Quadrupolar Dimmings During a Partial Halo Coronal Mass Ejection Event |
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| Authors: | J Yang Y Jiang R Zheng J Hong Y Bi L Yang |
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| Institution: | (1) Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA;(2) UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK;(3) Observatoire de Paris, LESIA, UMR 8109, CNRS, 92195 Meudon Principal Cedex, France;(4) Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary |
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| Abstract: | We present detailed observations of the formations of four distinct coronal dimmings during a flare of 17 September 2002,
which was followed by an eruption of a huge coronal loop system, and then an over-and-out partial halo coronal mass ejection
(CME), with the same direction as the loop system eruption but laterally far offset from the flare site. Among the four dimmings,
two compact ones were symmetrically located in the opposite polarity regions immediately adjacent to the highly sheared magnetic
polarity inversion line in the flare region, and hence were probably composed of bipolar double dimmings due to a flux-rope
eruption and represented its evacuated footpoints. However, another nearby compact dimming and a remote diffuse one were formed
in the opposite polarity footpoint regions of the eruptive loop system, and thus probably consisted of a pair of dimmings
magnetically linked by the erupting loop system and also indicated its evacuated footpoints. The loop system might have played
a role in guiding the erupting flare field and producing the over-and-out CME, but its eruption might simply have been pushed
out by the erupting flare field, because there was no reconnection signature between them. From comparison with a derived
potential-field source-surface (PFSS) magnetic configuration, our observations consistently suggest that the dimmings were
formed in pairs and originated from the eruptions of the two different magnetic systems. We thus define them as “quadrupolar
dimmings.” |
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