The Origin of Solar Filament Plasma Inferred from In Situ Observations   of Elemental Abundances

doi:10.3847/2041-8213/aa5d54

CORC > 北京大学 > 地球与空间科学学院

	The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances
	Song, H. Q. ; Chen, Y. ; Li, B. ; Li, L. P. ; Zhao, L. ; He, J. S. ; Duan, D. ; Cheng, X. ; Zhang, J.
刊名	ASTROPHYSICAL JOURNAL LETTERS
	2017
关键词	Sun: abundances Sun: coronal mass ejections (CMEs) Sun: filaments, prominences CORONAL MASS EJECTIONS CYCLE 23 WIND ACE REGION DISTRIBUTIONS SPACECRAFT PROTONS MISSION SWICS
DOI	10.3847/2041-8213/aa5d54
英文摘要	Solar 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.; NSFC [41274177, 41274175, 41331068]; US NSF [AGS-1249270]; NSF [AGS-1156120, AGS-1344835, AGS-1621686]; open research program of CAS Key Laboratory of Solar Activity; SCI(E); ARTICLE; 1; 836
语种	英语
内容类型	期刊论文
源URL	[http://ir.pku.edu.cn/handle/20.500.11897/475165]
专题	地球与空间科学学院
推荐引用方式 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.
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.
MLA	Song, H. Q.,et al."The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances".ASTROPHYSICAL JOURNAL LETTERS (2017).