Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbons in a Confined Flare
文献类型：期刊论文
| 作者 | Hernandez-Perez, Aaron1; Thalmann, Julia K.1; Veronig, Astrid M.1; Su, Yang2; Gomory, Peter3; Dickson, Ewan C.1 |
| 刊名 | ASTROPHYSICAL JOURNAL
 |
| 出版日期 | 2017-10-01 |
| 卷号 | 847期号:2页码:14 |
| 关键词 | Sun: corona Sun: flares Sun: magnetic fields Sun: X-rays, gamma-rays |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/aa8814 |
| 通讯作者 | Hernandez-Perez, Aaron(aaron.hernandez-perez@uni-graz.at) |
| 英文摘要 | We analyze a confined multiple-ribbon M2.1 flare (SOL2015-01-29T11:42) that originated from a fan-spine coronal magnetic field configuration, within active region NOAA 12268. The observed ribbons form in two steps. First, two primary ribbons form at the main flare site, followed by the formation of secondary ribbons at remote locations. We observe a number of plasma flows at extreme-ultraviolet temperatures during the early phase of the flare (as early as 15 minutes before the onset) propagating toward the formation site of the secondary ribbons. The secondary ribbon formation is co-temporal with the arrival of the pre-flare generated plasma flows. The primary ribbons are co-spatial with Ramaty High Energy Spectroscopic Imager (RHESSI) hard X-ray sources, whereas no enhanced X-ray emission is detected at the secondary ribbon sites. The (E)UV emission, associated with the secondary ribbons, peaks similar to 1 minute after the last RHESSI hard X-ray enhancement. A nonlinear force-free model of the coronal magnetic field reveals that the secondary flare ribbons are not directly connected to the primary ribbons, but to regions nearby. Detailed analysis suggests that the secondary brightenings are produced due to dissipation of kinetic energy of the plasma flows (heating due to compression), and not due to non-thermal particles accelerated by magnetic reconnection, as is the case for the primary ribbons. |
| WOS关键词 | CORONAL MASS EJECTIONS ; X-RAY OBSERVATIONS ; SOLAR-FLARES ; MAGNETIC RECONNECTION ; ACTIVE-REGION ; RHESSI ; MODEL ; BREMSSTRAHLUNG ; DISTRIBUTIONS ; PROMINENCES |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:000416699000015 |
| 出版者 | IOP PUBLISHING LTD |
| 源URL | [http://libir.pmo.ac.cn/handle/332002/18214]  |
| 专题 | 中国科学院紫金山天文台 |
| 通讯作者 | Hernandez-Perez, Aaron |
| 作者单位 | 1.Graz Univ, Inst Phys, IGAM, A-8010 Graz, Austria 2.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China 3.Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia |
| 推荐引用方式 GB/T 7714 | Hernandez-Perez, Aaron,Thalmann, Julia K.,Veronig, Astrid M.,et al. Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbons in a Confined Flare[J]. ASTROPHYSICAL JOURNAL,2017,847(2):14. |
| APA | Hernandez-Perez, Aaron,Thalmann, Julia K.,Veronig, Astrid M.,Su, Yang,Gomory, Peter,&Dickson, Ewan C..(2017).Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbons in a Confined Flare.ASTROPHYSICAL JOURNAL,847(2),14. |
| MLA | Hernandez-Perez, Aaron,et al."Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbons in a Confined Flare".ASTROPHYSICAL JOURNAL 847.2(2017):14. |
入库方式： OAI收割
来源：紫金山天文台
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