Models for the motions of flare loops and ribbons

doi:10.1007/BF00686534

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	Models for the motions of flare loops and ribbons
	Lin J(林隽); FORBES, TG; PRIEST, ER; BUNGEY, TN; LIN, J
发表期刊	SOLAR PHYSICS
	1995-07
卷号	159 期号:2 页码:275-299
DOI	10.1007/BF00686534
产权排序	第1完成单位
收录类别	SCI
摘要	We have found a conformal mapping which is valid for any magnetic boundary condition at the photosphere and which can be used to determine the evolution of an open, two-dimensional magnetic field configuration as it relaxes to a closed one. Solutions obtained with this mapping are in quasi-static equilibrium, and they contain a vertical current sheet and have line-tied boundary conditions. As a specific example, we determine the solution for a boundary condition corresponding to a submerged, two-dimensional dipole below the photosphere. We assume that the outer edges of the hottest X-ray loops correspond to field lines mapping from the outer edges of the H alpha ribbon to the lower tip of the current sheet where field lines reconnect at a Y-type neutral line which rises with time. The cooler H alpha loops are assumed to lie along the field lines mapping to the inner edges of the flare ribbons. With this correspondence between the plasma structures and the magnetic field we determine the shrinkage that field lines are observed to undergo as they are disconnected from the neutral line. During the early phase of the flare, we predict that shrinkage inferred from the height of the H alpha and X-ray loops is close to 100% of the loop height. However, the shrinkage should rapidly decrease with time to values on the order of 20% by the late phase. We also predict that the shrinkage in very large loops obeys a universal scaling law which is independent of the boundary condition, provided that the field becomes self-similar (i.e., all field lines have the same shape) at large distances. Specifically, for any self-similar field containing a Y-type neutral line, the observed shrinkage at large distances should decrease as (Delta X/X(R))(-2/3), where Delta X is the ribbon width and X(R) is the ribbon separation. Finally, we discuss the relation between the electric field at the neutral line and the motions of the flare loops and ribbons.
语种	英语
学科领域	Astronomy & Astrophysics
文章类型	Article
ISSN	0038-0938
URL	查看原文
WOS记录号	WOS:A1995RN23600005
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	RECONNECTION ; CORONA
引用统计	被引频次：40[WOS] [WOS记录] [WOS相关记录]
文献类型	期刊论文
条目标识符	http://ir.ynao.ac.cn/handle/114a53/6019
专题	太阳物理研究组
通讯作者	LIN, J
推荐引用方式 GB/T 7714	Lin J,FORBES, TG,PRIEST, ER,et al. Models for the motions of flare loops and ribbons[J]. SOLAR PHYSICS,1995,159(2):275-299.
APA	林隽,FORBES, TG,PRIEST, ER,BUNGEY, TN,&LIN, J.(1995).Models for the motions of flare loops and ribbons.SOLAR PHYSICS,159(2),275-299.
MLA	林隽,et al."Models for the motions of flare loops and ribbons".SOLAR PHYSICS 159.2(1995):275-299.

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