Genesis and Impulsive Evolution of the 2017 September 10 Coronal Mass Ejection

Veronig, Astrid; Podladchikova, Tatiana; Dissauer, Karin; Temmer, Manuela; Seaton, Daniel B.; Long, David M.; Guo, Jingnan; Vršnak, Bojan; Harra, L. K.; Kliem, B.

doi:10.3847/1538-4357/aaeac5

Cited by 103 publications

(107 citation statements)

References 91 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: 98%

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: 98%

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

Liu

Zhu

et al. 2019

ApJ

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“…Although strong overexpansion of the CME bubble has been previously observed to drive global EUV waves (cf. Patsourakos et al 2010;Veronig et al 2018), it has not yet been observed to drive Moreton-Ramsey waves. However, Moreton-Ramsey waves have traditionally been observed to be arc-shaped and therefore anisotropic (cf.…”

Section: Introductionmentioning

confidence: 98%

Quantifying the Relationship between Moreton–Ramsey Waves and “EIT Waves” Using Observations of Four Homologous Wave Events

Long

Jenkins²,

Valori³

2019

ApJ

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Freely-propagating global waves in the solar atmosphere are commonly observed using Extreme UltraViolet passbands (EUV or "EIT waves"), and less regularly in H-alpha (Moreton-Ramsey waves). Despite decades of research, joint observations of EUV and Moreton-Ramsey waves remain rare, complicating efforts to quantify the connection between these phenomena. We present observations of four homologous global waves originating from the same active region between 28-30 March 2014 and observed using both EUV and H-alpha data. Each global EUV wave was observed by the Solar Dynamics Observatory, with the associated Moreton-Ramsey waves identified using the Global Oscillations Network Group (GONG) network. All of the global waves exhibit high initial velocity (e.g., 842-1388 km s −1 in the 193Å passband) and strong deceleration (e.g., -1437 --782 m s −2 in the 193Å passband) in each of the EUV passbands studied, with the EUV wave kinematics exceeding those of the Moreton-Ramsey wave. The density compression ratio of each global wave was estimated using both differential emission measure and intensity variation techniques, with both indicating that the observed waves were weakly shocked with a fast magnetosonic Mach number slightly greater than one. This suggests that, according to current models, the global coronal waves were not strong enough to produce Moreton-Ramsey waves, indicating an alternative explanation for these observations. Instead, we conclude that the evolution of the global waves was restricted by the surrounding coronal magnetic field, in each case producing a downward-angled wavefront propagating towards the north solar pole which perturbed the chromosphere and was observed as a Moreton-Ramsey wave.

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“…This figure clearly demonstrates that the CME also possesses the three-part appearance in the EUV passbands. The bulge is formed in the propagation direction of the expanding hot blob, which moves much faster than the CME front, and thus protrudes from the bottom of the CME front (Veronig et al 2018). This illustrates the low-density zone in the low corona can be compressed significantly during propagation outward.…”

Section: The 2017 September 10 Eventmentioning

confidence: 92%

“…This event was recorded by the SOHO and STEREO-A from two perspectives on 2017 September 10 when the STEREO-A was 128 • east of the Earth, which was accompanied by an X8.2 class flare and has been used to investigate various aspects of CMEs (Yan et al 2018;Veronig et al 2018 and references therein). The CME first appeared in the C2 FOV at 16:00 UT at a high linear speed of 3163 km s −1 (CDAW).…”

Section: The 2017 September 10 Eventmentioning

confidence: 99%

The Structure of Solar Coronal Mass Ejections in the Extreme-Ultraviolet Passbands

Song¹

2020

Preprint

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So far most studies on the structure of coronal mass ejections (CMEs) are conducted through white-light coronagraphs, which demonstrate about one third of CMEs exhibit the typical three-part structure in the high corona (e.g., beyond 2 R ⊙ ), i.e., the bright front, the dark cavity and the bright core. In this paper, we address the CME structure in the low corona (e.g., below 1.3 R ⊙ ) through extreme-ultraviolet (EUV) passbands and find that the three-part CMEs in the white-light images can possess a similar three-part appearance in the EUV images, i.e., a leading edge, a low-density zone, and a filament or hot channel. The analyses identify that the leading edge and the filament or hot channel in the EUV passbands evolve into the front and the core later within several solar radii in the white-light passbands, respectively. What's more, we find that the CMEs without obvious cavity in the white-light images can also exhibit the clear three-part appearance in the EUV images, which means that the low-density zone in the EUV images (observed as the cavity in white-light images) can be compressed and/or transformed gradually by the expansion of the bright core and/or the reconnection of magnetic field surrounding the core during the CME propagation outward. Our study suggests that more CMEs can possess the clear three-part structure in their early eruption stage. The nature of the low-density zone between the leading edge and the filament or hot channel is discussed.

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Genesis and Impulsive Evolution of the 2017 September 10 Coronal Mass Ejection

Cited by 103 publications

References 91 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

Quantifying the Relationship between Moreton–Ramsey Waves and “EIT Waves” Using Observations of Four Homologous Wave Events

The Structure of Solar Coronal Mass Ejections in the Extreme-Ultraviolet Passbands

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