| Eruption of an Active-Region Filament Driven by an Emerging Bipole |
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| 作者姓名： | Yun-Chun Jiang Yuan-Deng Shen and Jing-Xiu Wang National Astronomical Observatories / Yunnan Observatory Chinese Academy of Sciences Kunming National Astronomical Observatories Chinese Academy of Sciences Beijing |
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| 作者单位： | Yun-Chun Jiang1，Yuan-Deng Shen1 and Jing-Xiu Wang2 1 National Astronomical Observatories / Yunnan Observatory，Chinese Academy of Sciences，Kunming 650011; 2 National Astronomical Observatories，Chinese Academy of Sciences，Beijing 100012 |
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| 基金项目： | 国家自然科学基金;国家自然科学基金 |
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| 摘 要： | 1 INTRODUCTION Filaments are cool, dense material suspended in the hot, tenuous corona. It is widely accepted that the global magnetic field surrounding the filaments plays a key role in their formation, structure and stability (Tandberg-Hanssen1995). Fil…
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| 关 键 词： | Sun: filaments—Sun: flares—Sun: magnetic fields—Sun: corona—Sun: X-rays |
Eruption of an Active-Region Filament Driven by an Emerging Bipole |
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| Yun-Chun Jiang,Yuan-Deng Shen and Jing-Xiu Wang National Astronomical Observatories / Yunnan Observatory,Chinese Academy of Sciences,Kunming , National Astronomical Observatories,Chinese Academy of Sciences,Beijing .Eruption of an Active-Region Filament Driven by an Emerging Bipole[J].Chinese Journal of Astronomy and Astrophysics,2007,7(1):129-140. |
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| Authors: | Yun-Chun Jiang Yuan-Deng Shen Jing-Xiu Wang |
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| Institution: | [1]National Astronomical Observatories / Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011 [2]National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 |
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| Abstract: | A section of an S-shaped filament underwent an eruption in a sigmoidal active re- gion (AR 8027) with S-shaped coronal structure, which was clearly driven by a bipole emerg- ing below the NW end of the filament. The bipole with two separating poles showed typical characteristics of emerging flux region (EFR) and its axis rotated counterclockwise. Two can- celling magnetic features (CMFs) were formed between the two poles and adjacent flux with opposite polarity and substantial flux cancellation occurred in them. Along with the bipole emergence the filament was strongly disturbed. Just before the filament eruption, two X-ray loops overlying the filament brightened, an axial X-ray structure and then a cusp structure appeared. During the eruption first the whole filament rose and then its SE end broke away from the chromosphere, while its NW end remained stationary. Helical structure and motion were observed in the filament body and downward mass motion in the two ends. After the eruption, a major part of the filament remained and slowly returned to quiescence, and an X-ray arcade and an axial structure formed. These observations suggest that the eruption re-sulted from the interaction between the bipole and the overlying loops. We provide evidence that steady photospheric reconnection between their footprints took place in the two CMFs during the bipole emergence. |
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| Keywords: | Sun: filaments - Sun: flares - Sun: magnetic fields - Sun: corona - Sun:X-rays |
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