Observational Evidence of the Kink Instability in Solar Filament Eruptions and Sigmoids

Rust, David M.; Labonte, B. J.

doi:10.1086/429379

Cited by 114 publications

(103 citation statements)

References 19 publications

(21 reference statements)

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“…It is very interesting that the observed helix is left-handed, which means that its sense of rotation agrees with the observed large-scale clockwise rotation of the erupting prominence. Hence, these observations give a strong support to the conversion of twist into writhe of the same sign in a kink-unstable magnetic flux-rope, as reported for instance by Rust & Labonte (2005); Zhou et al (2006).…”

Section: Discussionsupporting

confidence: 82%

Rotation of an erupting filament observed by the STEREO EUVI and COR1 instruments

Бемпорад

Mierla

Tripathi

2011

A&A

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On August 31, 2007, a prominence eruption was observed by the Solar TErrestrial RElations Observatory (STEREO) in the ExtremeUltraViolet Imager (EUVI) 304 images and later on, as the core of a three-part coronal mass ejection (CME) in images acquired by the inner STEREO coronagraph (COR1). Because they were covered by both STEREO spacecraft from right vantage points, these observations provide an excellent opportunity to perform a three-dimensional (3D) prominence reconstruction and study its evolution. We employed the tie-pointing technique to reconstruct the 3D shape and trajectory of the prominence, which has been followed from an heliocentric distance of ∼1.3 up to ∼2.4 R during the first 1.3 h of eruption. Data show evidence for a progressive clockwise prominence rotation by ∼90 • occurring not only in the early phase of the eruption sampled by EUVI, but also at larger heliocentric distances as seen by COR1. Interestingly, a counter-clockwise rotation of the filament was observed in Hα images in the week before the eruption; the filament does not show a twisted shape. In the same period, the potential field extrapolated at different times shows a clockwise rotation of closed lines overlying the filament. This suggests that a magnetic helicity storage occurred not in the filament itself, but in the global magnetic field configuration of the surrounding corona. Moreover, close inspection to the high-resolution EUVI images revealed a small scale helical feature along the erupting prominence. The sense of rotation of this helix agrees with the observed prominence rotation, providing evidence for the conversion of twist into writhe. The observed rotation of an erupting prominence, if representative of the flux rope rotation, may have a strong impact on the definition of geo-effectiveness of CMEs for space weather forecasting purposes.

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Section: Discussionsupporting

confidence: 82%

Rotation of an erupting filament observed by the STEREO EUVI and COR1 instruments

Бемпорад

Mierla

Tripathi

2011

A&A

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“…While many erupting filaments/flux-ropes appear to kink as they erupt (e.g. Rust & LaBonte 2005;, we are aware of no conclusive observational evidence that this eruption mechanism acts on its own. Initiation by an MHD instability without any field weakening by reconnection could be proved by observations of strong-field filament eruptions in which the impulsive phase is observed prior to any sign of X-ray or EUV brightening in the active region.…”

Section: Discussionmentioning

confidence: 91%

“…Moore & Roumeliotis 1992), external tether-cutting or "breakout" (Antiochos 1998;Antiochos et al 1999), or the flux cancelation model originally proposed by van Ballegooijen & Martens (1989) and further investigated by Linker et al (2003). Other models of filament eruptions include the kink instability of the filament/flux rope (Fan 2005;Rust & LaBonte 2005;. These models can be distinguished from each other mainly during the eruption initiation; they all tend to look the same during the eruption impulsive phase.…”

Section: Introductionmentioning

confidence: 99%

X-ray precursors to flares and filament eruptions

Chifor¹,

Tripathi²,

Mason³

et al. 2007

A&A

103

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Aims. To study preflare X-ray brightenings as diagnostics of the destabilisation of flare-associated erupting filaments/prominences. Methods. We combine new observations from the Transition Region and Coronal Explorer (TRACE) and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), as well as revisit events reported in the literature to date, in order to scrutinise the preflare activity during eight flare-associated filament eruptions. Results. The preflare activity occurs in the form of discrete, localised X-ray brightenings observed between 2 and 50 min before the impulsive phase of the flare and filament acceleration. These transient preflare brightenings are situated on or near (within 10 of) the polarity inversion line (PIL), coincident with emerging and/or canceling magnetic flux. The filaments begin to rise from the location of the preflare brightenings. In five out of eight events, the preflare brightenings were observed beneath the filament channel, close to the filament footpoint first observed to rise. Both thermal and nonthermal hard X-ray emissions during the preflare enhancement were detected with RHESSI, suggesting that both plasma heating and electron acceleration occurred at this time. The main energy release during the impulsive phase of the flare is observed close to (within 50 of) the preflare brightenings. The fast-rise phase of the filament eruption starts at the same time as the onset of the main flare or up to 5 min later. Conclusions. The preflare brightenings are precursors to the flare and filament eruption. These precursors represent distinct, localised instances of energy release, rather than a gradual energy release prior to the main flare. The X-ray precursors represent clearly observable signatures in the early stages of the eruption. Together with the timing of the filament fast-rise at or after the main flare onset, the X-ray precursors provide evidence for a tether-cutting mechanism initially manifested as localised magnetic reconnection being a common trigger for both flare emission and filament eruption.

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“…The idea of sigmoids being part of a kinked flux rope was supported by estimating the deformation of the kinked rope, which gave values consistent with the range observed for sigmoids (Török et al 2004). Observations of filament eruptions strongly suggested that a helical kink in flux rope topology was present (Ji et al 2003;Rust & LaBonte 2005;Williams et al 2005;Alexander et al 2006). Zhou et al (2006) described a clear case of two successive coronal mass ejections driven by the kink instability of an eruptive prominence.…”

Section: Introductionmentioning

confidence: 76%

Case study of a complex active-region filament eruption

et al. 2013

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Context. We investigated a solar active-region filament eruption associated with a C6.6 class flare and a coronal mass ejection (CME) in NOAA active region 08858 on 2000 February 9. Aims. We aim to better understand the relationship between filament eruptions and the associated flares and CMEs. Methods. Using BBSO, SOHO/EIT, and TRACE observational data, we analyzed the process of the active-region filament eruption in the chromosphere and the corona. Using the SOHO/MDI magnetograms, we investigated the change of the magnetic fields in the photosphere. Using the GOES soft X-ray flux and the SOHO/LASCO images, we identified the flare and CME, which were associated with this active-region filament eruption.Results. The brightenings in the chromosphere are a precursor of the filament expansion. The eruption itself can be divided into four phases: In the initial phase, the intertwined bright and dark strands of the filament expand. Then, the bright strands are divided into three parts with different expansion velocity. Next, the erupting filament-carrying flux rope expands rapidly and combines with the lower part of the expanding bright strands. Finally, the filament erupts accompanied by other dark strands overlying the filament.The overlying magnetic loops and the expansion of the filament strands can change the direction of the eruption. Conclusions. The time delay between the velocity peaks of the filament and that of the two parts of the bright strands clearly demonstrates that the breakup of the bright loops tying on the filament into individual strands is important for its eruption. The eruption is a collection of multiple processes that are physically coupled rather than a single process.

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Observational Evidence of the Kink Instability in Solar Filament Eruptions and Sigmoids

Cited by 114 publications

References 19 publications

Rotation of an erupting filament observed by the STEREO EUVI and COR1 instruments

Rotation of an erupting filament observed by the STEREO EUVI and COR1 instruments

X-ray precursors to flares and filament eruptions

Case study of a complex active-region filament eruption

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