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Boundary element-free method for elastodynamics

Science china(Physics,{1. & Astronomy) 2005年第6期48卷 641-657页

作者： cheng yumin1.& peng Miaojuan2 1. shanghai institute of applied mathematics and mechanics, shanghai university, shanghai 200072, china 2. Department of Civil Engineering, shanghai university, shanghai 200072, china 1. shanghai {1. of applied mathematics and mechanics Shanghai University 200072 Shanghai China 2. Department of Civil Engineering Shanghai University 200072 Shanghai China

The moving least-square approximation is discussed first. Sometimes the method can form an ill-conditioned equation system, and thus the solution cannot be obtained correctly. A Hilbert space is presented on which an orthogonal function system mixed a weight function is defined. Next the improved moving least-square approximation is discussed in detail. The improved method has higher computational efficiency and precision than the old method, and cannot form an ill-conditioned equation system. A boundary element-free method (BEFM) for elastodynamics problems is presented by combining the boundary integral equation method for elastodynamics and the improved moving least-square approximation. The boundary element-free method is a meshless method of boundary integral equation and is a direct numerical method compared with others, in which the basic unknowns are the real solutions of the nodal variables and the boundary conditions can be applied easily. The boundary element-free method has a higher computational efficiency and precision. In addition, the numerical procedure of the boundary element-free method for elastodynamics problems is presented in this paper. Finally, some numerical examples are given.

关键词： moving least-square approximation, improved moving least-square approximation, elastodynamics, boundary integral equation, meshless method, boundary element-free method, Fourier eigen transform.

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The Lyman-alpha Solar Telescope(LST) for the ASO-S mission——Ⅱ. design of LST

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Research in Astronomy and Astrophysics 2019年第11期19卷 33-48页

作者： Bo Chen Hui Li Ke-Fei Song Quan-Feng Guo Pei-Jie Zhang Ling-Ping He Shuang Dai Xiao-Dong Wang Hai-Feng Wang Chun-Long Liu Hong-Ji Zhang Guang Zhang Yunqi Wang Shi-Jie Liu Hong-Xin Zhang Lei Liu Shi-Lei Mao Yang Liu Jia-Hao peng peng Wang Liang Sun Yang Liu Zhen-Wei Han Yan-Long Wang Kun Wu Guang-Xing Ding peng Zhou Xin Zheng Ming-Yi Xia Qing-Wen Wu Jin-Jiang Xie Ya Chen Shu-Mei Song Hong Wang Bo Zhu Chang-Bo Chu Wen-Gang Yang Li Feng Yu Huang Wei-Qun Gan Ying Li Jing-Wei Li Lei Lu Jian-Chao Xue Bei-Li Ying Ming-Zhe Sun cheng Zhu Wei-Min Bao Lei Deng Zeng-Shan Yin Changchun institute of Optics FineMechanics and PhysicsChinese Academy of SciencesChangchun 130033China State Key Laboratory of applied Optics Changchun 130033China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210034China School of Astronomy and Space Science University of Science and Technology of ChinaHefei 230026China Xi’an institute of Optics and Precision {1. Chinese Academy of SciencesXi’an 710119China Shandong university Weihai 264209China Innovation Academy for Microsatellites Chinese Academy of SciencesShanghai 201210China

As one of the three payloads for the Advanced Space-based Solar Observatory(ASO-S)mission,the Lyman-alpha(Lyα)Solar Telescope(LST)is composed of three instruments:a Solar Corona Imager(SCI),a LyαSolar Disk Imager(SDI)and a full-disk White-light Solar Telescope(WST).When working in-orbit,LST will simultaneously perform high-resolution imaging observations of all regions from the solar disk to the inner corona up to 2.5 R⊙(R⊙stands for the mean solar radius)with a spatial resolution of 4.8′′and 1.2′′for coronal and disk observations,respectively,and a temporal resolution of 30–1.0 s and 1.1.0 s for coronal and disk observations,*** maximum exposure time can be up to20 s due to precise pointing and image stabilization *** the three telescopes of LST,SCI is a dual-waveband coronagraph simultaneously and independently observing the inner corona in the HI Lyα(1.1.6±1. nm)line and white light(WL)(700±40 nm)wavebands by using a narrowband Lyαbeam splitter and has a field of view(FOV)from 1.1.to 2.5 R⊙.The stray-light suppression level can attain1.^-6 B⊙(B⊙is the mean brightness of the solar disk)at 1.1.R⊙and≤5×1.^-8 B⊙at 2.5 R⊙.SDI and WST are solar disk imagers working in the Lyαline and 360.0 nm wavebands,respectively,which adopt an off-axis two-mirror reflective structure with an FOV up to 1.2 R⊙,covering the inner coronal edge area and relating to coronal *** present the up-to-date design for the LST payload.

关键词： telescopes—instrumentation high angular resolution—Sun flares—Sun coronal mass ejections(CMEs)—Sun UV radiation

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