Solar Magnetic Flux Ropes

Filippov, B. P.; Martsenyuk, O. V.; Srivastava, A. K.; Uddin, Wahab

doi:10.1007/s12036-015-9321-5

Cited by 47 publications

(34 citation statements)

References 137 publications

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“…Our resulting magnetic field also shows a certain separation between the flux rope axis and top most dips as suggested by cavity observations (Hudson et al 1999;Régnier et al 2011;Gibson 2015;Filippov et al 2015;Su et al 2015;Bak-Steslicka et al 2016). This is due to the curved geometry of the flux rope.…”

Section: Resultssupporting

confidence: 79%

The Apparent Critical Decay Index at the Onset of Solar Prominence Eruptions

Zuccarello

Aulanier

Gilchrist

2016

ApJL

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A magnetic flux rope (MFR) embedded in a line-tied external magnetic field that decreases with height asz n is unstable to perturbations if the decay index of the field n is larger than a critical value. The onset of this instability, called torus instability, is one of the main mechanisms that can initiate coronal mass ejections. Since flux ropes often possess magnetic dips that can support prominence plasma, this is also a valuable mechanism to trigger prominence eruptions. Magnetohydrodynamic (MHD) simulations of the formation and/or emergence of MFRs suggest a critical value for the onset of the instability in the range [1.4−2]. However, detailed observations of prominences suggest a value in the range [0.9−1.1]. In this Letter, by using a set of MHD simulations, we show why the large discrepancy between models and observations is only apparent. Our simulations indeed show that the critical decay index at the onset of the eruption is =  n 1.4 0.1 when computed at the apex of the flux rope axis, while it is =  n 1.1 0.1 when it is computed at the altitude of the topmost part of the distribution of magnetic dips. The discrepancy only arises because weakly twisted curved flux ropes do not have dips up to the altitude of their axis.

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Section: Resultssupporting

confidence: 79%

The Apparent Critical Decay Index at the Onset of Solar Prominence Eruptions

Zuccarello

Aulanier

Gilchrist

2016

ApJL

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“…Using New Solar Telescope (NST) observations, Wang et al (2015) also found that a set of loops developed into a flux rope before a two-ribbon flare. Filippov et al (2015) presented several filaments with highly twisted magnetic structure observed by the Transition Region And Coronal Explorer (TRACE) and Big Bear Solar Observatory (BBSO). These observations reveal that flux ropes may be ubiquitous in the solar atmosphere (Zhang et al 2015a).…”

Section: Introductionmentioning

confidence: 99%

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

Yan

Jiang

Xue

et al. 2017

ApJ

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Solar flares and coronal mass ejections are the most powerful explosions in the Sun. They are major sources of potentially destructive space weather conditions. However, the possible causes of their initiation remain controversial. Using high-resolution data observed by the New Solar Telescope of Big Bear Solar Observaotry, supplemented by Solar Dynamics Observatory observations, we present unusual observations of a small-scale emerging flux rope near a large sunspot, whose eruption produced an M-class flare and a coronal mass ejection. The presence of the small-scale flux rope was indicated by static nonlinear force-free field extrapolation as well as data-driven magnetohydrodynamics modeling of the dynamic evolution of the coronal three-dimensional magnetic field. During the emergence of the flux rope, rotation of satellite sunspots at the footpoints of the flux rope was observed. Meanwhile, the Lorentz force, magnetic energy, vertical current, and transverse fields were increasing during this phase. The free energy from the magnetic flux emergence and twisting magnetic fields is sufficient to power the M-class flare. These observations present, for the first time, the complete process, from the emergence of the small-scale flux rope, to the production of solar eruptions.

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“…In our interpretation of these observations we follow the flux-rope model (e.g., Canou & Amari 2010;Guo et al 2010;Joshi et al 2014b;Filippov et al 2015) of filaments, considering filament plasma accumulated in lower parts of helical flux tubes. Dextral filaments are contained within the left-handed helices, while sinistral filaments fill the righthanded ones.…”

Section: Interpretation and Discussionmentioning

confidence: 99%

“…The interaction of two nearby filament channels with different filament chiralities within a large-scale coronal fanspine magnetic structure have not been observed before, although fan-spine configurations have been discussed in the case of solar eruptions in "pseudostreamers" (Wang et al 2007;Török et al 2011b;Rachmeler et al 2014;Yang et al 2015), jets (Filippov et al 2009(Filippov et al , 2015Pariat et al 2009), and flares Joshi et al 2015).…”

Section: The Observations As Well As the Pfss Calculations Clearlymentioning

confidence: 99%

Interaction of Two Filament Channels of Different Chiralities

Joshi

Filippov

Schmieder

et al. 2016

ApJ

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We present observations of the interactions between the two filament channels of different chiralities and associated dynamics that occurred during 2014 April 18-20. While two flux ropes of different helicity with parallel axial magnetic fields can only undergo a bounce interaction when they are brought together, the observations at first glance show that the heated plasma is moving from one filament channel to the other. The SDO/AIA 171 Å observations and the potential-field source-surface magnetic field extrapolation reveal the presence of a fan-spine magnetic configuration over the filament channels with a null point located above them. Three different events of filament activations, partial eruptions, and associated filament channel interactions have been observed. The activation initiated in one filament channel seems to propagate along the neighboring filament channel. We believe that the activation and partial eruption of the filaments brings the field lines of flux ropes containing them closer to the null point and triggers the magnetic reconnection between them and the fan-spine magnetic configuration. As a result, the hot plasma moves along the outer spine line toward the remote point. Utilizing the present observations, for the first time we have discussed how two different-chirality filament channels can interact and show interrelation.

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Solar Magnetic Flux Ropes

Cited by 47 publications

References 137 publications

The Apparent Critical Decay Index at the Onset of Solar Prominence Eruptions

The Apparent Critical Decay Index at the Onset of Solar Prominence Eruptions

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

Interaction of Two Filament Channels of Different Chiralities

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