On the Nature of the Three-part Structure of Solar Coronal Mass Ejections

Song, Hongqiang; Zhang, J.; Li, Leping; Yang, Zihao; Xia, Li; Zheng, Ruisheng; Chen, Yao

doi:10.3847/1538-4357/aca6e0

Cited by 6 publications

(10 citation statements)

References 38 publications

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“…The new explanation also points out that CMEs can lose the three-part feature gradually when propagating outwards, because the dark cavity vanishes due to the MFR expansion and growth through magnetic reconnections, and/or because the bright core fades away due to the prominence expansion and drainage (Song et al 2023). This answers why only a portion of CMEs have the prototypical structure in previous survey studies (e.g., Vourlidas et al 2013).…”

Section: Introductionmentioning

confidence: 53%

“…Panel (c) shows the observation of C2 at 19:48:05 UT with the reddashed line delineating the CME front. The CME lost its threepart feature due to the MFR expansion and growth as mentioned (Song et al 2019a(Song et al , 2023.…”

Section: Observations and Resultsmentioning

confidence: 95%

“…The animation also demonstrates that the prominence did not erupt outward eventually. This leads to a non-three-part CME in the C2 image (Song et al 2023) as presented in panel (c), where the red-dashed line delineates the CME front.…”

Section: Observations and Resultsmentioning

confidence: 99%

“…However, recent studies pointed out that the traditional opinion is questionable, because some three-part CMEs are not associated with prominence eruptions at all (Howard et al 2017;Song et al 2017Song et al , 2019bWang et al 2022;Song et al 2023). Based on dual-viewpoint and seamless observations from the inner to outer corona, a new explanation on the threepart nature has been proposed, in which the bright frontal loop is formed due to the compression as the magnetic loops are successively pushed to stretch up by the underlying MFR (Low 2001;Chen 2009), the core can correspond to the MFR and/or prominence, and the dark cavity between the CME front and the MFR is a low-density zone with a sheared magnetic field (Song et al 2017(Song et al , 2019a.…”

Section: Introductionmentioning

confidence: 99%

“…Based on dual-viewpoint and seamless observations from the inner to outer corona, a new explanation on the threepart nature has been proposed, in which the bright frontal loop is formed due to the compression as the magnetic loops are successively pushed to stretch up by the underlying MFR (Low 2001;Chen 2009), the core can correspond to the MFR and/or prominence, and the dark cavity between the CME front and the MFR is a low-density zone with a sheared magnetic field (Song et al 2017(Song et al , 2019a. Recent observations clearly demonstrated that both hot channels (Song et al 2023) and coronal cavities (Song et al 2022) evolved into the bright core of three-part CMEs.…”

Section: Introductionmentioning

confidence: 99%

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The Structure of Coronal Mass Ejections Recorded by the K-Coronagraph at Mauna Loa Solar Observatory

Song

Zhou

et al. 2023

ApJL

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Previous survey studies reported that coronal mass ejections (CMEs) can exhibit various structures in white-light coronagraphs, and ∼30% of them have the typical three-part feature in the high corona (e.g., 2–6 R ⊙), which has been taken as the prototypical structure of CMEs. It is widely accepted that CMEs result from eruption of magnetic flux ropes (MFRs), and the three-part structure can be understood easily by means of the MFR eruption. It is interesting and significant to answer why only ∼30% of CMEs have the three-part feature in previous studies. Here we conduct a synthesis of the CME structure in the field of view (FOV) of K-Coronagraph (1.05–3 R ⊙). In total, 369 CMEs are observed from 2013 September to 2022 November. After inspecting the CMEs one by one through joint observations of the Atmospheric Imaging Assembly, K-Coronagraph, and LASCO/C2, we find 71 events according to the criteria: (1) limb event; (2) normal CME, i.e., angular width ≥30°; (3) K-Coronagraph caught the early eruption stage. All (or more than 90% considering several ambiguous events) of the 71 CMEs exhibit the three-part feature in the FOV of K-Coronagraph, while only 30%–40% have the feature in the C2 FOV (2–6 R ⊙). For the first time, our studies show that 90%–100% and 30%–40% of normal CMEs possess the three-part structure in the low and high corona, respectively, which demonstrates that many CMEs can lose the three-part feature during their early evolutions, and strongly supports that most (if not all) CMEs have the MFR structures.

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Section: Introductionmentioning

confidence: 53%

Section: Observations and Resultsmentioning

confidence: 95%

Section: Observations and Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Structure of Coronal Mass Ejections Recorded by the K-Coronagraph at Mauna Loa Solar Observatory

Song

Zhou

et al. 2023

ApJL

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A Revised Graduated Cylindrical Shell Model and its Application to a Prominence Eruption

Zhang

Hou

Bai

2023

Res. Astron. Astrophys.

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In this paper, the well-known graduated cylindrical shell (GCS) model is slightly revised by introducing longitudinal and latitudinal deflections of prominences originating from active regions (ARs). Subsequently, it is applied to the three-dimensional (3D) reconstruction of an eruptive prominence in AR 13110, which produced an M1.7 class flare and a fast coronal mass ejection (CME) on 2022 September 23. It is revealed that the prominence undergoes acceleration from $\sim$246 to $\sim$708 km s$^{-1}$. Meanwhile, the prominence experiences southward deflection by 15$\degr$$\pm$1$\degr$ without longitudinal deflection, suggesting that the prominence erupts non-radially. Southward deflections of the prominence and associated CME are consistent, validating the results of fitting using the revised GCS model. Besides, the true speed of the CME is calculated to be 1637$\pm$15 km s$^{-1}$, which is $\sim$2.3 times higher than that of prominence. This is indicative of continuing acceleration of the prominence during which flare magnetic reconnection reaches maximum beneath the erupting prominence. Hence, the reconstruction using the revised GCS model could successfully track a prominence in its early phase of evolution, including acceleration and deflection.

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Numerical Simulation on the Leading Edge of Coronal Mass Ejection in the Near-Sun Region

Mei,

Ye,

et al. 2023

ApJ

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The coronal mass ejections (CMEs) observed by white-light coronagraphs, such as the Large Angle and Spectrometric Coronagraph (LASCO) C2/C3, commonly exhibit the three-part structure, with the bright leading edge as the outermost part. In this work, we extend previous work on the leading edge by performing a large-scale 3D magnetohydrodynamic numerical simulation on the evolution of an eruptive magnetic flux rope (MFR) in a near-Sun region based on a radially stretched calculation grid in spherical coordination and the incorporation of solar wind. In the early stage, the new simulation almost repeats the previous results, i.e., the expanding eruptive MFR and associated CME bubble interact with the ambient magnetic field, which leads to the appearance of the helical current ribbon/boundary (HCB) wrapping around the MFR. The HCB can be interpreted as a possible mechanism of the CME leading edge. Later, the CME bubble propagates self-consistently to a larger region beyond a few solar radii from the solar center, similar to the early stage of evolution. The continuous growth and propagation of the CME bubbles leading to the HCB can be traced across the entire near-Sun region. Furthermore, we can observe the HCB in the white-light synthetic images as a bright front feature in the large field of view of LASCO C2 and C3.

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On the Nature of the Three-part Structure of Solar Coronal Mass Ejections

Cited by 6 publications

References 38 publications

The Structure of Coronal Mass Ejections Recorded by the K-Coronagraph at Mauna Loa Solar Observatory

The Structure of Coronal Mass Ejections Recorded by the K-Coronagraph at Mauna Loa Solar Observatory

A Revised Graduated Cylindrical Shell Model and its Application to a Prominence Eruption

Numerical Simulation on the Leading Edge of Coronal Mass Ejection in the Near-Sun Region

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