Research progress on coronal extreme ultraviolet waves

Shen, Yuandeng; Li, Bo; Chen, Pengfei; Zhou, Xinping; Liu, Yu

doi:10.1360/tb-2020-0748

Cited by 12 publications

(13 citation statements)

References 104 publications

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“…Here, both the on-disk and radial-propagating EUV waves should be driven by the CME, as has been reported in previous studies (e.g. Veronig et al, 2010;Shen and Liu, 2012c;Shen et al, 2020). To analyze the kinematics of the EUV wave ahead of the CME bubble, we selected three azimuthal paths, labeled C1 -C3 in Figure 2, to generate TDSPs from the AIA 193 Å base-difference images.…”

Section: Prominence Eruption Cme and The Cme-driven Euv Wavementioning

confidence: 85%

“…In the case of a pistondriven shock, the wavefront should be initially located ahead of the driver and then decouples from the driver and propagates freely in the supporting medium. In most studied cases, CMEs are proposed as the typical driver of large-scale single-pulse EUV waves (Liu and Ofman, 2014;Warmuth, 2015;Shen et al, 2020Shen et al, , 2021, such as the one ahead of the CME bubble in the present event. For the large-scale, quasi-periodic EUV wave train, not only appeared inside the CME bubble but also delayed the rapid expansion of the CME bubble by about four minutes.…”

Section: Conclusion and Discussionmentioning

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: Prominence Eruption Cme and The Cme-driven Euv Wavementioning

confidence: 85%

Section: Conclusion and Discussionmentioning

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 addition, QFP wave trains can also excite oscillations of filaments and coronal loops during their propagation. The evidence of reflection, refraction and transmission effects of single pulsed global EUV waves have been reported in many studies; interested readers can refer to several recent reviews (Liu and Ofman, 2014;Warmuth, 2015;Long et al, 2017b;Shen et al, 2020).…”

Section: Interaction With Coronal Structurementioning

confidence: 98%

“…During the past two decades, observational and theoretical studies were intensively performed to study the driving mechanism and physical nature of these large-scale coronal disturbances. Thanks to the high spatiotemporal resolution observations taken by the Atmospheric Imaging Assembly (AIA: Lemen et al, 2012) onboard the Solar Dynamic Observatory (SDO), now we have recognized that a large-scale propagating coronal disturbance is typically composed of a fast-mode magnetosonic wave or shock followed by a slower wavelike feature, in which the former is often driven by a CME, corresponding to the coronal counterpart of a chromospheric Moreton wave (e.g., Shen and Liu, 2012c;Ma et al, 2011;Cheng et al, 2012), while the origin and physical nature of the latter is still unclear (Liu and Ofman, 2014;Warmuth, 2015;Chen, 2016;Shen et al, 2020). It should be pointed out that a bewildering multitude of names were used in history for large-scale fast-propagating coronal disturbances, such as "EIT waves", "(large-scale) coronal waves", "(largescale) coronal propagating fronts", and "EUV waves".…”

Section: Introductionmentioning

confidence: 99%

“…The present review mainly focuses on new observational and theoretical advances in recent years, but also includes previous theoretical and observational studies for without sacrificing completeness. Other types of coronal MHD waves are not covered in this review, interested readers can refer to many excellent review papers published in recent years (e.g., Nakariakov and Verwichte, 2005;Nakariakov and Kolotkov, 2020;Nakariakov et al, 2021;Warmuth, 2015;McLaughlin et al, 2018;Li et al, 2020a;Van Doorsselaere et al, 2020;Shen et al, 2020;Zimovets et al, 2021).…”

Section: Introductionmentioning

confidence: 99%

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Coronal Quasi-periodic Fast-mode Propagating Wave Trains

Shen,

Zhou,

Duan

et al. 2021

Preprint

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Quasi-periodic fast-mode propagating (QFP) wave trains in the corona have been studied intensively in the past decade, thanks to the full-disk, high spatiotemporal resolution, and widetemperature coverage observations taken by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). In AIA observations, QFP wave trains are seen to consist of multiple coherent and concentric wavefronts emanating successively near the epicenter of the accompanying flares; they propagate outwardly either along or across coronal loops at fast-mode magnetosonic speeds from several hundred to more than 2000 km s −1 , and their periods are in the range of tens of seconds to several minutes. Based on the distinct different properties of QFP wave trains, they might be divided into two distinct categories including narrow and broad ones. For most QFP wave trains, some of their periods are similar to those of quasi-periodic pulsations (QPPs) in the accompanying flares, indicating that they are probably different manifestations of the same physical process. Currently, candidate generation mechanisms for QFP wave trains include two main categories: pulsed energy excitation mechanism in association with magnetic reconnection and dispersion evolution mechanism related to the dispersive evolution of impulsively generated broadband perturbations. In addition, the generation of some QFP wave trains might be driven by the leakage of three and five minute oscillations from the lower atmosphere. As one of the new discoveries of SDO, QFP wave trains provide a new tool for coronal seismology to probe the corona parameters, and they are also useful for diagnosing the generation of QPPs, flare processes including energy release and particle accelerations. This review aims to summarize the main observational and theoretical results of the spatially-resolved QFP wave trains in extreme ultraviolet observations, and states briefly a number of questions that deserve further investigations.

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