Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a Cme

Panesar, Navdeep K.; Sterling, Alphonse C.; Innes, D. E.; Moore, Ronald L.

doi:10.1088/0004-637x/811/1/5

Cited by 14 publications

(10 citation statements)

References 60 publications

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“…The minifilaments show a slow-rise, followed by a fast-rise as they erupt (MOVIE1 and MOVIE2), analogous to many longer-scale filament eruptions (e.g. Sterling & Moore 2005;Panesar et al 2015). Table 1; (g-i) show HMI magnetograms of the same region.…”

Section: Evolution Of Minifilaments and Jetsmentioning

confidence: 91%

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

Panesar¹,

Sterling²,

Moore³

et al. 2016

ApJL

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We report observations of ten random on-disk solar quiet region coronal jets found in high resolution Extreme Ultraviolet (EUV) images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and having good coverage in magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). Recent studies show that coronal jets are driven by the eruption of a small-scale filament (called a minifilament). However the trigger of these eruptions is still unknown. In the present study we address the question: what leads to the jet-driving minifilament eruptions? The EUV observations show that there is a cool-transitionregion-plasma minifilament present prior to each jet event and the minifilament eruption drives the jet. By examining pre-jet evolutionary changes in the line-of-sight photospheric magnetic field we observe that each pre-jet minifilament resides over the neutral line between majority-polarity and minority-polarity patches of magnetic flux. In each of the ten cases, the opposite-polarity patches approach and merge with each other (flux reduction between 21 and 57%). After several hours, continuous flux cancellation at the neutral line apparently destabilizes the field holding the cool-plasma minifilament to erupt and undergo internal reconnection, and external reconnection with the surrounding-coronal field. The external reconnection opens the minifilament field allowing the minifilament material to escape outwards, forming part of the jet spire. Thus we found that each of the ten jets resulted from eruption of a minifilament following flux cancellation at the neutral line under the minifilament. These observations establish that magnetic flux cancellation is usually the trigger of quiet region coronal jet eruptions.

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Section: Evolution Of Minifilaments and Jetsmentioning

confidence: 91%

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

Panesar¹,

Sterling²,

Moore³

et al. 2016

ApJL

Self Cite

130

249

View full text Add to dashboard Cite

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“…Moreover, even if one could predict that a certain trigger mechanism will take place, it would still be hard to predict whether an eruption will produce a CME or remains confined (e.g., Moore et al, 2001;Török and Kliem, 2005;Guo et al, 2010) as we know little about the conditions under which trigger mechanisms can succeed in switching on driving mechanisms. In fact, it seems that, at least in some events, several confined eruptions are required before a full eruption can occur (e.g., Panesar et al, 2015;Chintzoglou et al, 2015;Liu et al, 2016).…”

Section: Initiation Mechanisms Of Solar Eruptionsmentioning

confidence: 99%

The Origin, Early Evolution and Predictability of Solar Eruptions

Green¹,

et al. 2018

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Coronal mass ejections (CMEs) were discovered in the early 1970s when spaceborne coronagraphs revealed that eruptions of plasma are ejected from the Sun. Today, it is known that the Sun produces eruptive flares, filament eruptions, coronal mass ejections and failed eruptions; all thought to be due to a release of energy stored in the coronal magnetic field during its drastic reconfiguration. This review discusses the observations and physical mechanisms behind this eruptive activity, with a view to making an assessment of the current capability of forecasting these events for space weather risk and impact mitigation. Whilst a wealth of observations exist, and detailed models have been developed, there still exists a need to draw these approaches together. In particular more realistic models are encouraged in order to asses the full range of complexity of the solar atmosphere and the criteria for which an eruption is formed. From the observational side, a more detailed understanding of the role of photospheric flows and reconnection is needed in order to identify the evolutionary path that ultimately means a magnetic structure will erupt.

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“…This follows from the finding that a full eruption requires a certain fraction of the active-region flux to reside in the current-carrying, erupting flux (Bobra et al 2008;Savcheva & van Ballegooijen 2009;Su et al 2011). Alternatively, a part of the stabilizing overlying flux can be removed, as conjectured, e.g., in Panesar et al (2015), but this requires a multipolar source structure and an external agent (see, e.g., Török et al 2011), which jointly exist only in a minority of the eruptions. If the flare associated with the confined eruption involves the standard flare reconnection, which can be inferred from the formation of flare ribbons and loops, then the addition of flux is already initiated by the flare reconnection of the confined eruption itself.…”

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

confidence: 99%

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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Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares Leading to a Cme

Cited by 14 publications

References 60 publications

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

The Origin, Early Evolution and Predictability of Solar Eruptions

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

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