Observation of a Reversal of Breakout Reconnection Preceding a Jet: Evidence of Oscillatory Magnetic Reconnection?

Hong, Jiang; Yang, Jiayan; Chen, Huadong; Bi, Yong; Yang, Bo; Chen, Hechao

doi:10.3847/1538-4357/ab0c9d

Cited by 32 publications

(22 citation statements)

References 86 publications

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“…Subarcsecond plasmoids were detected by the IRIS, whose average size is about 0.57 Mm, and their ejecting speed ranges from 10 to 220 km s −1 [135]. Besides the observation of plasmoids in straight anemone jets [81,[136][137][138][139], they were also observed in two-sided-loop jets [44] (figure 4). Analysis results indicated that plasmoids observed in different types of jets were similar, and they were thought to be created by magnetic reconnection as a result of the tearing instability of the current sheets.…”

Section: (Ii) Plasmoidmentioning

confidence: 97%

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: (Ii) Plasmoidmentioning

confidence: 97%

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

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“…Such cancelation and the resulting formation and eruption of small-scale ("mini") filaments has been proposed as driving mechanism for many coronal jets that feed into the solar wind (Sterling et al, 2015). Recent IRIS/SJI and SDO observations have been used to provide support for this mechanism (Hong et al, 2019) through imaging of the evolution of the predicted break-out current sheet that precedes the eruption of a mini-filament and jet.…”

Section: Mass Supply To the Solar Windmentioning

confidence: 99%

A New View of the Solar Interface Region from the Interface Region Imaging Spectrograph (IRIS)

et al. 2021

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The Interface Region Imaging Spectrograph (IRIS) has been obtaining near- and far-ultraviolet images and spectra of the solar atmosphere since July 2013. IRIS is the highest resolution observatory to provide seamless coverage of spectra and images from the photosphere into the low corona. The unique combination of near- and far-ultraviolet spectra and images at sub-arcsecond resolution and high cadence allows the tracing of mass and energy through the critical interface between the surface and the corona or solar wind. IRIS has enabled research into the fundamental physical processes thought to play a role in the low solar atmosphere such as ion–neutral interactions, magnetic reconnection, the generation, propagation, and dissipation of waves, the acceleration of non-thermal particles, and various small-scale instabilities. IRIS has provided insights into a wide range of phenomena including the discovery of non-thermal particles in coronal nano-flares, the formation and impact of spicules and other jets, resonant absorption and dissipation of Alfvénic waves, energy release and jet-like dynamics associated with braiding of magnetic-field lines, the role of turbulence and the tearing-mode instability in reconnection, the contribution of waves, turbulence, and non-thermal particles in the energy deposition during flares and smaller-scale events such as UV bursts, and the role of flux ropes and various other mechanisms in triggering and driving CMEs. IRIS observations have also been used to elucidate the physical mechanisms driving the solar irradiance that impacts Earth’s upper atmosphere, and the connections between solar and stellar physics. Advances in numerical modeling, inversion codes, and machine-learning techniques have played a key role. With the advent of exciting new instrumentation both on the ground, e.g. the Daniel K. Inouye Solar Telescope (DKIST) and the Atacama Large Millimeter/submillimeter Array (ALMA), and space-based, e.g. the Parker Solar Probe and the Solar Orbiter, we aim to review new insights based on IRIS observations or related modeling, and highlight some of the outstanding challenges.

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“…Generally, the fan-spine magnetic system represents the 3D magnetic topology of straight anemone type solar jets Shen (2021), and many observational and numerical simulation works are all taken such a special magnetic system as the basic coronal magnetic environment of solar jets (e.g., Pariat et al 2009;Sterling et al 2015;Wyper et al 2018;Shen et al 2019a;Hong et al 2019). Many recent high spatiotemporal resolution observations showed that solar jets are driven by mini-filament eruptions in fan-spine systems and in association with photospheric magnetic flux cancellations, and these features are also frequently observed in largescale energetic solar eruptions (e.g., Shen et al 2012aShen et al , 2017Sterling et al 2015;Hong et al 2016Hong et al , 2017Wyper et al 2017;Panesar et al 2017Panesar et al , 2018Sterling et al 2018;Samanta et al 2019).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Sympathetic Filament Eruptions within a Fan-spine Magnetic System

Zhou,

Shen,

Zhou

et al. 2021

Preprint

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It is unclear whether successive filament eruptions at different sites within a short time interval are physically connected or not. Here, we present the observations of the successive eruptions of a small and a large filament in a tripolar magnetic field region whose coronal magnetic field showed as a fanspine magnetic system. By analyzing the multi-wavelength observations taken by the Solar Dynamic Observatory (SDO) and the extrapolated three-dimensional coronal magnetic field, we find that the two filaments resided respectively in the two lobes that make up the inner fan structure of the fan-spine magnetic system. In addition, a small fan-spine system was also revealed by the squashing factor Q map, which located in the east lobe of the fan structure of the large fan-spine system. The eruption of the small filament was a failed filament eruption, which did not cause any coronal mass ejection (CME) except for three flare ribbons and two post-flare-loop systems connecting the three magnetic polarities. The eruption of the large filament not only caused similar post-flare-loop systems and flare ribbons as observed in the small filament eruption, but also a large-scale CME. Based on our analysis results, we conclude that the two successive filament eruptions were physically connected, in which the topology change caused by the small filament eruption is thought to be the physical linkage. In addition, the eruption of the small fan-spine structure further accelerated the instability and violent eruption of the large filament.

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Observation of a Reversal of Breakout Reconnection Preceding a Jet: Evidence of Oscillatory Magnetic Reconnection?

Cited by 32 publications

References 86 publications

Observation and modelling of solar jets

Observation and modelling of solar jets

A New View of the Solar Interface Region from the Interface Region Imaging Spectrograph (IRIS)

Sympathetic Filament Eruptions within a Fan-spine Magnetic System

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