Solar stereoscopy - where are we and what developments do we require to progress?
文献类型：期刊论文
| 作者 | Wiegelmann, T.1; Inhester, B.1; Feng, L.1,2
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| 刊名 | ANNALES GEOPHYSICAE
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| 出版日期 | 2009 |
| 卷号 | 27期号:7页码:2925-2936 |
| 关键词 | Solar physics, astrophysics,and astronomy Corona and transition region Magnetic fields Ultraviolet emissions |
| 英文摘要 | Observations from the two STEREO-spacecraft give us for the first time the possibility to use stereoscopic methods to reconstruct the 3-D solar corona. Classical stereoscopy works best for solid objects with clear edges. Consequently an application of classical stereoscopic methods to the faint structures visible in the optically thin coronal plasma is by no means straight forward and several problems have to be treated adequately: 1) First there is the problem of identifying one-dimensional structures-e. g. active region coronal loops or polar plumes-from the two individual EUVimages observed with STEREO/EUVI. 2) As a next step one has the association problem to find corresponding structures in both images. This becomes more difficult as the angle between STEREO-A and B increases. 3) Within the reconstruction problem stereoscopic methods are used to compute the 3-D-geometry of the identified structures. Without any prior assumptions, e. g., regarding the footpoints of coronal loops, the reconstruction problem has not one unique solution. 4) One has to estimate the reconstruction error or accuracy of the reconstructed 3-D-structure, which depends on the accuracy of the identified structures in 2-D, the separation angle between the spacecraft, but also on the location, e. g., for east-west directed coronal loops the reconstruction error is highest close to the loop top. 5) Eventually we are not only interested in the 3-D-geometry of loops or plumes, but also in physical parameters like density, temperature, plasma flow, magnetic field strength etc. Helpful for treating some of these problems are coronal magnetic field models extrapolated from photospheric measurements, because observed EUV-loops outline the magnetic field. This feature has been used for a new method dubbed " magnetic stereoscopy". As examples we show recent application to active region loops. |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 类目[WOS] | Astronomy & Astrophysics ; Geosciences, Multidisciplinary ; Meteorology & Atmospheric Sciences |
| 研究领域[WOS] | Astronomy & Astrophysics ; Geology ; Meteorology & Atmospheric Sciences |
| 关键词[WOS] | CORONAL MAGNETIC-FIELDS ; ACTIVE-REGION LOOPS ; FORCE-FREE ; OPTIMIZATION APPROACH ; VECTOR MAGNETOGRAMS ; EUV IMAGES ; RECONSTRUCTION ; GEOMETRY ; TEMPERATURES ; INFORMATION |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000268622700028 |
| 源URL | [http://libir.pmo.ac.cn/handle/332002/15900]  |
| 专题 | 紫金山天文台_太阳高能及相关物理过程研究团组 |
| 作者单位 | 1.Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany 2.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China |
| 推荐引用方式 GB/T 7714 | Wiegelmann, T.,Inhester, B.,Feng, L.. Solar stereoscopy - where are we and what developments do we require to progress?[J]. ANNALES GEOPHYSICAE,2009,27(7):2925-2936. |
| APA | Wiegelmann, T.,Inhester, B.,&Feng, L..(2009).Solar stereoscopy - where are we and what developments do we require to progress?.ANNALES GEOPHYSICAE,27(7),2925-2936. |
| MLA | Wiegelmann, T.,et al."Solar stereoscopy - where are we and what developments do we require to progress?".ANNALES GEOPHYSICAE 27.7(2009):2925-2936. |
入库方式： OAI收割
来源：紫金山天文台
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