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The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection
Song, H. Q.1,2,3; Cheng, X.4; Chen, Y.1,2; Zhang, J.5; Wang, B.1,2; Li, L. P.3; Li, B.1,2; Hu, Q.6,7; Li, G.6,7
2017-10-10
Source PublicationASTROPHYSICAL JOURNAL
Volume848Issue:1
AbstractCoronal mass ejections (CMEs) often exhibit the typical three-part structure in the corona when observed with white-light coronagraphs, i.e., the bright leading front, dark cavity, and bright core, corresponding to a high-low-high density sequence. As CMEs result from eruptions of magnetic flux ropes (MFRs), which can possess either lower (e.g., coronal-cavity MFRs) or higher (e.g., hot-channel MFRs) density compared to their surroundings in the corona, the traditional opinion regards the three-part structure as the manifestations of coronal plasma pileup (high density), coronal-cavity MFR (low density), and filament (high density) contained in the trailing part of MFR, respectively. In this paper, we demonstrate that filament-unrelated CMEs can also exhibit the classical three-part structure. The observations were made from different perspectives through an event that occurred on 2011 October 4. The CME cavity corresponds to the low-density zone between the leading front and the high-density core, and it is obvious in the low corona and gradually becomes fuzzy when propagating outward. The bright core corresponds to a high-density structure that is suggested to be an erupting MFR. The MFR is recorded from both edge-on and face-on perspectives, exhibiting different morphologies that are due to projection effects. We stress that the zone (MFR) with lower (higher) density in comparison to the surroundings can appear as the dark cavity (bright core) when observed through white-light coronagraphs, which is not necessarily the coronal-cavity MFR (erupted filament).
SubtypeArticle
KeywordMagnetic Reconnection Sun: Coronal Mass Ejections (Cmes) Sun: Flares
WOS HeadingsScience & Technology ; Physical Sciences
Funding OrganizationShandong Provincial Natural Science Foundation(JQ201710) ; Shandong Provincial Natural Science Foundation(JQ201710) ; Joint Research Fund in Astronomy(U1731102) ; Joint Research Fund in Astronomy(U1731102) ; NSFC grant(41331068 ; NSFC grant(41331068 ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120) ; NSF(AGS-1156120) ; 41774180) ; 41774180) ; Shandong Provincial Natural Science Foundation(JQ201710) ; Shandong Provincial Natural Science Foundation(JQ201710) ; Joint Research Fund in Astronomy(U1731102) ; Joint Research Fund in Astronomy(U1731102) ; NSFC grant(41331068 ; NSFC grant(41331068 ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120) ; NSF(AGS-1156120) ; 41774180) ; 41774180)
DOI10.3847/1538-4357/aa8d1a
WOS KeywordCURRENT SHEET ; MAGNETIC RECONNECTION ; MORPHOLOGY ; ERUPTIONS ; CAVITIES ; ARCADES ; LASCO ; SHOCK ; CME
Indexed BySCI
Language英语
Funding OrganizationShandong Provincial Natural Science Foundation(JQ201710) ; Shandong Provincial Natural Science Foundation(JQ201710) ; Joint Research Fund in Astronomy(U1731102) ; Joint Research Fund in Astronomy(U1731102) ; NSFC grant(41331068 ; NSFC grant(41331068 ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120) ; NSF(AGS-1156120) ; 41774180) ; 41774180) ; Shandong Provincial Natural Science Foundation(JQ201710) ; Shandong Provincial Natural Science Foundation(JQ201710) ; Joint Research Fund in Astronomy(U1731102) ; Joint Research Fund in Astronomy(U1731102) ; NSFC grant(41331068 ; NSFC grant(41331068 ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; open research program of the CAS Key Laboratory of Solar Activity(KLSA201605) ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120) ; NSF(AGS-1156120) ; 41774180) ; 41774180)
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000412575600001
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/20217
Collection太阳物理研究部
Affiliation1.Shandong Univ, Shandong Prov Key Lab Opt Astron & Solar Terr Env, Weihai 264209, Shandong, Peoples R China
2.Shandong Univ, Inst Space Sci, Weihai 264209, Shandong, Peoples R China
3.Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China
4.Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China
5.George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA
6.Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA
7.Univ Alabama, CSPAR, Huntsville, AL 35899 USA
Recommended Citation
GB/T 7714
Song, H. Q.,Cheng, X.,Chen, Y.,et al. The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection[J]. ASTROPHYSICAL JOURNAL,2017,848(1).
APA Song, H. Q..,Cheng, X..,Chen, Y..,Zhang, J..,Wang, B..,...&Li, G..(2017).The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection.ASTROPHYSICAL JOURNAL,848(1).
MLA Song, H. Q.,et al."The Three-part Structure of a Filament-unrelated Solar Coronal Mass Ejection".ASTROPHYSICAL JOURNAL 848.1(2017).
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