Rapid Rotation of an Erupting Prominence and the Associated Coronal Mass Ejection on 13 May 2013

Abstract

In this paper, we report the multiwavelength observations of an erupting prominence and the associated CME on 13 May 2013. The event occurs behind the western limb in the field of view of SDO/AIA. The prominence is supported by a highly twisted magnetic flux rope and shows rapid rotation in the counterclockwise direction during the rising motion. The rotation of the prominence lasts for $\sim$47 minutes. The average period, angular speed, and linear speed are $\sim$806 s, $\sim$0.46 rad min${}^{-1}$, and $\sim$355 km s${}^{-1}$, respectively. The total twist angle reaches $\sim$7$\pi$, which is considerably larger than the threshold for kink instability. Writhing motion during 17:42$-$17:46 UT is clearly observed by SWAP in 174 Å and EUVI on board the behind STEREO spacecraft in 304 Å after reaching an apparent height of $\sim$405\,Mm. Therefore, the prominence eruption is most probably triggered by kink instability. A pair of conjugate flare ribbons and post-flare loops are created and observed by STA/EUVI. The onset time of writhing motion is consistent with the commencement of the impulsive phase of the related flare. The 3D morphology and positions of the associated CME are derived using the graduated cylindrical shell (GCS) modeling. The kinetic evolution of the reconstructed CME is divided into a slow-rise phase ($\sim$330 km s${}^{-1}$) and a fast-rise phase ($\sim$1005 km s${}^{-1}$) by the writhing motion. The edge-on angular width of the CME is a constant (60${}^{\circ }$), while the face-on angular width increases from 96${}^{\circ }$ to 114${}^{\circ }$, indicating a lateral expansion. The latitude of the CME source region decreases slightly from $\sim$18${}^{\circ }$ to $\sim$13${}^{\circ }$, implying an equatorward deflection during propagation.

arXiv comment28 pages, 20 figures, accepted for publication in Solar Physics, comments are welcome

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• The Structure of Coronal Mass Ejections Recorded by the K-Coronagraph at Mauna Loa Solar Observatory
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