Birthplaces of Extreme Ultraviolet Waves Driven by Impingement of Solar Jets upon Coronal Loops

Zhang, Liang; Zheng, Ruisheng; Chen, Huadong; Chen, Yao

doi:10.3847/1538-4357/ac61db

Cited by 4 publications

(2 citation statements)

References 29 publications

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“…Small-scale eruptions can drive EUV waves (e.g., Zheng et al 2012Zheng et al , 2013Shen et al 2018;Zhang et al 2022a). In this study, we observed an EUV wave associated with a blowout jet.…”

Section: Discussionmentioning

confidence: 55%

A Type II Radio Burst Driven by a Blowout Jet on the Sun

Hou

Madjarska

et al. 2023

ApJ

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Type II radio bursts are often associated with coronal shocks that are typically driven by coronal mass ejections (CMEs) from the Sun. Here we conduct a case study of a type II radio burst that is associated with a C4.5-class flare and a blowout jet, but without the presence of a CME. The blowout jet is observed near the solar disk center in the extreme-ultraviolet (EUV) passbands with different characteristic temperatures. Its evolution involves an initial phase and an ejection phase with a velocity of 560 ± 87 km s−1. Ahead of the jet front, an EUV wave propagates at a projected velocity of ∼403 ± 84 km s−1 in the initial stage. The velocity of the type II radio burst is estimated to be ∼641 km s−1, which corresponds to the shock velocity against the coronal density gradient. The EUV wave and the type II radio burst are closely related to the ejection of the blowout jet, suggesting that both are likely the manifestation of a coronal shock driven by the ejection of the blowout jet. The type II radio burst likely starts lower than those associated with CMEs. The combination of the velocities of the radio burst and the EUV wave yields a modified shock velocity at ∼757 km s−1. The Alfvén Mach number is in the range of 1.09–1.18, implying that the shock velocity is 10%–20% larger than the local Alfvén velocity.

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Section: Discussionmentioning

confidence: 55%

A Type II Radio Burst Driven by a Blowout Jet on the Sun

Hou

Madjarska

et al. 2023

ApJ

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“…Magnetohydrodynamic (MHD) wave theory in structured plasmas was formulated in the 1970s and 1980s (e.g., Zajtsev & Stepanov 1975;Roberts 1981). Over the past decades, modern observation instruments have captured various MHD wave modes (see review by Nakariakov & Verwichte 2005;Nakariakov & Kolotkov 2020;Van Doorsselaere et al 2020), such as standing fast kink waves (e.g., Aschwanden et al 1999;Nakariakov et al 1999;Nakariakov & Ofman 2002;Ofman & Wang 2008), global extreme-ultraviolet (EUV) waves (e.g., Chen et al 2002Chen et al , 2005Chen 2011;Cheng et al 2012a;Shen & Liu 2012a;Li et al 2012;Guo et al 2015;Liu et al 2019;Hu et al 2019;Zheng et al 2020;Zhou et al 2020;Shen et al 2020;Zheng et al 2022;Zhang et al 2022;Chen 2022), and trapped fast sausage waves (e.g., Nakariakov et al 2003;Inglis et al 2009;Li et al 2020), providing detailed study conditions. In addition to playing an important role in coronal heating, the measured parameters of the MHD waves provide a condition for diagnosing coronal physical parameters that are hard to measure directly, such as the magnetic field strength (Nakariakov & Ofman 2001;Shen et al 2014;Long et al 2019;Nakariakov & Kolotkov 2020;Yang et al 2020;Miao et al 2021;Long et al 2021) through seismological diagnostics first proposed by Uchida (1970) and…”

Section: Introductionmentioning

confidence: 99%

Recurrent Narrow Quasiperiodic Fast-propagating Wave Trains Excited by the Intermittent Energy Release in the Accompanying Solar Flare

Zhou

Shen

et al. 2022

ApJ

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About the driven mechanisms of the quasiperiodic fast-propagating (QFP) wave trains, there exist two dominant competing physical explanations: they are associated with the flaring energy release or attributed to the waveguide dispersion. Employing Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å images, we investigated a series of QFP wave trains composed of multiple wave fronts propagating along a loop system during the accompanying flare on 2011 November 11. The wave trains showed a high correlation in start times with the energy release of the accompanying flare. Measurements show that the wave trains’ phase speed is almost consistent with its group speed with a value of about 1000 km s−1, indicating that the wave trains should not be considered dispersed waves. The period of the wave trains was the same as that of the oscillatory signal in X-ray emissions released by the flare. Thus we propose that the QFP wave trains were most likely triggered by the flare rather than by dispersion. We investigated the seismological application with the QFP waves and then obtained that the magnetic field strength of the waveguide was about 10 G. Meanwhile, we also estimated that the energy flux of the wave trains was about 1.2 × 105 erg cm−2 s−1.

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An extreme-ultraviolet wave associated with the possible expansion of sheared arcades

Yu¹,

Zheng²,

Zhang³

et al. 2023

A&A

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Context. Solar extreme-ultraviolet (EUV) waves are propagating disturbances in the corona, and they are usually accompanied with various solar eruptions, from large-scale coronal mass ejections to small-scale coronal jets. Aims. Generally, it is believed that EUV waves are driven by the rapid expansion of coronal loops overlying the erupting cores. In this paper, we present an exception of an EUV wave that was not triggered by the expansion of coronal loops overlying the erupting core. Methods. Combining the multiwavelength observations from multiple instruments, we studied the event in detail. Results. The eruption was restricted in the active region (AR) and disturbed the nearby sheared arcades (SAs) connecting the source AR to a remote AR. Interestingly, following the disturbance, an EUV wave formed close to the SAs, but far away from the eruption source. Conclusions. All the results show that the EUV wave had a closer temporal and spatial relationship with the disappearing part of SAs than the confined eruption. Hence, we suggest that the EUV wave was likely triggered by the expansion of some strands of SAs, rather than the expansion of erupting loops. It can be a possible complement for the driving mechanisms of EUV waves.

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Birthplaces of Extreme Ultraviolet Waves Driven by Impingement of Solar Jets upon Coronal Loops

Cited by 4 publications

References 29 publications

A Type II Radio Burst Driven by a Blowout Jet on the Sun

A Type II Radio Burst Driven by a Blowout Jet on the Sun

Recurrent Narrow Quasiperiodic Fast-propagating Wave Trains Excited by the Intermittent Energy Release in the Accompanying Solar Flare

An extreme-ultraviolet wave associated with the possible expansion of sheared arcades

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