Confined Partial Filament Eruption and Its Reformation Within a Stable Magnetic Flux Rope

Joshi, Navin Chandra; Srivastava, A. K.; Filippov, B. P.; Kayshap, Pradeep; Uddin, Wahab; Chandra, Ramesh; Choudhary, Debi Prasad; Dwivedi, B. N.

doi:10.1088/0004-637x/787/1/11

Cited by 60 publications

(33 citation statements)

References 51 publications

(102 reference statements)

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“…Photospheric magnetic cancellation (van Ballegooijen & Martens 1989) and the coronal tether-cutting reconnection (Sturrock et al 1984;Moore et al 2001) are two main mechanisms known for the buildup as well as the initial rising of sigmoid structures in the solar corona. Several studies have been performed showing the formation of sigmoid with these mechanisms (Inoue et al 2011;Liu et al 2012Liu et al , 2013Joshi et al 2014aJoshi et al , 2014bVemareddy & Zhang 2014). Other mechanisms such as torus instability (Kliem & Török 2006), kink instability (Török et al 2004), and the magnetic breakout (Antiochos et al 1999) are well known to drive the eruptions.…”

Section: Introductionmentioning

confidence: 99%

The Role of Erupting Sigmoid in Triggering a Flare With Parallel and Large-Scale Quasi-Circular Ribbons

Joshi

Liu

Sun

et al. 2015

ApJ

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In this paper, we present observations and analysis of an interesting sigmoid formation, eruption, and the associated flare that occurred on 2014 April 18 using multi-wavelength data sets. We discuss the possible role of the sigmoid eruption in triggering the flare, which consists of two different sets of ribbons: parallel ribbons and a large-scale quasi-circular ribbon. Several observational evidence and nonlinear force-free field extrapolation results show the existence of a large-scale fan-spine type magnetic configuration with a sigmoid lying under a section of the fan dome. The event can be explained with the following two phases. During the preflare phase, we observed the formation and appearance of the sigmoid via tether-cutting reconnection between the two sets of sheared fields under the fan dome. The second, main flare phase features the eruption of the sigmoid, the subsequent flare with parallel ribbons, and a quasi-circular ribbon. We propose the following multi-stage successive reconnection scenario for the main flare. First, tether-cutting reconnection is responsible for the formation and the eruption of the sigmoid structure. Second, the reconnection occurring in the wake of the erupting sigmoid produces the parallel flare ribbons on the both sides of the circular polarity inversion line. Third, the null-type reconnection higher in the corona, possibly triggered by the erupting sigmoid, leads to the formation of a large quasi-circular ribbon. For the first time, we suggest a mechanism for this type of flare consisting of a double set of ribbons triggered by an erupting sigmoid in a large-scale fan-spine-type magnetic configuration.

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Section: Introductionmentioning

confidence: 99%

The Role of Erupting Sigmoid in Triggering a Flare With Parallel and Large-Scale Quasi-Circular Ribbons

Joshi

Liu

Sun

et al. 2015

ApJ

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“…It is debated whether the flux rope exists before a filament eruption or forms during the eruption. Further, there is also a class of eruptive filaments in which only a part of a filament erupts (e.g., Joshi et al 2014) or there is a failed eruption (Török & Kliem 2005). Such eruptions are modeled by simulations of partial flux rope eruptions (Gibson & Fan 2006).…”

Section: Introductionmentioning

confidence: 99%

Interrupted Eruption of Large Quiescent Filament Associated With a Halo Cme

Gosain

Filippov

Maurya

et al. 2016

ApJ

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We analyze the observations of an eruptive quiescent filament associated with a halo Coronal Mass Ejection (CME). We use observations from the Atmospheric Imaging Assembly (AIA) instrument onboard the Solar Dynamics Observatory (SDO), Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO), and the Solar Terrestrial Relations Observatory (STEREO A/B) satellites. The filament exhibits a slow-rise phase followed by a gradual acceleration and then completely disappears. The filament could be traced in STEREO observations up to an altitude of about 1.44  R , where its rise speed reached ∼14 km s −1 and disappeared completely at about 10:32 UT on 2011 October 21. The CME associated with the filament eruption and two bright ribbons in the chromosphere both appeared at about 01:30 UT on October 22, i.e., 15 hr after the filament eruption was seen in He II 304 Å filtergrams. We show that this delay is abnormally large even if the slow rise speed and slow acceleration of the filament are taken into account. To understand the cause of this delay, we compute the decay index (n) of the overlying coronal magnetic field. The height distribution of the decay index, n, suggests that the zone of instability ( > n 1) at a lower altitude, 144-480 Mm, is followed by a zone of stability ( < n 1) between 540 and 660 Mm. We interpret the observed delay to be due to the presence of the latter zone, i.e., the zone of stability, which could provide a second quasi-equilibrium state to the filament until it finally erupts.

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“…Recently, the direct observations of flux ropes in the low corona have been reported (Li and Zhang, 2013a, 2013cChen et al, 2014aChen et al, , 2014bSong et al, 2014;Joshi et al, 2014b) by using the extreme ultraviolet (EUV) data from the Atmospheric Imaging Assembly (AIA; Lemen et al, 2012) onboard the Solar Dynamics Observatory (SDO; Pesnell et al, 2012). Kumar et al (2010) presented a successive activation of magnetic flux ropes in chromospheric and EUV lines and concluded that such activation plays an important role in triggering the flare.…”

Section: Introductionmentioning

confidence: 99%

High-Resolution Observations of a Flux Rope with the Interface Region Imaging Spectrograph

Zhang

2015

Sol Phys

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We report the observations of a flux rope at transition region temperatures with the Interface Region Imaging Spectrograph (IRIS) on 30 August 2014. Initially, magnetic flux cancellation constantly took place and a filament was activated. Then the bright material from the filament moved southward and tracked out several fine structures. These fine structures were twisted and tangled with each other, and appeared as a small flux rope at 1330Å, with a total twist of about 4π. Afterwards, the flux rope underwent a counter-clockwise (viewed top-down) unwinding motion around its axis. Spectral observations of C ii 1335.71Å at the southern leg of the flux rope showed that Doppler redshifts of 6−24 km s −1 appeared at the western side of the axis, which is consistent with the counter-clockwise rotation motion. We suggest that the magnetic flux cancellation initiates reconnection and some activation of the flux rope. The stored twist and magnetic helicity of the flux rope are transported into the upper atmosphere by the unwinding motion in the late stage. The small-scale flux rope (width of 8.3′′ ) had a cylindrical shape with helical field lines, similar to the morphology of the large-scale CME core (width of 1.54 R ⊙ ) on 2 June 1998. This similarity shows the presence of flux ropes of different scales on the Sun.

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Confined Partial Filament Eruption and Its Reformation Within a Stable Magnetic Flux Rope

Cited by 60 publications

References 51 publications

The Role of Erupting Sigmoid in Triggering a Flare With Parallel and Large-Scale Quasi-Circular Ribbons

The Role of Erupting Sigmoid in Triggering a Flare With Parallel and Large-Scale Quasi-Circular Ribbons

Interrupted Eruption of Large Quiescent Filament Associated With a Halo Cme

High-Resolution Observations of a Flux Rope with the Interface Region Imaging Spectrograph

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