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We present an investigation of the polar crown prominence that erupted on2012 March 12. This prominence is observed at the southeast limb by SDO/AIA(end-on view) and displays a quasi vertical-thread structure. BrightU-shape/horn-like structure is observed surrounding the upper portion of theprominence at 171 angstrom before the eruption and becomes more prominentduring the eruption. The disk view of STEREO-B shows that this long prominenceis composed of a series of vertical threads and displays a half loop-likestructure during the eruption. We focus on the magnetic support of theprominence vertical threads by studying the structure and dynamics of theprominence before and during the eruption using observations from SDO andSTEREO-B. We also construct a series of magnetic field models (sheared arcademodel, twisted flux rope model, and unstable model with hyperbolic flux tube(HFT)). Various observational characteristics appear to be in favor of thetwisted flux rope model. We find that the flux rope supporting the prominenceenters the regime of torus instability at the onset of the fast rise phase, andsignatures of reconnection (post-eruption arcade, new U-shape structure, risingblobs) appear about one hour later. During the eruption, AIA observes darkribbons seen in absorption at 171 angstrom corresponding to the bright ribbonsshown at 304 angstrom, which might be caused by the erupting filament materialfalling back along the newly reconfigured magnetic fields. Brightenings at theinner edge of the erupting prominence arcade are also observed in all AIA EUVchannels, which might be caused by the heating due to energy released fromreconnection below the rising prominence.

Magnetic Structure and Dynamics of the Erupting Solar Polar Crown Prominence on 2012 March 12