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A large polar-crown prominence composed of different segments spanning nearlythe entire solar disk erupted on 2010 December 6. Prior to the eruption, thefilament in the active region part splits into two layers: a lower layer and anelevated layer. The eruption occurs in several episodes. Around 14:12 UT, thelower layer of the active region filament breaks apart, one part ejects towardsthe west, while the other part ejects towards the east, which leads to theexplosive eruption of the eastern quiescent filament. During the early risephase, part of the quiescent filament sheet displays strong rolling motion(observed by STEREO$\_$B) in the clockwise direction (views from east to west)around the filament axis. This rolling motion appears to start from the borderof the active region, then propagates towards the east. AIA observes anothertype of rotating motion: in some other parts of the erupting quiescentprominence the vertical threads turn horizontal, then turn upside down. Theelevated active region filament does not erupt until 18:00 UT, when theerupting quiescent filament already reaches a very large height. We develop twosimplified three-dimensional models which qualitatively reproduce the observedrolling and rotating motions. The prominence in the models is assumed toconsist of a collection of discrete blobs that are tied to particular fieldlines of a helical flux rope. The observed rolling motion is reproduced bycontinuous twist injection into the flux rope in Model 1 from the active regionside. Asymmetric reconnection induced by the asymmetric distribution of themagnetic fields on the two sides of the filament may cause the observed rollingmotion. The rotating motion of the prominence threads observed by AIA isconsistent with the removal of the field line dips in Model 2 from the top downduring the eruption.

Rotating Motions and Modeling of the Erupting Solar Polar Crown Prominence on 2010 December 6