Quadrupolar Dimmings During a Partial Halo Coronal Mass Ejection Event

Details Quadrupolar Dimmings During a Partial Halo Coronal Mass Ejection Event Quadrupolar Dimmings During a Partial Halo Coronal Mass Ejection Event

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011soph..270..551y&link_type=abstract

Solar Physics, Volume 270, Issue 2, pp.551-559

Physics

3

Corona, Activity, Coronal Mass Ejections, Low Coronal Signatures, Magnetic Fields, Corona, Prominences, Activity

Scientific paper

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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