A Revised Graduated Cylindrical Shell Model and its Application to a Prominence Eruption  

作　　者：Qing-Min Zhang Zhen-Yong Hou Xian-Yong Bai 

机构地区：[1]Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Nanjing 210023,China [2]Yunnan Key Laboratory of the Solar Physics and Space Science,Kunming 650216,China [3]School of Earth and Space Sciences,Peking University,Beijing 100871,China [4]National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [5]University of Chinese Academy of Sciences,Beijing 100049,China [6]Key Laboratory of Solar Activity and Space Weather,National Space Science Center,Chinese Academy of Sciences,Beijing 100190,China

出　　处：《Research in Astronomy and Astrophysics》2023年第12期63-72,共10页天文和天体物理学研究（英文版）

基　　金：supported by the National Key R&D Program of China 2022YFF0503003(2022YFF0503000),2021YFA1600500(2021YFA1600502);the National Natural Science Foundation of China(No.12373065);Yunnan Key Laboratory of Solar Physics and Space Science under the No.YNSPCC202206;NSFC under grant No.12373065。

摘　　要：In this paper,the well-known graduated cylindrical shell(GCS)model is slightly revised by introducing longitudinal and latitudinal deflections of prominences originating from active regions(ARs).Subsequently,it is applied to the three-dimensional(3D)reconstruction of an eruptive prominence in AR 13110,which produced an M1.7 class flare and a fast coronal mass ejection(CME)on 2022 September 23.It is revealed that the prominence undergoes acceleration from~246 to~708 km s^(-1).Meanwhile,the prominence experiences southward deflection by 15°±1°without longitudinal deflection,suggesting that the prominence erupts non-radially.Southward deflections of the prominence and associated CME are consistent,validating the results of fitting using the revised GCS model.Besides,the true speed of the CME is calculated to be 1637±15 km s^(-1),which is~2.3 times higher than that of prominence.This is indicative of continuing acceleration of the prominence during which flare magnetic reconnection reaches maximum beneath the erupting prominence.Hence,the reconstruction using the revised GCS model could successfully track a prominence in its early phase of evolution,including acceleration and deflection.

关 键 词：SUN flares-Sun filaments-prominences-Sun coronal mass ejections(CMEs) 

分 类 号：P182.61[天文地球—天文学]