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The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances
Song, H. Q.1,2,3; Chen, Y.1,2; Li, B.1,2; Li, L. P.3; Zhao, L.4; He, J. S.5; Duan, D.5; Cheng, X.6; Zhang, J.7
2017-02-10
Source PublicationASTROPHYSICAL JOURNAL LETTERS
Volume836Issue:1
AbstractSolar filaments/prominences are one of the most common features in the corona, which may lead to energetic coronal mass ejections (CMEs) and flares when they erupt. Filaments are about 100 times cooler and denser than the coronal material, and physical understanding of their material origin remains controversial. Two types of scenarios have been proposed: one argues that the filament plasma is brought into the corona from photosphere or chromosphere through a siphon or evaporation/injection process, while the other suggests that the material condenses from the surrounding coronal plasma due to thermal instability. The elemental abundance analysis is a reasonable clue to constrain the models, as the siphon or evaporation/injection model would predict that the filament material abundances are close to the photospheric or chromospheric ones, while the condensation model should have coronal abundances. In this Letter, we analyze the elemental abundances of a magnetic cloud that contains the ejected filament material. The corresponding filament eruption occurred on 1998 April 29, accompanying an M6.8 class soft X-ray flare located at the heliographic coordinates S18E20 (NOAA 08210) and a fast halo CME with the linear velocity of 1374 km s(-1) near the Sun. We find that the abundance ratios of elements with low and high first ionization potential such as Fe/O, Mg/O, and Si/O are 0.150, 0.050, and 0.070, respectively, approaching their corresponding photospheric values 0.065, 0.081, and 0.066, which does not support the coronal origin of the filament plasma.
SubtypeArticle
KeywordSun: Abundances Sun: Coronal Mass Ejections (Cmes) Sun: Filaments Prominences
WOS HeadingsScience & Technology ; Physical Sciences
Funding OrganizationNSFC(41274177 ; NSFC(41274177 ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120 ; NSF(AGS-1156120 ; open research program of CAS Key Laboratory of Solar Activity ; open research program of CAS Key Laboratory of Solar Activity ; 41274175 ; 41274175 ; AGS-1344835 ; AGS-1344835 ; 41331068) ; 41331068) ; AGS-1621686) ; AGS-1621686) ; NSFC(41274177 ; NSFC(41274177 ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120 ; NSF(AGS-1156120 ; open research program of CAS Key Laboratory of Solar Activity ; open research program of CAS Key Laboratory of Solar Activity ; 41274175 ; 41274175 ; AGS-1344835 ; AGS-1344835 ; 41331068) ; 41331068) ; AGS-1621686) ; AGS-1621686)
DOI10.3847/2041-8213/aa5d54
WOS KeywordCORONAL MASS EJECTIONS ; CYCLE 23 ; WIND ; ACE ; REGION ; DISTRIBUTIONS ; SPACECRAFT ; PROTONS ; MISSION ; SWICS
Indexed BySCI
Language英语
Funding OrganizationNSFC(41274177 ; NSFC(41274177 ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120 ; NSF(AGS-1156120 ; open research program of CAS Key Laboratory of Solar Activity ; open research program of CAS Key Laboratory of Solar Activity ; 41274175 ; 41274175 ; AGS-1344835 ; AGS-1344835 ; 41331068) ; 41331068) ; AGS-1621686) ; AGS-1621686) ; NSFC(41274177 ; NSFC(41274177 ; US NSF(AGS-1249270) ; US NSF(AGS-1249270) ; NSF(AGS-1156120 ; NSF(AGS-1156120 ; open research program of CAS Key Laboratory of Solar Activity ; open research program of CAS Key Laboratory of Solar Activity ; 41274175 ; 41274175 ; AGS-1344835 ; AGS-1344835 ; 41331068) ; 41331068) ; AGS-1621686) ; AGS-1621686)
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000402913600001
Citation statistics
Cited Times:7[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/8809
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.Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48105 USA
5.Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China
6.Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China
7.George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA
Recommended Citation
GB/T 7714
Song, H. Q.,Chen, Y.,Li, B.,et al. The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances[J]. ASTROPHYSICAL JOURNAL LETTERS,2017,836(1).
APA Song, H. Q..,Chen, Y..,Li, B..,Li, L. P..,Zhao, L..,...&Zhang, J..(2017).The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances.ASTROPHYSICAL JOURNAL LETTERS,836(1).
MLA Song, H. Q.,et al."The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances".ASTROPHYSICAL JOURNAL LETTERS 836.1(2017).
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