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Prediction method for October 2.03 solar storm

science china(Technological {2.) 2006年第5期49卷 629-640页

作者： xie yanqiong1, 2. 3,{2., feng xueshang1 & zhong dingkun1, 2.1. state key laboratory of space weather, center for space science and applied research, chinese academy of sciences, Beijing 100080, china 2. Graduate School, chinese academy of sciences, Beijing 100039, china 3. Institute of Meteorology, PLA University of science and Technology, Nanjing 2.1.01, china state key {2. of {2. weather Center for Space Science applied research Chinese Academy of Sciences Beijing 100080 China Graduate School Chinese Academy of Sciences Beijing 100039 China Institute of Meteorology PLA University of Science Technology Nanjing 211101 China

Aiming at two intense shock events on October 2. and 2., 2.03, this paper presents a two-step method, which combines synoptic analysis of space weather ——“observing” and quantitative prediction ——“palpating”, and then uses it to test predictions. In the first step of “observing”, on the basis of observations of the solar source surface magnetic field, interplanetary scintillation (IPS) and ACE spacecraft, we find that the propagation of the shocks is asymmetric relative to the normal direction of their solar sources, and the Earth is located near the direction of the fastest speed and the greatest energy of the shocks. As the two fast ejection shock events, the fast explosion of coronal mass of the extremely high temperature, the strong magnetic field, and the high speed background solar wind are also helpful to their rapid propagation. In the second step of “palpating”, we adopt a new membership function of the fast shock events for the ISF method. The predicted results show that for the onset time of the geomagnetic disturbance, the relative errors between the observational and the predicted results are 1.8% and 6.7%; and for the magnetic disturbance magnitude, the relative errors are 4.1% and 3.1%, re- spectively. Furthermore, the comparison among the predicted results of our two-step method with those of five other prevailing methods shows that the two-step method is advantageous. The results tell us that understanding the physical features of shock propagation thoroughly is of great importance in improving the prediction precision.

关键词： solar storm, interplanetary shock, interplanetary scintillation, two-step method, ISF method.

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GPU-accelerated computing of three-dimensional solar wind background

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science china Earth {2. 2013年第11期56卷 1864-1880页

作者： feng xueshang {2. dingkun XIANG ChangQing ZHANG Yao SIGMA weather Group State Key Laboratory for Space Weather Center for Space Science and Applied ResearchChinese Academy of Sciences

High-performance computational models are required to make the real-time or faster than rea^-time numerical prediction of adverse space weather events and their influence on the geospace environment. The main objective in this article is to explore the application of programmable graphic processing units （GPUs） to the numerical space weather modeling for the study of solar wind background that is a crucial part in the numerical space weather modeling. GPU programming is realized for our Solar-Interplanetary-CESE MHD model （SIP-CESE MHD model） by numerically studying the solar corona/interplanetary so- lar wind. The global solar wind structures are obtained by the established GPU model with the magnetic field synoptic data as input. Meanwhile, the time-dependent solar surface boundary conditions derived from the method of characteristics and the mass flux limit are incorporated to couple the observation and the three-dimensional （3D） MHD model. The simulated evolu- tion of the global structures for two Carrington rotations 2.58 and 2.62.is compared with solar observations and solar wind measurements t^om spacecraft near the Earth. The MHD model is also validated by comparison with the standard potential field source surface （PFSS） model. Comparisons show that the MHD results are in good overall agreement with coronal and interplanetary structures, including the size and distribution of coronal holes, the position and shape of the streamer belts, and the transition of the solar wind speeds and magnetic field polarities.

关键词： space weather modeling SIP-CESE MHD model GPU computing

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快速射电暴X射线对应体的量子电动力学磁重联起源

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science Bulletin 2023年第17期68卷 1857-1861页

作者：谢雨耿金军朱熹炜赵忠海雷柱袁文强赵刚吴雪峰乔宾 state key {2. of Nuclear Physics and Technology Center for Applied Physics and Technologyand HEDPSSchool of PhysicsPeking UniversityBeijing 100094China research center of Laser Fusion China Academy of Engineering PhysicsMianyang 621900China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210023China key laboratory for Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100094China School of Astronomy and space sciences University of Science and Technology of ChinaHefei 230026China Frontiers science center for Nano-optoelectronic Peking UniversityBeijing 100094China

快速射电暴(FRB)是宇宙中短时标的射电闪耀现象.近期,来自于SGR 1935+2.54的一个独特的FRB(FRB 2.042.)和非热X射线爆发的成协的天文探测,证实了FRB起源于磁坨星的可能性.然而,无论是快速射电暴还是非热X射线的物理起源都不确定.制约相... 详细信息

快速射电暴(FRB)是宇宙中短时标的射电闪耀现象.近期,来自于SGR 1935+2.54的一个独特的FRB(FRB 2.042.)和非热X射线爆发的成协的天文探测,证实了FRB起源于磁坨星的可能性.然而,无论是快速射电暴还是非热X射线的物理起源都不确定.制约相关研究进展的重要的原因之一是磁坨星磁层附近磁场强度接近施温格极限,此时量子电动力学(QED)效应(特别是正负电子对产生效应)主导了相对论等离子体过程,使其超快、超强的能量释放的过程异常复杂.本文针对这类磁陀星附近的非热X-ray产生机制提出了精确的理论模型,将小尺度的QED磁重联加速与大尺度的光子辐射以及多次康普顿散射自洽地耦合在一起,进行了跨尺度的数值模拟.其数值结果与我国慧眼卫星Insight-HXMT的观测数据的时间和光谱特征非常一致,表明与FRB成协的X射线暴可能来自磁陀星磁层内的QED重联过程.这类模拟方法可以推广到更为广泛、复杂的跨尺度天体物理现象的研究.

关键词：量子电动力学康普顿散射正负电子对 X射线磁重联光子辐射能量释放对应体

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Solar X-ray and EUV imager on board the FY-3E satellite

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Light(science & Applications) 2022年第12期11卷 2939-2951页

作者： Bo Chen Xiao-Xin Zhang Ling-Ping He Ke-Fei Song Shi-Jie Liu Guang-Xing Ding Jin-Ping Dun Jia-wei Li Zhao-Hui Li Quan-feng Guo Hai-feng Wang Xiao-Dong Wang Yun-Qi Wang Hong-Ji Zhang Guang Zhang Zhen-wei Han Shuang Dai Pei-Jie Zhang Liang Sun Yang Liu software engineer Peng Wang Kun Wu Chen Tao Shi-Lei Mao Gui Mei Liang Yang Li-Heng Chen Chun-Yang Han Bin Huang Yang Liu mechanical engineer Shuai Ren Peng Zhou Ze-Xiwei Xiao-Xue Zhang Yue Zhang Xin Zheng Yang Wang Ya Chen Jing-Jiang xie Fei He Qiao Song wei-Guo Zong Xiu-Qing Hu Peng Zhang Jing-Song Wang {2.-Dong Yang Changchun Institute of Optics Fine Mechanics and PhysicsChinese Academy of SciencesChangchunChina state key {2. of {2. Optics Chinese Academy of SciencesChangchunChina National Satellite Meteorological center China Meteorological AdministrationBeijingChina key laboratory of {2. {2. National Center for Space WeatherChina Meteorological AdministrationBeijingChina Innovation center for fengyun Meteorological Satellite(FYSIC) BeijingChina key laboratory of Earth and Planetary Physics Institute of Geology and GeophysicsChinese Academy of SciencesBeijingChina

The solar X-ray and Extreme Ultraviolet Imager(X-EUVI),developed by the Changchun Institute of Optics,Fine Mechanics and Physics,chinese academy of {2.(CIOMP),is the first space-based solar X-ray and Extreme ultraviolet(EUV)imager of china loaded on the fengyun-3E(FY-3E)satellite supported by the china Meteorological Administration(CMA)for solar *** started work on July 11,2.2.,X-EUVI has obtained many solar *** instrument employs an innovative dual-band design to monitor a much larger temperature range on the Sun,which covers 0.6-8.0 nm in the X-ray region with six channels and 19.5 nm in the EUV region.X-EUVI has a field of view of 42.,an angular resolution of 2.5″per pixel in the EUV band and an angular resolution of 4.1″per pixel in the X-ray *** instrument also includes an X-ray and EUV irradiance sensor(X-EUVS)with the same bands as its imaging optics,which measures the solar irradiance and regularly calibrates the solar *** radiometric calibration of X-EUVS on the ground has been completed,with a calibration accuracy of 12..X-EUVI is loaded on the FY-3E satellite and rotates relative to the Sun at a uniform ***-field calibration is conducted by utilizing successive rotation solar *** agreement between preliminarily processed X-EUVI images and SDO/AIA and Hinode/XRT images indicates that X-EUVI and the data processing algorithm operate properly and that the data from X-EUVI can be applied to the space weather forecast system of CMA and scientific investigations on solar activity.

关键词： image instrument Solar

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