Forward Modeling of SDO/AIA and X-Ray Emission from a Simulated Flux Rope Ejection
Zhao,Xiaozhou1,2,3; Xia,Chun4; Doorsselaere,Tom Van2; Keppens,Rony2,4; Gan,Weiqun1
Source PublicationThe Astrophysical Journal
AbstractAbstract We conduct forward-modeling analysis based on our 2.5 dimensional magnetohydrodynamics (MHD) simulation of magnetic flux rope (MFR) formation and eruption driven by photospheric converging motion. The current sheet (CS) evolution during the MFR formation and eruption process in our MHD simulation can be divided into four stages. The first stage shows the CS forming and gradually lengthening. Resistive instabilities that disrupt the CS mark the beginning of the second stage. Magnetic islands disappear in the third stage and reappear in the fourth stage. Synthetic images and light curves of the seven Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) channels, i.e., 94 ?, 131 ?, 171 ?, 193 ?, 211 ?, 304 ?, and 335 ?, and the 3–25 keV thermal X-ray are obtained with forward-modeling analysis. The loop-top source and the coronal sources of the soft X-ray are reproduced in forward modeling. The light curves of the seven SDO/AIA channels start to rise once resistive instabilities develop. The light curve of the 3–25 keV thermal X-ray starts to go up when the reconnection rate reaches one of its peaks. Quasiperiodic pulsations (QPPs) appear twice in the SDO/AIA 171 ?, 211 ?, and 304 ? channels, corresponding to the period of chaotic (re)appearance and CS-guided displacements of the magnetic islands. QPPs appear once in the SDO/AIA 94 ? and 335 ? channels after the disruption of the CS by resistive instabilities and in the 193 ? channel when the chaotic motion of the magnetic islands reappears.
Keywordmagnetic reconnection magnetohydrodynamics (MHD) methods: numerical radiation mechanisms: thermal Sun: coronal mass ejections (CMEs) Sun: flares
WOS IDIOP:0004-637X-872-2-ab0284
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 210008 Nanjing, People’s Republic of China,
2.Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium;,
3.University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
4.School of Physics and Astronomy, Yunnan University, 650050 Kunming, People’s Republic of China;
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Zhao,Xiaozhou,Xia,Chun,Doorsselaere,Tom Van,et al. Forward Modeling of SDO/AIA and X-Ray Emission from a Simulated Flux Rope Ejection[J]. The Astrophysical Journal,2019,872(2).
APA Zhao,Xiaozhou,Xia,Chun,Doorsselaere,Tom Van,Keppens,Rony,&Gan,Weiqun.(2019).Forward Modeling of SDO/AIA and X-Ray Emission from a Simulated Flux Rope Ejection.The Astrophysical Journal,872(2).
MLA Zhao,Xiaozhou,et al."Forward Modeling of SDO/AIA and X-Ray Emission from a Simulated Flux Rope Ejection".The Astrophysical Journal 872.2(2019).
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