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H alpha dimmings associated with the X1.6 flare and halo coronal mass ejection on 2001 October 19
Jiang YC(姜云春)1,2; Ji, HS1; Wang, HM1; Chen HD(陈华东)2; Jiang, YC (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, 40386 N Shore Lane, Big Bear City, CA 92314 USA.
Source PublicationASTROPHYSICAL JOURNAL
2003-11-10
Volume597Issue:2Pages:L161-L164
DOI10.1086/379756
Contribution Rank第2完成单位
Indexed BySCI
KeywordSun : Activity Sun : Coronal Mass Ejections (Cmes) Sun : Filaments Sun : Flares Sun : Magnetic Fields
AbstractAs the optical counterpart of coronal dimmings, we present the first direct evidence of Halpha dimmings associated with the X1.6 flare, filament eruption, and coronal mass ejection (CME) that occurred on 2001 October 19. As two main Halpha flare ribbons parallel to the erupting filament slowly separated, two other ribbons first quickly expanded near the feet of the filament, then their interiors substantially dimmed and became darker than the preflare brightness. This formed two dimming regions with sharp bright edges. The two Halpha dimmings were different from the flare nimbus and the Halpha darkenings found by Ellison, McKenna, & Reid and Neidig et al., respectively, but similar to the coronal "double dimmings" studied by Sterling & Hudson. The coronal dimmings of the event were also observed in 171 Angstrom images from the Transition Region and Coronal Explorer (TRACE). The 171 Angstrom and Halpha dimmings showed very similar evolutions and occurred at the same two sites with opposite magnetic polarities. They formed in the course of the filament eruption, and after the eruption, some 171 Angstrom loops of the postflare arcade developed to connect their inner edges while some loops with footpoints near their outer edges disappeared. Observations from the Solar and Heliospheric Observatory Extreme-ultraviolet Imaging Telescope (SOHO/EIT) showed more extended dimmings associated with the eruption. Only a small portion of EIT dimmings was cospatial with the Halpha dimmings, while the major other portion was associated with the disappeared 171 Angstrom loops. These joint observations are interpreted by using the flux rope model of CMEs, in which the Halpha dimmings represent the evacuated feet of the erupted flux rope. The mass supply of the halo CME could be coming from both the erupted flux rope itself and the lost material close to the flare footpoint regions as shown by Halpha dimmings.
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0004-637X
URL查看原文
WOS IDWOS:000186433200019
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordMAGNETIC RECONNECTION
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Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6060
Collection太阳物理研究组
Corresponding AuthorJiang, YC (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, 40386 N Shore Lane, Big Bear City, CA 92314 USA.
Affiliation1.Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314-9672
2.National Astronomical Observatory/Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming 650011, China
Recommended Citation
GB/T 7714
Jiang YC,Ji, HS,Wang, HM,et al. H alpha dimmings associated with the X1.6 flare and halo coronal mass ejection on 2001 October 19[J]. ASTROPHYSICAL JOURNAL,2003,597(2):L161-L164.
APA Jiang YC,Ji, HS,Wang, HM,Chen HD,&Jiang, YC .(2003).H alpha dimmings associated with the X1.6 flare and halo coronal mass ejection on 2001 October 19.ASTROPHYSICAL JOURNAL,597(2),L161-L164.
MLA Jiang YC,et al."H alpha dimmings associated with the X1.6 flare and halo coronal mass ejection on 2001 October 19".ASTROPHYSICAL JOURNAL 597.2(2003):L161-L164.
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