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

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Abstract

In this paper, we report the multiwavelength observations of an erupting prominence and the associated coronal mass ejection (CME) on 13 May 2013. The event occurs behind the western limb in the field of view of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) spacecraft. 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 ∼ 47 minutes. The average period, angular speed, and linear speed are ∼ 806 sec, ∼ 0.46 rad min−1, and ∼ 355 km s−1, respectively. The total twist angle reaches ∼ 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 Extreme-UltraViolet Imager (EUVI) on board the behind Solar Terrestrial Relations Observatory (STEREO) spacecraft in 304 Å after reaching an apparent height of ∼ 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 (∼ 330 km s−1) and a fast-rise phase (∼ 1005 km s−1) by the writhing motion. The edge-on angular width of the CME is a constant (60∘), while the face-on angular width increases from 96∘ to 114∘, indicating a lateral expansion. The latitude of the CME source region decreases slightly from ∼ 18∘ to ∼ 13∘, implying an equatorward deflection during propagation.

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Data Availability

The AIA data are courtesy of the NASA/SDO science teams. STEREO/SECCHI data are provided by a consortium of the US, UK, Germany, Belgium, and France.

Notes

  1. cdaw.gsfc.nasa.gov/CME_list.

  2. www.e-callisto.org.

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Acknowledgments

The authors appreciate the reviewer for valuable and constructive suggestions that improved the quality of this article. We thank Drs. **aoli Yan and Zhike Xue from Yunnan Observatories for helpful discussions. SDO is a mission of NASA’s Living With a Star Program.

Funding

This work is supported by the National Key R&D Program of China 2022YFF0503003 (2022YFF0503000), 2021YFA1600500 (2021YFA1600502), and NSFC grants (No. 11790302, 11790300).

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  1. Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, CAS, Nan**g, 210023, China

    Yuhao Zhou, Haisheng Ji & Qingmin Zhang

  2. School of Astronomy and Space Science, University of Science and Technology of China, Hefei, 230026, China

    Yuhao Zhou

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Haisheng Ji discovered the rapid rotation of the erupting prominence. Qingmin Zhang performed 3D reconstruction of the related CME. Qingmin Zhang and Yuhao Zhou wrote the main manuscript text and prepared figures and animations. All authors reviewed the manuscript.

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Zhou, Y., Ji, H. & Zhang, Q. Rapid Rotation of an Erupting Prominence and the Associated Coronal Mass Ejection on 13 May 2013. Sol Phys 298, 35 (2023). https://doi.org/10.1007/s11207-023-02126-5

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