Coronal Quasi-periodic Fast-mode Propagating Wave Trains

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

doi:10.1007/s11207-022-01953-2

Cited by 23 publications

(41 citation statements)

References 251 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In Figure 4(c), we can identify that the relative amplitude intensity is about 35%. These parameters are in agreement with those of broad QFP wave trains (Shen et al 2019(Shen et al , 2022 and typical single-pulsed EUV waves (Veronig et al 2010;Warmuth 2015). However, the intensity amplitude is significantly greater than that of the narrow QFP wave train (Shen et al 2022).…”

Section: Resultssupporting

confidence: 86%

“…The wave train propagated along the solar surface with an angular extent of about 270°and a relative maximum intensity amplitude of about 35% relative to the unperturbed background corona. These parameters are significantly larger than the QFP wave trains along open or closed coronal loops (i.e., narrow QFP wave trains), where the angular width and maximum intensity amplitude are in the range of 10°-60°and 1%-5%, respectively (Liu & Ofman 2014;Shen et al 2022). These differences suggest that the observed wave train belongs to the broad type of QFP wave train, as proposed in Shen et al (2022), which has a relatively larger intensity amplitude, higher energy flux, and larger angular extent than narrow QFP wave trains along coronal loops.…”

Section: Discussionmentioning

confidence: 94%

“…It should be pointed out that the main periods (errors) of the wave train and flare were determined by the peak (FWHM) of the corresponding global wavelet power spectra. The common 90 s periodicities of the wave train and the accompanying flare strongly suggest that the two different phenomena should originate from the same physical process, such as the nonlinear magnetic reconnection process in the flare (Shen et al 2022).…”

Section: Resultsmentioning

confidence: 99%

“…In Shen et al (2019), since the period of the wave train was similar to the unwinding filament threads in the eruption source region, the authors alternatively proposed that the wave train was excited by the sequentially outward expansion of the unwinding filament threads. 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).…”

Section: Introductionmentioning

confidence: 99%

“…In comparison, the physical parameters of broad QFP wave trains are more similar to the typical single-pulsed EUV waves. The generation mechanism of broad QFP waves is still an open question (Shen et al 2022), although several numerical simulations have been performed (Yang et al 2015;Takasao & Shibata 2016;Pascoe et al 2017;Wang et al 2021a).…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

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

Zhou¹,

Shen²,

Liu³

et al. 2022

ApJL

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Resultssupporting

confidence: 86%

Section: Discussionmentioning

confidence: 94%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

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

Zhou¹,

Shen²,

Liu³

et al. 2022

ApJL

Self Cite

View full text Add to dashboard Cite

show abstract

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

Zhou

Shen

et al. 2021

Sol Phys

View full text Add to dashboard Cite

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.

show abstract