| A Filament—Associated Halo Coronal Mass Ejection |
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| 引用本文： | JunZhang JingxiuWang 等.A Filament—Associated Halo Coronal Mass Ejection[J].中国天文和天体物理学报,2001,1(1):85-98. |
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| 作者姓名： | JunZhang JingxiuWang |
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| 作者单位： | Beijing Astronomical Observatory，National Astronomical Observatories，Chinese Academy of Sciences，Beijing 100012; Lockheed Martin Solar and Astrophysics Laboratory，Palo Alto，CA 94304，USA |
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| 基金项目： | the Major Project 19791090, funded by the
National Natural Science FOundation of China (NSFC) |
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| 摘 要： | 1 INTRODUCTIONCoronal majss ejections (CMEs) are often seen as spectacular eruptions of matter fromthe Sun which propagate outward through the heliosphere and often interact with the Earth'smagnetosphere (Hundhausen, 1997; Gosling, 1997; and references herein). It is well known thatthese interactions can have substalltial consequences on the geomagnetic environment of theEarth, sometimes resulting in damage to satellites (e.g., McAllister et al., 1996; Berdichevskyet al., 1998). CMEs…
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| 关 键 词： | 太阳 日冕 CME 光环 晕圈 |
A Filament-Associated Halo Coronal Mass Ejection |
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| Jun Zhang,Jingxiu Wang,and Nariaki Nitta.A Filament-Associated Halo Coronal Mass Ejection[J].Chinese Journal of Astronomy and Astrophysics,2001,1(1):85-98. |
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| Authors: | Jun Zhang Jingxiu Wang and Nariaki Nitta |
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| Institution: | BeijingAstronomicalObservatory,NationalAstronomicalObservatories,ChineseAcademyofSciences,Beijing1000 |
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| Abstract: | There are only a few observations published so far that show the initiation of a coronal mass ejection(CME) and illustrate the magnetic changes in the surface origin of a CME.Any attempt to connect a CME with its local solar activities is meaningful. In this paper we present a clear instance of a halo CME initiation. A careful analysis of magnetograms shows that the only obvious magnetic changes in the surface region of the CME is a magnetic flux cancellation underneath a quiescent filament. The early disturbance was seen as the slow upward motion in segments of the quiescent filament. Four hours later, the filament was accelerated to about 50 km s^-1 and erupted. While a small part of the material in the filament was ejected into the upper corona, most of the mass was transported to a nearby region. About forty minutes later, the transported mass was also ejected partially to the upper corona. The eruption of the filament triggered a two-ribbon flare, with post-flare loops connecting the flare ribbons. A halo CME, which is inferred to be associated with the eruptive filament, was observed from LASCO/C2 and C3. The halo CME contained two CME events, each event corresponded to a partial mass ejection of the filament. We suggest that the magnetic reconnection at the lower atmosphere is responsible for the filament eruption and the halo CME. |
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| Keywords: | Sun: filament - Sun: magnetic fields-Sun: coronal mass ejection |
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