The eruption of a small filament in the quiet Sun

Ren, D. B.; Jiang, Yong; Yang, Jiayan; Zheng, Ruisheng; Bi, Yi; Wang, M.

doi:10.1007/s10509-008-9908-2

Cited by 22 publications

(13 citation statements)

References 32 publications

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“…This is consistent with the idea of other workers, e.g. Hermans & Martin (1986), Jiang & Wang (2001), Sakajiri et al (2004), and Ren et al (2008), that flux convergence and cancellation plays an important role in small-scale filament eruptions. In those listed studies, the small-scale filaments are smaller than typical solar filaments but larger than our minifilaments.…”

Section: Evolution Of Minifilaments and Jetssupporting

confidence: 93%

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

Panesar¹,

Sterling²,

Moore³

et al. 2016

ApJL

134

249

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We report observations of ten random on-disk solar quiet region coronal jets found in high resolution Extreme Ultraviolet (EUV) images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and having good coverage in magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). Recent studies show that coronal jets are driven by the eruption of a small-scale filament (called a minifilament). However the trigger of these eruptions is still unknown. In the present study we address the question: what leads to the jet-driving minifilament eruptions? The EUV observations show that there is a cool-transitionregion-plasma minifilament present prior to each jet event and the minifilament eruption drives the jet. By examining pre-jet evolutionary changes in the line-of-sight photospheric magnetic field we observe that each pre-jet minifilament resides over the neutral line between majority-polarity and minority-polarity patches of magnetic flux. In each of the ten cases, the opposite-polarity patches approach and merge with each other (flux reduction between 21 and 57%). After several hours, continuous flux cancellation at the neutral line apparently destabilizes the field holding the cool-plasma minifilament to erupt and undergo internal reconnection, and external reconnection with the surrounding-coronal field. The external reconnection opens the minifilament field allowing the minifilament material to escape outwards, forming part of the jet spire. Thus we found that each of the ten jets resulted from eruption of a minifilament following flux cancellation at the neutral line under the minifilament. These observations establish that magnetic flux cancellation is usually the trigger of quiet region coronal jet eruptions.

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Section: Evolution Of Minifilaments and Jetssupporting

confidence: 93%

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

Panesar¹,

Sterling²,

Moore³

et al. 2016

ApJL

134

249

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“…They show deep dimmings and flare-like brightenings at the onset site and, in about one third of the events, more extended fainter dimming waves propagating out to several tens of Mm (Ren et al 2008;Innes et al 2009;Podladchikova et al 2010). Furthermore their frequency extends the power-law distribution of large CMEs down to the 20 Mm scale (Schrijver 2010).…”

Section: Introductionmentioning

confidence: 93%

STEREO quadrature observations of coronal dimming at the onset of mini-CMEs

Innes

McIntosh

Pietarila

2010

A&A

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Context. Using unique quadrature observations with the two STEREO spacecraft, we investigate coronal dimmings at the onset of small-scale eruptions. In CMEs they are believed to indicate the opening up of the coronal magnetic fields at the start of the eruption. Aims. It is to determine whether coronal dimming seen in small-scale eruptions starts before or after chromospheric plasma ejection.Methods. One STEREO spacecraft obtained high cadence, 75 s, images in the He ii 304 Å channel, and the other simultaneous images in the Fe ix/Fe x 171 Å channel. We concentrate on two well-positioned chromospheric eruptions that occurred at disk center in the 171 Å images, and on the limb in 304 Å. One was in the quiet Sun and the other was in an equatorial coronal hole. We compare the timing of chromospheric eruption seen in the 304 Å limb images with the brightenings and dimmings seen on disk in the 171 Å images. Further we use off-limb images of the low frequency 171 Å power to infer the coronal structure near the eruptions. Results. In both the quiet Sun and the coronal hole eruption, on disk 171 Å dimming was seen before the chromospheric eruption, and in both cases it extends beyond the site of the chromospheric eruption. The quiet Sun eruption occurred on the outer edge of the enclosing magnetic field of a prominence and may be related to a small disruption of the prominence just before the 171 Å dimming. Conclusions. These small-scale chromospheric eruptions started with a dimming in coronal emission just like their larger counterparts. We therefore suggest that a fundamental step in triggering them was the removal of overlying coronal field.

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“…Eruptive small-scale features, such as minifilaments, are frequently observed on the solar surface (Moore et al 1977;Hermans & Martin 1986;Chae et al 1999;Wang et al 2000;Sakajiri et al 2004;Zuccarello et al 2007;Ren et al 2008). They are located above a magnetic neutral line (also known as polarity inversion line, PIL) between adjacent oppositepolarity magnetic flux clumps in the photosphere (Martin 1986(Martin , 1998.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Flux Cancellation as the Origin of Solar Quiet-region Pre-jet Minifilaments

Panesar

Sterling

Moore

2017

ApJ

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We investigate the origin of ten solar quiet region pre-jet minifilaments, using EUV images from SDO/AIA and magnetograms from SDO/HMI. We recently found (Panesar et al. 2016b) that quiet region coronal jets are driven by minifilament eruptions, where those eruptions result from flux cancelation at the magnetic neutral line under the minifilament. Here, we study the longer-term origin of the pre-jet minifilaments themselves. We find that they result from flux cancelation between minority-polarity and majority-polarity flux patches. In each of ten pre-jet regions, we find that opposite-polarity patches of magnetic flux converge and cancel, with a flux reduction of 10-40% from before to after the minifilament appears. For our ten events, the minifilaments exist for periods ranging from 1.5 hr to two days before erupting to make a jet. Apparently, the flux cancelation builds highly sheared field that runs above and traces the neutral line, and the cool-transition-region-plasma minifilament forms in this field and is suspended in it. We infer that the convergence of the opposite-polarity patches results in reconnection in the low corona that builds a magnetic arcade enveloping the minifilament in its core, and that the continuing flux cancelation at the neutral line finally destabilizes the minifilament field so that it erupts and drives the production of a coronal jet. Thus our observations strongly support that quiet region magnetic flux cancelation results in both the formation of the pre-jet minifilament and its jet-driving eruption.

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The eruption of a small filament in the quiet Sun

Cited by 22 publications

References 32 publications

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

Magnetic Flux Cancelation as the Trigger of Solar Quiet-Region Coronal Jets

STEREO quadrature observations of coronal dimming at the onset of mini-CMEs

Magnetic Flux Cancellation as the Origin of Solar Quiet-region Pre-jet Minifilaments

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