Case study of a complex active-region filament eruption

XL, Yan; ZQ, Qu; DF, Kong; LH, Deng; Xue, Zhike

doi:10.1051/0004-6361/201219032

Cited by 12 publications

(4 citation statements)

References 53 publications

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“…Solar filaments/prominences are one of the most common structures in the corona, which may lead to energetic coronal mass ejections (CMEs) and flares when they erupt (Chen & Shibata 2000;Forbes 2000;Lin & Forbes 2000;Yan et al 2013;Xue et al 2016;Yang et al 2017). They appear at the limb as bright features called prominences.…”

Section: Introductionmentioning

confidence: 99%

Formation of an Active Region Filament Driven By a Series of Jets

Wang

Yan

et al. 2018

ApJ

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We present a formation process of a filament in active region NOAA 12574 during the period from 2016 August 11 to 12. Combining the observations of GONG Hα, Hida spectrum and SDO/AIA 304 A, the formation process of the filament is studied. It is found that cool material (T ∼ 10 4 K) is ejected by a series of jets originating from the western foot-point of the filament. Simultaneously, the magnetic flux emerged from the photosphere in the vicinity of the western foot-point of the filament. These observations suggest that cool material in the low atmosphere can be directly injected into the upper atmosphere and the jets are triggered by the magnetic reconnection between pre-existing magnetic fields and new emerging magnetic fields. Detailed study of a jet at 18:02 UT on August 11 with GST/BBSO TiO observations reveals that some dark threads appeared in the vicinity of the western foot-point after the jet and the projection velocity of plasma along the filament axis was about 162.6±5.4 km/s. Using with DST/Hida observations, we find that the injected plasma by a jet at 00:42 UT on August 12 was rotating. Therefore, we conclude that the jets not only supplied the material for the filament, but also injected the helicity into the filament simultaneously. Comparing the quantity of mass injection by the jets with the mass of the filament, we conclude that the estimated mass loading by the jets is sufficient to account for the mass in the filament.

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Section: Introductionmentioning

confidence: 99%

Formation of an Active Region Filament Driven By a Series of Jets

Wang

Yan

et al. 2018

ApJ

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“…Typically, transient X-ray brightenings, so-called preflares, are observed before the flares (Chifor et al 2007;Sterling et al 2011), which are coincident with magnetic cancellation or emerging magnetic flux (Schmieder et al 2008). Moreover, Yan et al (2013) suggested that the brightening in the chromosphere before the filament expansion may indicate the onset of TC reconnection. And Chen et al (2018) detected obvious brightenings in UV bands and hot outflows in the chromosphere, which showed the preflare reconnection process of the partial eruptions.…”

Section: Interpretation and Discussionmentioning

confidence: 99%

“…Typically, filament eruptions are preceded by their precursor activities (Chen 2011), such as darkening and widening (Martin 1980), reconnection-favored emerging flux (Feynman & Martin 1995), large-amplitude oscillation (Chen et al 2008;Zhang et al 2012), heating and particle acceleration (Hernandez-Perez et al 2019), and soft X-ray (SXR) brightening (Mitra et al 2020). In addition, EUV or chromosphere brightenings inside the filament or its close vicinity are also considered as precursors (Sterling & Moore 2005;Alexander et al 2006;Sterling et al 2011;Yan et al 2013;Wang et al 2018;Devi et al 2020).…”

Section: Introductionmentioning

confidence: 99%

A Partial Filament Eruption in Three Steps Induced by External Magnetic Reconnection

Dai

Wang

et al. 2022

ApJ

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We present an investigation of partial filament eruption on 2012 June 17 in the active region NOAA 11504. For the first time, we observed the vertical splitting process during the partial eruption with high-resolution narrowband images at 10830 Å. The active filament was rooted in a small δ-sunspot of the active region. Particularly, it underwent the partial eruption in three steps, i.e., the precursor, the first eruption, and the second eruption, while the latter two were associated with a C1.0 flare and a C3.9 flare, respectively. During the precursor, slow magnetic reconnection took place between the filament and the adjoining loops that also rooted in the δ-sunspot. The continuous reconnection not only caused the filament to split into three groups of threads vertically but also formed a new filament, which was growing and accompanied brightening took place around the site. Subsequently, the growing filament erupted together with one group splitted threads, resulted in the first eruption. At the beginning of the first eruption, a subsequent magnetic reconnection occurred between the erupting splitted threads and another ambient magnetic loop. After about 3 minutes, the second eruption occurred as a result of the eruption of two larger unstable filaments induced by the magnetic reconnection. The high-resolution observation provides a direct evidence that magnetic reconnection between filament and its ambient magnetic fields could induce the vertical splitting of the filament, resulting in partial eruption.

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“…With typical temperatures of around ∼6000 K and densities of ∼10 11 cm −3 (Munro et al 1979;Gopalswamy et al 2003;, they are usually located above magnetic polarity inversion lines (PILs) and are believed to be supported by the magnetic tension force provided by concave upward magnetic dips (Low & Hundhausen 1995;Démoulin & Aulanier 2010;Ichimoto et al 2023). When disturbed, they can undergo eruptions and result in the formation of flares and coronal mass ejections (CMEs), which can have significant impacts on the Earth and planetary space environments (Yan et al 2013;Sun et al 2022;Yang et al 2023). Therefore, investigating the eruption processes of solar filaments is essential for a better understanding of their effects on space weather.…”

Section: Introductionmentioning

confidence: 99%

Observation of Two Splitting Processes in a Partial Filament Eruption on the Sun: The Role of Breakout Reconnection

Sun

Hou

et al. 2023

ApJ

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Partial filament eruptions have often been observed; however, the physical mechanisms that lead to filament splitting are not yet fully understood. In this study, we present a unique event of a partial filament eruption that undergoes two distinct splitting processes. The first process involves vertical splitting and is accompanied by brightenings inside the filament, which may result from internal magnetic reconnection within the filament. Following the first splitting process, the filament is separated into an upper part and a lower part. Subsequently, the upper part undergoes a second splitting, which is accompanied by a coronal blowout jet. An extrapolation of the coronal magnetic field reveals a hyperbolic flux tube structure above the filament, indicating the occurrence of breakout reconnection that reduces the constraining field above. Consequently, the filament is lifted up, but at a nonuniform speed. The high-speed part reaches the breakout current sheet to generate the blowout jet, while the low-speed part falls back to the solar surface, resulting in the second splitting. In addition, continuous brightenings are observed along the flare ribbons, suggesting the occurrence of a slipping reconnection process. This study presents, for the first time, the unambiguous observation of a two-stage filament-splitting process, advancing our understanding of the complex dynamics of solar eruptions.

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Case study of a complex active-region filament eruption

Cited by 12 publications

References 53 publications

Formation of an Active Region Filament Driven By a Series of Jets

Formation of an Active Region Filament Driven By a Series of Jets

A Partial Filament Eruption in Three Steps Induced by External Magnetic Reconnection

Observation of Two Splitting Processes in a Partial Filament Eruption on the Sun: The Role of Breakout Reconnection

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