magnetic twists. Moreover, we make a parameter survey for the flux ropes of the Titov-Démoulin-modified model to explore the factors affecting the twist of a force-free magnetic flux rope. It is found that the twist of a force-free flux rope, |T w |, is proportional to its axial length to minor radius ratio L/a, and is basically independent of the overlying background magnetic field strength. Thus, we infer that

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“…Since the distribution of the coronal and the photospheric magnetic fields play a dominant role in triggering coronal flux rope eruptions (Yeates 2014;Yang et al 2018;Thalmann et al 2019;Xing et al 2020), the influence of flux feeding processes on the major rope system should be sensitive to the scale of the magnetic field strength in the small rope. The magnetic parameters of the resultant flux ropes after the flux feeding processes with different C E are tabulated in Table 1.…”

Section: Initiation Of Eruptionsmentioning

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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Quantifying the Toroidal Flux of Preexisting Flux Ropes of Coronal Mass Ejections

Cited by 11 publications

References 92 publications

Estimating the Magnetic Structure of an Erupting CME Flux Rope From AR12158 Using Data-Driven Modeling

Estimating the Magnetic Structure of an Erupting CME Flux Rope From AR12158 Using Data-Driven Modeling

Magnetic Twists of Solar Filaments

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

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