Volume 637, May 2020
|Number of page(s)||10|
|Section||The Sun and the Heliosphere|
|Published online||13 May 2020|
Numerical simulation and data analysis of the 23 July 2012 SEP event observed by ACE, STEREO-A, and STEREO-B
School of Science, Harbin Institute of Technology, Shenzhen 518055, PR China
2 College of Sciences, Henan Agricultural University, Zhengzhou 450002, PR China
3 State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, PR China
4 College of Earth Sciences, University of Chinese Academy of Sciences, Beijing 100049, PR China
Accepted: 16 March 2020
An extremely powerful, superfast interplanetary coronal mass ejection (ICME) from the Sun on 23 July 2012 was detected by widely separated multiple spacecraft, namely STEREO-A, STEREO-B, and ACE, together with the ICME-driven shock and associated solar energetic particles (SEPs). We use the Parker spiral magnetic field model to analyze the relationship between the propagation of the shock and the SEP flux. Furthermore, we simulate the SEP event by numerically solving the three-dimensional focused transport equation of SEPs considering the shock as the moving source of energetic particles. To deal with the fact that protons and electrons behave completely differently for both parallel and perpendicular diffusion, for simplicity, we use the same diffusion model format for the simulations of protons and electrons but with different parameters. We find that the analysis can qualitatively explain the important features of the SEP flux observed by the multiple spacecraft simultaneously. In addition, the numerical results for both energetic protons and electrons approximately agree with multi-spacecraft observations.
Key words: shock waves / turbulence / scattering / Sun: coronal mass ejections (CMEs) / Sun: particle emission
© ESO 2020
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