GPU-accelerated computing of three-dimensional solar wind background

作     者：FENG XueShang ZHONG DingKun XIANG ChangQing ZHANG Yao 

作者机构：SIGMA Weather GroupState Key Laboratory for Space Weather Center for Space Science and Applied ResearchChinese Academy of Sciences 

出 版 物：《Science China Earth Sciences》 (中国科学（地球科学英文版）)

年 卷 期：2013年第56卷第11期

页      面：1864-1880页

核心收录：

学科分类：070802[理学-空间物理学] 07[理学] 08[工学] 080203[工学-机械设计及理论] 0708[理学-地球物理学] 0802[工学-机械工程] 

基　　金：supported by the National Natural Science Foundation of China(Grant Nos.41031066,41231068,41274192,41074121&41074122) the National Basic Research Program of China(Grant No.2012CB825601) the Knowledge Innovation Program of the Chinese Academy of Sciences(Grant No.KZZD-EW-01-4) the Specialized Research Fund for State Key Laboratories 

主　　题：space weather modeling SIP-CESE MHD model GPU computing 

摘      要：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 2058 and 2062 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.