Blowout Surge due to Interaction between a Solar Filament and Coronal Loops

Li, Haidong; Jiang, Yong; Yang, Jiayan; Qu, Zhining; Yang, Bo; Xu, Zhe; Bi, Yong; Hong, Jiang; Chen, Hechao

doi:10.3847/2041-8213/aa762c

Cited by 37 publications

(28 citation statements)

References 49 publications

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“…Taken together with the results of Panesar et al [66][67][68] they also claim that flux cancellation is the main process whereby the energy is stored prior to eruption in all jets and CMEs, and may also be involved in the triggering process. So far, the finding of blowout jets has been confirmed by many observational studies, and now we recognize that the vast majority of solar jets are caused by magnetic flux cancellation rather than flux emergence [63,[69][70][71][72][73][74][75][76][77][78][79][80][81][82][83][84]. Recently, high-resolution observational studies have shown that two-sided-loop jets are also associated with flux cancellations and include the eruption of mini-filaments inside the base arches [44,46,49,85,86], and two-sidedloop jets occurring in filament channels may be important for causing the eruption of large filaments [87].…”

Section: Observational Feature (A) Morphology and Classificationmentioning

confidence: 99%

“…Shen et al [63,69] studied two blowout jets and found that the erupting mini-filaments directly form the cool component of coronal jets (figure 2). Recently, more and more observational studies have confirmed that blowout jets are driven by mini-filament eruptions or filament channels [73][74][75][76][77][78][79][80][81][82][83][84]97,98]; some authors even proposed that all coronal jets originate from mini-filament eruptions, and their generation resembles the eruption of large-scale, energetic filament/CME eruptions [36,65,99].…”

Section: (B) Precursormentioning

confidence: 99%

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Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

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The solar atmosphere is full of complicated transients manifesting the reconfiguration of the solar magnetic field and plasma. Solar jets represent collimated, beam-like plasma ejections; they are ubiquitous in the solar atmosphere and important for our understanding of solar activities at different scales, the magnetic reconnection process, particle acceleration, coronal heating, solar wind acceleration, as well as other related phenomena. Recent high-spatio-temporal-resolution, wide-temperature coverage and spectroscopic and stereoscopic observations taken by ground-based and space-borne solar telescopes have revealed many valuable new clues to restrict the development of theoretical models. This review aims at providing the reader with the main observational characteristics of solar jets, physical interpretations and models, as well as unsolved outstanding questions in future studies.

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Section: Observational Feature (A) Morphology and Classificationmentioning

confidence: 99%

Section: (B) Precursormentioning

confidence: 99%

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

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“…Therefore, we suspect that there is a close relationship between the jets and the flux emergence. More and more observational evidences and numerical simulations manifest that the jets can be triggered by the magnetic reconnection between the emerging flux and the pre-existing magnetic flux (Yokoyama & Shibata 1995;Shimojo et al 1998;Cheung & Isobe 2014;Li et al 2017).…”

Section: Formation Process Of the Active-region Filamentmentioning

confidence: 99%

Formation and material supply of an active-region filament associated with newly emerging flux

Wang

Yan

Guo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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With the observations of S DO/AIA 304 Å and NVST Hα bands, we present the formation process of an active-region filament in active region NOAA 11903 during the period from 02:00 UT to 10:00 UT on November 25, 2013. A series of jets occurring in the vicinity of the south-western footpoint of the filament directly ejected cool and hot plasma to filament height and supplied material for the filament. Some newly emerging flux is found in the vicinity of the filament south-western footpoint during these jets. In this paper, we mainly focus on the material supply of the filament. The plasma mass uploaded by the jets and the mass of the filament are estimated, which manifests the fact that the mass carried by jets can supply sufficient material for the formation of the filament. We found two types of jets. one is Hα jet, and the other is EUV jet. The significant finding is that some cool jets seen in the Hα band but not in the SDO/AIA bands also could eject the cool material for the filament. These results suggest that cool plasma in the low atmosphere can be directly injected into the upper atmosphere and become the filament material by two types of jets. Moreover, the newly emerging flux with non-potential field plays an important role in the appearances of the jets and the magnetic structure of the filament.

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“…Xue et al (2017) analyzed a tether-cutting reconnection event that results in the formation of a flux rope. While magnetic reconnection is believed to occur in fan-spine configuration where there may be a mini-filament under the null point, and it can reconnect with spine lines and then form a jet (Joshi et al 2015;Li et al 2017;Xu et al 2017). Although magnetic reconnections associated with filaments, including small-scale filaments, are often reported during their eruptions (e.g., Joshi et al 2018;Yang et al 2017), the detailed process of magnetic reconnection is rarely noticed in the previous studies.…”

Section: Introductionmentioning

confidence: 97%

A solar filament disconnected by magnetic reconnection

Xue

Yan

Yang

et al. 2020

A&A

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Aims. We aim to study a high-resolution observation of an asymmetric inflow magnetic reconnection between a filament and its surrounding magnetic loops in active region NOAA 12436 on 2015 October 23. Methods. We analyzed the multiband observations of the magnetic reconnection obtained by the New Vacuum Solar Telescope (NVST) and the Solar Dynamic Observatory. We calculated the NVST Hα Dopplergrams to determine the Doppler properties of the magnetic reconnection region and the rotation of a jet. Results. The filament firstly becomes active and then approaches its southwestern surrounding magnetic loops (L1) with a velocity of 9.0 km s−1. During this period, the threads of the filament become loose in the reconnection region and then reconnect with L1 in turn. L1 is pressed backward by the filament with a velocity of 5.5 km s−1, and then the magnetic reconnection occurs between them. A set of newly formed loops are separated from the reconnection site with a mean velocity of 127.3 km s−1. In the middle stage, some threads of the filament return back first with a velocity of 20.1 km s−1, and others return with a velocity of 4.1 km s−1 after about 07:46 UT. Then, L1 also begins to return with a velocity of 3.5 km s−1 at about 07:47 UT. At the same time, magnetic reconnection continues to occur between them until 07:51 UT. During the reconnection, a linear typical current sheet forms with a length of 5.5 Mm and a width of 1.0 Mm, and a lot of hot plasma blobs are observed propagating from the typical current sheet. During the reconnection, the plasma in the reconnection region and the typical current sheet always shows redshifted feature. Furthermore, the material and twist of the filament are injected into the newly longer-formed magnetic loops by the magnetic reconnection, which leads to the formation of a jet, and its rotation. Conclusions. The observational evidence for the asymmetric inflow magnetic reconnection is investigated. We conclude that the magnetic reconnection does occur in this event and results in the disconnection of the filament. The looseness of the filament may be due to the pressure imbalance between the inside and outside of the filament. The redshifted feature in the reconnection site can be explained by the expansion of the right flank of the filament to the lower atmosphere because of the complex magnetic configuration in this active region.

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Blowout Surge due to Interaction between a Solar Filament and Coronal Loops

Cited by 37 publications

References 49 publications

Observation and modelling of solar jets

Observation and modelling of solar jets

Formation and material supply of an active-region filament associated with newly emerging flux

A solar filament disconnected by magnetic reconnection

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