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

Zhou, Xinping; Shen, Yuandeng; Su, Jiangtao; Tang, Zehao; Zhou, Chen; Duan, Yadan; Tan, Song

doi:10.1007/s11207-021-01913-2

Cited by 23 publications

(19 citation statements)

References 120 publications

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“…As for quasiperiodic fast-propagating (QFP) wave trains, Shen et al (2022) divided them into narrow and broad QFP types based on their different physical properties. The former is characterized as propagating coherent wave fronts along the coronal loops with a relatively narrow angular width and a small intensity amplitude (Liu et al 2011;Shen & Liu 2012c;Miao et al 2019;Zhou et al 2021;Duan et al 2022), while the latter propagates along the solar surface with a broad angular width and a relatively large intensity amplitude (Shen et al 2019). In comparison, the physical parameters of broad QFP wave trains are more similar to the typical single-pulsed EUV waves.…”

Section: Introductionmentioning

confidence: 99%

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Zhou¹,

Shen²,

Liu³

et al. 2022

ApJL

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Large-scale extreme-ultraviolet (EUV) waves are frequently observed as an accompanying phenomenon of flares and coronal mass ejections (CMEs). Previous studies mainly focused on EUV waves with single wave fronts that are generally thought to be driven by the lateral expansion of CMEs. Using high spatiotemporal resolution multi-angle imaging observations taken by the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory, we present the observation of a broad quasiperiodic fast-propagating (QFP) wave train composed of multiple wave fronts along the solar surface during the rising phase of a GOES M3.5 flare on 2011 February 24. The wave train transmitted through a lunate coronal hole (CH) with a speed of ∼840 ± 67 km s−1, and the wave fronts showed an intriguing refraction effect when they passed through the boundaries of the CH. Due to the lunate shape of the CH, the transmitted wave fronts from the north and south arms of the CH started to approach each other and finally collided, leading to a significant intensity enhancement at the collision site. This enhancement might hint at the occurrence of interference between the two transmitted wave trains. The estimated magnetosonic Mach number of the wave train is about 1.13, which indicates that the observed wave train was a weak shock. Period analysis reveals that the period of the wave train was ∼90 s, in good agreement with that of the accompanying flare. Based on our analysis results, we conclude that the broad QFP wave train was a large-amplitude fast-mode magnetosonic wave or a weak shock driven by some nonlinear energy release processes in the accompanying flare.

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Section: Introductionmentioning

confidence: 99%

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Zhou¹,

Shen²,

Liu³

et al. 2022

ApJL

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“…For the EUV waves, dome-like wavefronts have been reported by some authors (Veronig et al 2010;Li et al 2012;Liu et al 2012;Selwa et al 2012;Shen et al 2014a;Zhou et al 2021a). Veronig et al (2010), Li et al (2012), andShen et al (2014a) found that the upward expansions of their studied wavefronts were faster than the lateral expansions of the wavefronts.…”

Section: Discussionmentioning

confidence: 78%

“…Limb observations have shown that an EUV wave does have a dome-shaped wavefront (Veronig et al 2010;Li et al 2012;Liu et al 2012;Selwa et al 2012;Shen et al 2014a;Zhou et al 2021a). In the studies of Veronig et al (2010), Li et al (2012), andShen et al (2014a), the upward expansions of wavefronts were found to be faster than the lateral expansions.…”

Section: Introductionmentioning

confidence: 99%

Three-dimensional Propagation of the Global EUV Wave associated with a solar eruption on 2021 October 28

Hou,

Tian,

Wang

et al. 2022

Preprint

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We present a case study for the global extreme ultraviolet (EUV) wave and its chromospheric counterpart 'Moreton-Ramsey wave' associated with the second X-class flare in Solar Cycle 25 and a halo coronal mass ejection (CME). The EUV wave was observed in the Hα and EUV passbands with different characteristic temperatures. In the 171 Å and 193/195 Å images, the wave propagates circularly with an initial velocity of 600-720 km s −1 and a deceleration of 110-320 m s −2 . The local coronal plasma is heated from log(T/K)≈5.9 to log(T/K)≈6.2 during the passage of the wavefront. The Hα and 304 Å images also reveal signatures of wave propagation with a velocity of 310-540 km s −1 . With multi-wavelength and dual-perspective observations, we found that the wavefront likely propagates forwardly inclined to the solar surface with a tilt angle of ∼53.2 • . Our results suggest that this EUV wave is a fast-mode magnetohydrodynamic wave or shock driven by the expansion of the associated CME, whose wavefront is likely a dome-shaped structure that could impact the upper chromosphere, transition region and corona.

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“…They can provide potential diagnostics on coronal magnetic field strengths and coronal plasma parameters for global coronal seismology (Kwon et al 2013;Long et al 2013Long et al , 2017. It is generally believed that EUV waves are best interpreted as the bimodal composition of an outer fast-mode MHD wave and an inner nonwave component of coronal mass ejections (CMEs) (Chen & Wu 2011;Zheng et al 2013Zheng et al , 2014Liu & Ofman 2014;Mei et al 2020;Zhou et al 2020Zhou et al , 2021Chandra et al 2021). More details about EUV waves can be found in recent reviews (Liu & Ofman 2014;Warmuth 2015;Chen 2016;Long et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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

Zhang

Zheng

Chen

et al. 2022

ApJ

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Solar extreme ultraviolet (EUV) waves are large-scale propagating disturbances in the corona. It is generally believed that a vital key to the formation of EUV waves is the rapid expansion of the loops that overlie erupting cores in solar eruptions, such as coronal mass ejections (CMEs) and solar jets. However, the details of the interaction between the erupting cores and overlying loops are not clear because the overlying loops always instantly open after energetic eruptions. Here, we present three typical jet-driven EUV waves without CMEs to study the interaction between the jets and the overlying loops that remained closed during the events. All three jets emanated from magnetic flux cancellation sites in the source regions. Interestingly, after the interactions between the jets and overlying loops, three EUV waves respectively formed ahead of the top, the near end (close to the jet source), and the far (another) end of the overlying loops. According to the magnetic field distribution of the loops extrapolated through the potential field source surface method, it is confirmed that the birthplaces of three jet-driven EUV waves were around the parts of the overlying loops with the weakest magnetic field strengths. We suggest that the jet-driven EUV waves preferentially occur at the weakest part of the overlying loops, and the location can be subject to the magnetic field intensity around the ends of the loops.

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

Cited by 23 publications

References 120 publications

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Three-dimensional Propagation of the Global EUV Wave associated with a solar eruption on 2021 October 28

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

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