A Complex Solar Coronal Jet with Two Phases

Chen, Jie; Su, Jiangtao; Deng, Yuanyong; Priest, E. R.

doi:10.3847/1538-4357/aa6c59

Cited by 13 publications

(10 citation statements)

References 41 publications

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“…Sterling et al (2015) mention that a likely trigger of the eruption is magnetic flux cancelation in the feet of the magnetic field in and around the minifilament flux rope, and Panesar et al (2016Panesar et al ( , 2018 have presented compelling evidence that in most coronal jets in quiet regions and coronal holes flux cancelation at the polarity inversion line under the pre--jet minifilament triggers the eruption. The results of Panesar et al (2016Panesar et al ( , 2018 are from 23 randomly selected jets, and are consistent with many recent studies of smaller samples of jets in which there is evidence for flux cancelation being the trigger (e.g., Young & Muglach 2014a, 2014bChen & Innes 2016;Chen et al 2017;Zhu et al 2017;Chandra et al 2017). The present paper is a direct follow--on to the Sterling et al (2015) paper.…”

supporting

confidence: 90%

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Moore

Sterling

Panesar

2018

ApJ

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We follow up on the Sterling et al (2015) discovery that nearly all polar coronal X--ray jets are made by an explosive eruption of closed magnetic field carrying a miniature filament in its core. In the same X--ray and EUV movies used by Sterling et al (2015), we examine the onset and growth of the driving magnetic explosion in 15 of the 20 jets that they studied. We find evidence that: (1) in a large majority of polar X--ray jets, the runaway internal/tether--cutting reconnection under the erupting minifilament flux rope starts after both the minifilament's rise and the spire--producing external/breakout reconnection have started; and (2) in a large minority, (a) before the eruption starts there is a current sheet between the explosive closed field and the ambient open field, and (b) the eruption starts with breakout reconnection at that current sheet. The variety of event sequences in the eruptions supports the idea that the magnetic explosions that make polar X--ray jets work the same way as the much larger magnetic explosions that make a flare and coronal mass ejection (CME). That idea, and recent observations indicating that magnetic flux cancelation is the fundamental process that builds the field in and around the pre--jet mininfilament and triggers that field's jet--driving explosion, together suggest that flux cancelation inside the magnetic arcade that explodes in a flare/CME eruption is usually the fundamental process that builds the explosive field in the core of the arcade and triggers that field's explosion.

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supporting

confidence: 90%

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Moore

Sterling

Panesar

2018

ApJ

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“…Chen et al ( 2017) observed a complex jet with two intrinsic phases to the west of NOAA AR 11 513 on July 2, 2012 with high spatial resolution using data obtained by Atmospheric Imaging Assembly (AIA) (Lemen et al, 2012) on-board the Solar Dynamics Observatory (SDO) and analyzed the driving mechanism of the jet. In this paper, we report the observation of multiple blobs and analyze the evolution of the detected blobs in the complex jet which were studied by Chen et al (2017). We also investigate the physical properties of these jets and present possible mechanisms responsible for the evolution of the jet.…”

Section: Introductionmentioning

confidence: 99%

“…A series of jets appeared at the west edge of AR 11 513 on 2012 July 2 (Chen et al, 2015). One of these jets occurred at around 22: 30 UT, and the driving mechanism are studied by Chen et al (2017). The complex jet went through two phases originating from different magnetic patches.…”

Section: Introduction Of a Jetmentioning

confidence: 99%

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Blobs in a Solar EUV Jet

Chen

Erdélyi

et al. 2022

Front. Astron. Space Sci.

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An Extreme Ultraviolet (EUV) jet that occurred around 22:30 on July 2, 2012 was observed by the Atmospheric Imaging Assembly (AIA) on-board the Solar Dynamics Observatory (SDO). There were two phases of the jet. In Phase 1, two blobs were observed. In Phase 2, the intensity of the jet was almost coherent initially. One minute later, three blobs were formed at the same time in the jet, and the width of the jet changed after the formation of these blobs. The formation and evolution processes of the blobs in these two phases are analyzed in this paper. The physical parameters of the blobs are determined. The measured width of the blobs is 0.8 − 2.3 Mm, and the apparent velocities of the blobs are from 59 km s−1 to 185 km s−1. The formation mechanism of the blobs is likely to be tear-mode instability.

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“…Most theories and observations suggest that the rotational motion of solar coronal jets should be a process involving "untwisting"[e.g., Shibata and Uchida, 1986;Jibben and Canfield, 2004;Moreno-Insertis et al, 2008;Pariat et al, 2009;Liu et al, 2009;Shen et al, 2012;Lee et al, 2015;Fang et al, 2014;Filippov et al, 2015b;Liu et al, 2016b]. The physical scenario of "untwisting" jets is usually described as follows: a newly emerging [e.g., observations in Liu et al, 2016b;Zheng et al, 2018] or a pre-existing closed flux system [disturbed by footpoint motions, e.g., observations in Chen et al, 2017] reconnects with the ambient open magnetic field, during which twists contained in the closed flux system could be passed into the open fields and are then released during the rotational motion of the associated jet. Following this idea, a natural question may be raised: will all the twists stored in the pre-reconnection flux rope be released during the coronal jet eruption?…”

Section: Introductionmentioning

confidence: 99%

How Many Twists Do Solar Coronal Jets Release?

Liu

Wang

Erdélyi

2019

Front. Astron. Space Sci.

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Highly twisted magnetic flux ropes, with finite length, are subject to kink instabilities, and could lead to a number of eruptive phenomena in the solar atmosphere, including flares, coronal mass ejections (CMEs) and coronal jets. The kink instability threshold, which is the maximum twist a kink-stable magnetic flux rope could contain, has been widely studied in analytical models and numerical simulations, but still needs to be examined by observations. In this article, we will study twists released by 30 off-limb rotational solar coronal jets, and compare the observational findings with theoretical kink instability thresholds. We have found that: 1) the number of events with more twist release becomes less; 2) each of the studied jets has released a twist number of at least 1.3 turns (a twist angle of 2.6π); and 3) the size of a jet is highly related to its twist pitch instead of twist number. Our results suggest that the kink instability threshold in the solar atmosphere should not be a constant. The found lower limit of twist number of 1.3 turns should be merely a necessary but not a sufficient condition for a finite solar magnetic flux rope to become kink unstable.

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A Complex Solar Coronal Jet with Two Phases

Cited by 13 publications

References 41 publications

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Blobs in a Solar EUV Jet

How Many Twists Do Solar Coronal Jets Release?

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