| Formation of the CME Leading Edge Observed in the 2003 February 18 Event |
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| 作者姓名： | Xing-Ming Bao Hong-Qi Zhang and Jun Lin National Astronomical Observatories Chinese Academy of Sciences Beijing National Astronomical Observatories / Yunnan Observatory Chinese Academy of Sciences Kunming Harvard-Smithsonian Center for Astrophysics Garden Street Cambridge MA USA |
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| 作者单位： | Xing-Ming Bao，Hong-Qi Zhang and Jun Lin National Astronomical Observatories，Chinese Academy of Sciences，Beijing 100012; National Astronomical Observatories / Yunnan Observatory，Chinese Academy of Sciences，Kunming 650011 Harvard-Smithsonian Center for Astrophysics，60 Garden Street，Cambridge，MA 02138，USA |
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| 基金项目： | Supported by the National Natural Science Foundation of China. |
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| 摘 要： | This work investigates a typical coronal mass ejection (CME) observed on 2003 February 18, by various space and ground instruments, in white light, Ha, EUV and X-ray. The Ha and EUV images indicate that the CME started with the eruption of a long filament located near the solar northwest limb. The white light coronal images show that the CME initiated with the rarefaction of a region above the solar limb and followed by the formation of a bright arcade at the boundary of the rarefying region at height 0.46 R(?) above the solar surface. The rarefying process synchronized with the slow rising phase of the eruptive filament, and the CME leading edge was observed to form as the latter started to accelerate. The lower part of the filament brightened in Ha as the filament rose to a certain height and parts of the filament was visible in the GOES X-ray images during the rise. These brightenings imply that the filament may be heated by the magnetic reconnection below the filament in the early stage of the eruption. We suggest that a possible mechanism which leads to the formation of the CME leading edge and cavity is the magnetic reconnection which takes place below the filament after the filament has reached a certain height.
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| 关 键 词： | 太阳 日冕物质抛出 耀斑 暗纹 形成机制 2003年2月 |
Formation of the CME Leading Edge Observed in the 2003 February 18 Event |
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| Xing-Ming Bao,Hong-Qi Zhang and Jun Lin National Astronomical Observatories,Chinese Academy of Sciences,Beijing , National Astronomical Observatories / Yunnan Observatory,Chinese Academy of Sciences,Kunming Harvard-Smithsonian Center for Astrophysics, Garden Street,Cambridge,MA ,USA.Formation of the CME Leading Edge Observed in the 2003 February 18 Event[J].Chinese Journal of Astronomy and Astrophysics,2006,6(6):741-750. |
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| Authors: | Xing-Ming Bao Hong-Qi Zhang Jun Lin |
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| Institution: | [1]National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 [2]National Astronomical Observatories / Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011 [3]Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA |
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| Abstract: | This work investigates a typical coronal mass ejection (CME) observed on 2003 February 18, by various space and ground instruments, in white light, Ha, EUV and X-ray. The Ha and EUV images indicate that the CME started with the eruption of a long filament located near the solar northwest limb. The white light coronal images show that the CME initiated with the rarefaction of a region above the solar limb and followed by the formation of a bright arcade at the boundary of the rarefying region at height 0.46 R(?) above the solar surface. The rarefying process synchronized with the slow rising phase of the eruptive filament, and the CME leading edge was observed to form as the latter started to accelerate. The lower part of the filament brightened in Ha as the filament rose to a certain height and parts of the filament was visible in the GOES X-ray images during the rise. These brightenings imply that the filament may be heated by the magnetic reconnection below the filament in the early stage of the eruption. We suggest that a possible mechanism which leads to the formation of the CME leading edge and cavity is the magnetic reconnection which takes place below the filament after the filament has reached a certain height. |
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| Keywords: | Sun: coronal mass ejections (CMEs) - Sun: filaments - Sun: flares |
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