Observation and modelling of solar jets

Shen, Yuandeng

doi:10.1098/rspa.2020.0217

Cited by 96 publications

(92 citation statements)

References 336 publications

(644 reference statements)

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“…Here, the narrow, quasi-periodic EUV wave train should be a so-called QFP magnetosonic wave like those reported in previous studies (e.g. Liu et al, 2011;Shen and Liu, 2012b;Shen et al, 2013a; Yuan et al, 2013;Miao et al, 2021). The propagation of such QFP waves is typically trapped in coronal loops acting as waveguides (high density, low Alfvén speed).…”

Section: Flare-ignited Quasi-periodic Euv Wave Trainssupporting

confidence: 60%

“…It is worth pointing out that CMEs are not a necessary requirement for producing large-scale EUV waves, although they have been generally accepted as the driver of EUV waves. Some recent observations have shown that large-scale EUV waves can also be driven by various non-CME-associated solar eruptions, such as coronal jets (Zheng et al, 2013;Shen et al, 2018a,c,d;Shen, 2021), mini-filament eruptions (Wang et al, 2020), expanding coronal loops (Su et al, 2015;Shen et al, 2017bShen et al, , 2018c, and newly formed sigmoidal loops (Zheng et al, 2012b). Recently, large-scale quasi-periodic EUV waves with periods of a few minutes have been detected, which can propagate simultaneously along and across magnetic-field lines and cause the oscillations of filaments and coronal loops (Liu et al, 2012;Shen et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

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CME-Driven and Flare-Ignited Fast Magnetosonic Waves Detected in a Solar Eruption

Zhou

Shen

et al. 2021

Sol Phys

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We present Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) observation of three types of fast-mode, propagating, magnetosonic waves in a GOES C3.0 flare on 23 April 2013, which was accompanied by a prominence eruption and a broad coronal mass ejection (CME). During the fast-rising phase of the prominence, a large-scale, dome-shaped, extreme-ultraviolet (EUV) wave firstly formed ahead of the CME bubble and propagated at a speed of about 430 km s −1 in the CME's lateral direction. One can identify the separation process of the EUV wave from the CME bubble. The reflection effect of the on-disk counterpart of this EUV wave was also observed when it interacted with a remote active region. Six minutes after the first appearance of the EUV wave, a large-scale, quasi-periodic EUV train with a period of about 120 seconds, which emanated from the flare epicenter and propagated outward at an average speed up to 1100 km s −1 , appeared inside the CME bubble. In addition, another narrow, quasi-periodic EUV wave train, which also emanated from the flare epicenter, propagated at a speed of about 475 km s −1 and with a period of about 110 seconds, was observed along a closed-loop system connecting two adjacent active regions. We propose that all of the observed waves are fast-mode magnetosonic waves, in which the large-scale, dome-shaped EUV wave ahead of the CME bubble was driven by the expansion of the CME bubble, while the large-scale, quasi-periodic EUV train within the CME bubble and the narrow quasi-periodic EUV wave train along the closedloop system were excited by the intermittent energy-releasing process in the flare. Coronal seismology application and energy carried by the waves are also estimated based on the measured wave parameters.

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Section: Flare-ignited Quasi-periodic Euv Wave Trainssupporting

confidence: 60%

Section: Introductionmentioning

confidence: 99%

CME-Driven and Flare-Ignited Fast Magnetosonic Waves Detected in a Solar Eruption

Zhou

Shen

et al. 2021

Sol Phys

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“…In 2010, the SDO was launched with two important instruments onboard: the Atmospheric Imaging Assembly (AIA: Lemen et al, 2012), providing extreme ultraviolet (EUV) and ultraviolet (UV) data, and the Helioseismic and Magnetic Imager (HMI: Scherrer et al, 2012), providing magnetograms both with a high spatial resolution (0.6 and 0.5 arc sec) and high temporal cadence (12 and 45 s). A very impressive number of publications concerning jets observed with AIA with more precise results of their characteristics and their triggers appeared (Raouafi et al, 2016;Shen, 2021). In the review of Hinode Review Team (2019), there is not only an interesting discussion of the jets observed with the Hinode instruments but also a deep discussion on the origin of the jets observed with the SDO/AIA.…”

Section: Sdo and The Onset Of Jetsmentioning

confidence: 99%

Solar Jets: SDO and IRIS Observations in the Perspective of New MHD Simulations

Schmieder

2022

Front. Astron. Space Sci.

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Solar jets are observed as collimated plasma beams over a large range of temperatures and wavelengths. They have been observed in H α and optical lines for more than 50 years and called surges. The term “jet” comes from X-ray observations after the launch of the Yohkoh satellite in 1991. They are the means of transporting energy through the heliosphere and participate to the corona heating and the acceleration of solar wind. Several characteristics have been derived about their velocities, their rates of occurrence, and their relationship with CMEs. However, the initiation mechanism of jets, e.g. emerging flux, flux cancellation, or twist, is still debated. In the last decade coordinated observations of the Interface Region Imaging Spectrograph (IRIS) with the instruments on board the Solar Dynamic Observatory (SDO) allow to make a step forward for understanding the trigger of jets and the relationship between hot jets and cool surges. We observe at the same time the development of 2D and 3D MHD numerical simulations to interpret the results. This paper summarizes recent studies of jets showing the loci of magnetic reconnection in null points or in bald patch regions forming a current sheet. In the pre-jet phase a twist is frequently detected by the existence of a mini filament close to the dome of emerging flux. The twist can also be transferred to the jet from a flux rope in the vicinity of the reconnection by slippage of the polarities. Bidirectional flows are detected at the reconnection sites. We show the role of magnetic currents detected in the footprints of flux rope and quasi-separatrix layers for initiating the jets. We select a few studies and show that with the same observations, different interpretations are possible based on different approaches e.g. non linear force free field extrapolation or 3D MHD simulation.

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“…Jets may also be formed by shock waves (e.g., De Pontieu et al, 2004). Detailed descriptions of coronal jets can be found in recent reviews (Innes et al, 2016;Raouafi et al, 2016;Shen, 2021).…”

Section: Introductionmentioning

confidence: 99%

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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Observation and modelling of solar jets

Cited by 96 publications

References 336 publications

CME-Driven and Flare-Ignited Fast Magnetosonic Waves Detected in a Solar Eruption

CME-Driven and Flare-Ignited Fast Magnetosonic Waves Detected in a Solar Eruption

Solar Jets: SDO and IRIS Observations in the Perspective of New MHD Simulations

Blobs in a Solar EUV Jet

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