Geometry, Kinematics, and Heliospheric Impact of a Large CME-driven Shock in 2017 September

Liu, Ying D.; Zhu, Bei; Zhao, Xiaowei

doi:10.3847/1538-4357/aaf425

Cited by 38 publications

(41 citation statements)

References 48 publications

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“…In this paper we fit only the CME-driven shock using the 3D ellipsoid model. Investigation of the CME geometry can be seen in, e.g., Gopalswamy et al (2018), Veronig et al (2018), and Liu et al (2019). Figure 2(e-f) present the modeled shock structure at ∼16:11 UT, and show that the shock has almost propagated backward to the opposite side of the eruption.…”

Section: Global Properties and Associated Shockmentioning

confidence: 96%

“…A three-dimensional (3D) modeled structure of the shock based on imaging observations from STEREO-A, SOHO, and GOES-16 is illustrated in Figure 2 (also see Liu et al 2019). The 3D model is developed by Kwon et al (2014) using an ellipsoid structure to represent a CME-driven shock, which can determine the 3D outermost structure of the shock by fitting multiple-viewpoint imaging observations (e.g., Kwon & Vourlidas 2017;Zhu et al 2018;Liu et al 2019). The ellipsoid model has seven free parameters: the height, longitude, and latitude of the center of the ellipsoid; the lengths of the three semiprincipal axes; and the rotation angle of the ellipsoid.…”

Section: Global Properties and Associated Shockmentioning

confidence: 99%

“…Veronig et al (2018) suggest that the EUV wave observed by SUVI is connected with the shock detected by C2 and detaches from the CME structure in the initial stage. The shock is caused by the impulsive expansion of the CME structure (Veronig et al 2018;Liu et al 2019). Therefore, it is still appropriate to call the shock a "CME-driven" shock despite the early detachment of the shock from the CME structure.…”

Section: Global Properties and Associated Shockmentioning

confidence: 99%

“…The global EUV wave was accompanied by an X8.2 flare and a violent CME driving a shock on the west limb of the Sun on 2017 September 10, which was observed by spacecraft on the opposite sides of the Sun. The related coronal and interplanetary properties have been studied in several works (e.g., Seaton & Darnel 2018;Li et al 2018;Yan et al 2018;Goryaev et al 2018;Luhmann et al 2018;Liu et al 2018;Cheng et al 2018;Liu et al 2019). In this paper we analyze the observations of Solar Terrestrial Relations Observatory A (STEREO-A), Solar Dynamics Observatory (SDO), Geostationary Operational Environmental Satellite 16 (GOES-16 ), and Solar and Heliospheric Observatory (SOHO) from nearly opposite sides of the Sun.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

Liu

Zhu

et al. 2019

ApJ

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We investigate a global extreme-ultraviolet (EUV) wave associated with a coronal mass ejection (CME)-driven shock on 2017 September 10. The EUV wave is transmitted by north-and south-polar coronal holes (CHs), which is observed by the Solar Dynamics Observatory (SDO) and Solar Terrestrial Relations Observatory A (STEREO-A) from opposite sides of the Sun. We obtain key findings on how the EUV wave interacts with multiple coronal structures, and on its connection with the CME-driven shock:(1) the transmitted EUV wave is still connected with the shock that is incurvated to the Sun, after the shock has reached the opposite side of the eruption; (2) the south CH transmitted EUV wave is accelerated inside an on-disk, low-density region with closed magnetic fields, which implies that an EUV wave can be accelerated in both open and closed magnetic field regions; (3) part of the primary EUV wavefront turns around a bright point (BP) with a bipolar magnetic structure when it approaches a dim, low-density filament channel near the BP; (4) the primary EUV wave is diffused and apparently halted near the boundaries of remote active regions (ARs) that are far from the eruption, and no obvious AR related secondary waves are detected; (5) the EUV wave extends to an unprecedented scale of ∼360 • in latitudes, which is attributed to the polar CH transmission. These results provide insights into the effects of coronal density and magnetic field distributions on the evolution of an EUV wave, and into the connection between the EUV wave and the associated CME-driven shock.

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Section: Global Properties and Associated Shockmentioning

confidence: 96%

Section: Global Properties and Associated Shockmentioning

confidence: 99%

Section: Global Properties and Associated Shockmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

Liu

Zhu

et al. 2019

ApJ

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“…Zhang et al 2019). Eruptions are frequently impulsively accelerated in the low corona within 10−15 min (the initial phase can take significantly longer; see Liu et al 2010Liu et al , 2019Manchester et al 2017). CMEs reach speeds of up to 3000 km s −1 and carry a total energy of around ∼10 25 J (=10 32 erg).…”

Section: How Do Cmes Evolve Through the Corona And Innermentioning

confidence: 99%

The Solar Orbiter mission

Müller

Cyr

Zouganelis

et al. 2020

A&A

677

281

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Aims. Solar Orbiter, the first mission of ESA’s Cosmic Vision 2015–2025 programme and a mission of international collaboration between ESA and NASA, will explore the Sun and heliosphere from close up and out of the ecliptic plane. It was launched on 10 February 2020 04:03 UTC from Cape Canaveral and aims to address key questions of solar and heliospheric physics pertaining to how the Sun creates and controls the Heliosphere, and why solar activity changes with time. To answer these, the mission carries six remote-sensing instruments to observe the Sun and the solar corona, and four in-situ instruments to measure the solar wind, energetic particles, and electromagnetic fields. In this paper, we describe the science objectives of the mission, and how these will be addressed by the joint observations of the instruments onboard. Methods. The paper first summarises the mission-level science objectives, followed by an overview of the spacecraft and payload. We report the observables and performance figures of each instrument, as well as the trajectory design. This is followed by a summary of the science operations concept. The paper concludes with a more detailed description of the science objectives. Results. Solar Orbiter will combine in-situ measurements in the heliosphere with high-resolution remote-sensing observations of the Sun to address fundamental questions of solar and heliospheric physics. The performance of the Solar Orbiter payload meets the requirements derived from the mission’s science objectives. Its science return will be augmented further by coordinated observations with other space missions and ground-based observatories.

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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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Geometry, Kinematics, and Heliospheric Impact of a Large CME-driven Shock in 2017 September

Cited by 38 publications

References 48 publications

Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

The Solar Orbiter mission

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

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