Models for the motions of flare loops and ribbons
文献类型：期刊论文
| 作者 | Lin J(林隽) ; FORBES, TG; PRIEST, ER; BUNGEY, TN
|
| 刊名 | SOLAR PHYSICS
 |
| 出版日期 | 1995-07 |
| 卷号 | 159期号:2页码:275-299 |
| ISSN号 | 0038-0938 |
| 产权排序 | 第一完成单位 |
| 通讯作者 | LIN, J |
| 英文摘要 | 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. |
| 学科主题 | Astronomy & Astrophysics |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | RECONNECTION ; CORONA |
| 收录类别 | SCI |
| 原文出处 | http://link.springer.com/article/10.1007%2FBF00686534 |
| 语种 | 英语 |
| WOS记录号 | WOS:A1995RN23600005 |
| 公开日期 | 2016-05-03 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/6019]  |
| 专题 | 云南天文台_太阳物理研究组 |
| 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.(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. |
入库方式： OAI收割
来源：云南天文台
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