Formation of a Compound Flux Rope by the Merging of Two Filament Channels, the Associated Dynamics, and Its Stability

Joshi, Navin Chandra; Magara, Tetsuya; Inoue, Satoshi

doi:10.1088/0004-637x/795/1/4

Cited by 42 publications

(39 citation statements)

References 39 publications

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“…In order to define the size, orientation, and location of the selected boxes we examined the post-flare loops in AIA 94Å images. As the post-flare arcades are believed to be the regions above which magnetic reconnection occurs (Liu et al, 2013;Joshi, Magara, and Inoue, 2014;Kumar et al, 2016b), we have selected our region of interest by enclosing the major post flare arcade structures seen in AIA 94Å images ( of these two values are greater than the noise level of ten Gauss on either of the two arrays, then the pixel that is in between these two minimum and maximum valued pixels is identified as the pixel tracing the PIL. These pixels were then joined to make the PIL.…”

Section: Discussionmentioning

confidence: 99%

A Comparative Study of the Eruptive and Non-eruptive Flares Produced by the Largest Active Region of Solar Cycle 24

Sarkar

Srivastava

2018

Sol Phys

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We investigate the morphological and magnetic characteristics of solar active region (AR) NOAA 12192. AR 12192 was the largest region of Solar Cycle 24; it underwent noticeable growth and produced 6 X-class flares, 22 M-class flares, and 53 C-class flares in the course of its disc passage. However, the most peculiar fact of this AR is that it was associated with only one CME in spite of producing several X-class flares. In this work, we carry out a comparative study between the eruptive and non-eruptive flares produced by AR 12192. We find that the magnitude of abrupt and permanent changes in the horizontal magnetic field and Lorentz force are significantly smaller in the case of the confined flares compared to the eruptive one. We present the areal evolution of AR 12192 during its disc passage. We find the flare-related morphological changes to be weaker during the confined flares, whereas the eruptive flare exhibits a rapid and permanent disappearance of penumbral area away from the magnetic neutral line after the flare. Furthermore, from the extrapolated nonlinear force-free magnetic field, we examine the overlying coronal magnetic environment over the eruptive and non-eruptive zones of the AR. We find that the critical decay index for the onset of torus instability was achieved at a lower height over the eruptive flaring region, than for the non-eruptive core area. These results suggest that the decay rate of the gradient of overlying magnetic field strength may play a decisive role to determine the CME productivity of the AR. In addition, the magnitude of changes in the flare-related magnetic characteristics are found to be well correlated with the nature of solar eruptions.

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Section: Discussionmentioning

confidence: 99%

A Comparative Study of the Eruptive and Non-eruptive Flares Produced by the Largest Active Region of Solar Cycle 24

Sarkar

Srivastava

2018

Sol Phys

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“…They also proposed that the merging interaction has significant reconnection involving mostly the azimuthal fields, and the two interacting flux tubes merge into one after the interaction. Filaments are believed to embed in the magnetic configurations of filament channels or flux ropes (Aulanier et al 2002;Liu et al 2012), and the merging interactions can occur between filaments along one common filament channel or along different filament channels (Martin et al 1994;Schmieder et al 2004;DeVore et al 2005;Aulanier et al 2006;Su et al 2007;Bone et al 2009;Chandra et al 2011;Jiang et al 2014;Joshi et al 2014Joshi et al , 2016. The newly-formed filament can eventually erupt, if it is destabilized by further magnetic cancellation at the footpoints (Litvinenko & Martin 1999;Martens & Zwaan 2001;DeVore et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Interaction of Two Filaments in a Long Filament Channel Associated with Twin Coronal Mass Ejections

Zheng¹,

Zhang²,

Chen³

et al. 2017

ApJ

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Using the high-quality observations of the Solar Dynamics Observatory, we present the interaction of two filaments (F1 and F2) in a long filament channel associated with twin coronal mass ejections (CMEs) on 2016 January 26. Before the eruption, a sequence of rapid cancellation and emergence of the magnetic flux has been observed, which likely triggered the ascending of the west filament (F1). The east footpoints of rising F1 moved toward the east far end of the filament channel, accompanying with post-eruption loops and flare ribbons. It likely indicated a large-scale eruption involving the long filament channel, resulted from the interaction between F1 and the east filament (F2). Some bright plasma flew over F2, and F2 stayed at rest during the eruption, likely due to the confinement of its overlying lower magnetic field. Interestingly, the impulsive F1 pushed its overlying magnetic arcades to form the first CME, and F1 finally evolved into the second CME after the collision with the nearby coronal hole. We suggest that the interaction of F1 and the overlying magnetic field of F2 led to the merging reconnection that form a longer eruptive filament loop. Our results also provide a possible picture of the origin of twin CMEs, and show the large-scale magnetic topology of the coronal hole is important for the eventual propagation direction of CMEs.

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“…The merging of two filament channels after dynamic interactions has also been observed by Schmieder et al (2004), Bone et al (2009), Jiang et al (2014a, and Joshi et al (2014a). Schmieder et al (2004) found evidence of a merging of two segments with dextral chiralities to form a long dextral filament.…”

Section: Introductionmentioning

confidence: 59%

“…Filaments exist in the magnetic dips within magnetic configurations known as filament channels or flux ropes (Aulanier et al 2002;Liu et al 2012). Filaments and/or associated channels sometimes interact and show interesting dynamics in the chromosphere and low corona (Uralov et al 2002;Schmieder et al 2004;Su et al 2007;Bone et al 2009;Kumar et al 2010;Liu et al 2010;Chandra et al 2011;Filippov 2011;Li & Ding 2012;Jiang et al 2013Jiang et al , 2014Joshi et al 2014a). During an interaction under specific conditions, these magnetic structures can reconnect and change their footpoint connectivity.…”

Section: Introductionmentioning

confidence: 99%

“…Recently, Jiang et al (2014) reported the interaction and merging of two sinistral filaments on 2001 December 6, and found that they form a new long magnetic channel. More recently, Joshi et al (2014a) reported an interesting dynamic event of the merging of two filament channels and formation of a long compound flux rope on 2014 January 1. On the basis of numerical simulations, some authors discussed various conditions necessary for the interaction/merging of filaments.…”

Section: Introductionmentioning

confidence: 99%

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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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Formation of a Compound Flux Rope by the Merging of Two Filament Channels, the Associated Dynamics, and Its Stability

Cited by 42 publications

References 39 publications

A Comparative Study of the Eruptive and Non-eruptive Flares Produced by the Largest Active Region of Solar Cycle 24

A Comparative Study of the Eruptive and Non-eruptive Flares Produced by the Largest Active Region of Solar Cycle 24

Interaction of Two Filaments in a Long Filament Channel Associated with Twin Coronal Mass Ejections

Interaction of Two Filament Channels of Different Chiralities

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