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Effects of reconnection on the coronal mass ejection process
Lin J(林隽)1,2; Forbes, TG1; Lin, J
Source PublicationJOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
2000-02-01
Volume105Issue:A2Pages:2375-2392
DOI10.1029/1999JA900477
Contribution Rank第2完成单位
Indexed BySCI
AbstractThis work investigates how magnetic reconnection affects the acceleration of coronal mass ejections (CMEs) and how the acceleration in turn affects the reconnection pro-cess. To model the CME process, we use a two-dimensional flux rope model, which drives the ejection by means of a catastrophic loss of mechanical equilibrium. Our model provides a method for relating the motion of the ejected material to the reconnection rate in the current sheet created by the erupting field. In the complete absence of reconnection the tension force associated with the current sheet is always strong enough to prevent the flux rope from escaping from the Sun. However, our results imply that even a fairly small reconnection rate is sufficient to allow the flux rope to escape. Specifically, for a coronal density model that decreases exponentially with height we find that average Alfven Mach number M-A for the inflow into the reconnection site can be as small as M-A = 0.005 and still be fast enough to give a plausible eruption. The best fit to observations is obtained by assuming an inflow rate on the order of M-A approximate to 0.1. With this value the energy output matches the temporal behavior inferred for the long duration events often associated with CMEs. The model also suggests an explanation for the peculiar motion of giant X-ray arches reported by Svestka et al. [1995, 1997]. X-ray arches are the large loops associated with CMEs which are similar in form to "post"-flare loops, but they have an upward motion that is often different. Instead of continually slowing with time, the arches move upward at a rate that remains nearly constant or may even increase with time. Here we show how the difference can be explained by reversal of the gradient of the coronal Alfven speed with height.
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0148-0227
URL查看原文
Archive Date2000-12-31
WOS IDWOS:000085189300007
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordMAGNETIC-FIELD EVOLUTION ; YOHKOH SXT IMAGES ; FORCE-FREE FIELD ; ERUPTIVE FLARES ; 2-RIBBON FLARES ; ACTIVE REGIONS ; FLUX-ROPE ; MODEL
Citation statistics
Cited Times:417[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6034
Collection太阳物理研究组
Corresponding AuthorLin, J
Affiliation1.Institute for the Study of Earth, Ocean, and Space (EOS), University of New Hampshire, Durham
2.Yunnan Observatory, Kunming, Yunnan, People's Republic of China
Recommended Citation
GB/T 7714
Lin J,Forbes, TG,Lin, J. Effects of reconnection on the coronal mass ejection process[J]. JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS,2000,105(A2):2375-2392.
APA Lin J,Forbes, TG,&Lin, J.(2000).Effects of reconnection on the coronal mass ejection process.JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS,105(A2),2375-2392.
MLA Lin J,et al."Effects of reconnection on the coronal mass ejection process".JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 105.A2(2000):2375-2392.
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