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| 1 | Origin and structures of solar eruptions Ⅰ: Magnetic flux rope显示文摘Coronal mass ejections(CMEs) and solar flares are the large-scale and most energetic eruptive phenomena in our solar system and able to release a large quantity of plasma and magnetic flux from the solar atmosphere into the solar wind. When these high-speed magnetized plasmas along with the energetic particles arrive at the Earth, they may interact with the magnetosphere and ionosphere, and seriously affect the safety of human high-tech activities in outer space. The travel time of a CME to 1 AU is about 1–3 days, while energetic particles from the eruptions arrive even earlier. An efficient forecast of these phenomena therefore requires a clear detection of CMEs/flares at the stage as early as possible. To estimate the possibility of an eruption leading to a CME/flare, we need to elucidate some fundamental but elusive processes including in particular the origin and structures of CMEs/flares. Understanding these processes can not only improve the prediction of the occurrence of CMEs/flares and their effects on geospace and the heliosphere but also help understand the mass ejections and flares on other solar-type stars. The main purpose of this review is to address the origin and early structures of CMEs/flares, from multi-wavelength observational perspective. First of all, we start with the ongoing debate of whether the pre-eruptive configuration, i.e., a helical magnetic flux rope(MFR), of CMEs/flares exists before the eruption and then emphatically introduce observational manifestations of the MFR. Secondly, we elaborate on the possible formation mechanisms of the MFR through distinct ways. Thirdly, we discuss the initiation of the MFR and associated dynamics during its evolution toward the CME/flare. Finally, we come to some conclusions and put forward some prospects in the future. | CHENG Xin GUO Yang DING MingDe | 2017 | Science China Earth Sciences2017，60，8： | 10 |
| 2 | The Chinese Hα Solar Explorer(CHASE) mission: An overview显示文摘The Chinese Hα Solar Explorer(CHASE), dubbed “Xihe”—Goddess of the Sun, was launched on October 14, 2021 as the first solar space mission of China National Space Administration(CNSA). The CHASE mission is designed to test a newly developed satellite platform and to acquire the spectroscopic observations in the Hα waveband. The Hα Imaging Spectrograph(HIS)is the scientific payload of the CHASE satellite. It consists of two observational modes: raster scanning mode and continuum imaging mode. The raster scanning mode obtains full-Sun or region-of-interest spectral images from 6559.7 to 6565.9 ? and from 6567.8 to 6570.6 ? with 0.024 ? pixel spectral resolution and 1 min temporal resolution. The continuum imaging mode obtains photospheric images in continuum around 6689 ? with the full width at half maximum of 13.4 ?. The CHASE mission will advance our understanding of the dynamics of solar activity in the photosphere and chromosphere. In this paper, we present an overview of the CHASE mission including the scientific objectives, HIS instrument overview, data calibration flow, and first results of on-orbit observations. | Chuan Li Cheng Fang Zhen Li MingDe Ding PengFei Chen Ye Qiu Wei You Yuan Yuan MinJie An HongJiang Tao XianSheng Li Zhe Chen Qiang Liu Gui Mei Liang Yang Wei Zhang WeiQiang Cheng JianXin Chen ChangYa Chen Qiang Gu QingLong Huang MingXing Liu ChengShan Han HongWei Xin ChangZheng Chen YiWei Ni WenBo Wang ShiHao Rao HaiTang Li Xi Lu Wei Wang Jun Lin YiXian Jiang LingJie Meng Jian Zhao | 2022 | Science China(Physics,Mechanics & Astronomy)2022，65，8： | 7 |
| 3 | Origin and structures of solar eruptions Ⅱ: Magnetic modeling显示文摘The topology and dynamics of the three-dimensional magnetic field in the solar atmosphere govern various solar eruptive phenomena and activities, such as flares, coronal mass ejections, and filaments/prominences. We have to observe and model the vector magnetic field to understand the structures and physical mechanisms of these solar activities. Vector magnetic fields on the photosphere are routinely observed via the polarized light, and inferred with the inversion of Stokes profiles. To analyze these vector magnetic fields, we need first to remove the 180° ambiguity of the transverse components and correct the projection effect. Then, the vector magnetic field can be served as the boundary conditions for a force-free field modeling after a proper preprocessing. The photospheric velocity field can also be derived from a time sequence of vector magnetic fields.Three-dimensional magnetic field could be derived and studied with theoretical force-free field models, numerical nonlinear force-free field models, magnetohydrostatic models, and magnetohydrodynamic models. Magnetic energy can be computed with three-dimensional magnetic field models or a time series of vector magnetic field. The magnetic topology is analyzed by pinpointing the positions of magnetic null points, bald patches, and quasi-separatrix layers. As a well conserved physical quantity,magnetic helicity can be computed with various methods, such as the finite volume method, discrete flux tube method, and helicity flux integration method. This quantity serves as a promising parameter characterizing the activity level of solar active regions. | GUO Yang CHENG Xin DING MingDe | 2017 | Science China Earth Sciences2017，60，8： | 6 |
| 4 | Calibration procedures for the CHASE/HIS science data显示文摘The Hα line is an important optical line in solar observations containing the information from the photosphere to the chromosphere. To study the mechanisms of solar eruptions and the plasma dynamics in the lower atmosphere, the Chinese Hα Solar Explorer(CHASE) was launched into a Sun-synchronous orbit on October 14, 2021. The scientific payload of the CHASE satellite is the Hα Imaging Spectrograph(HIS). The CHASE/HIS acquires, for the first time, seeing-free Hα spectroscopic observations with high spectral and temporal resolutions. It consists of two observational modes. The raster scanning mode provides full-Sun or region-of-interest spectra at Hα(6559.7-6565.9 ?) and Fe I(6567.8-6570.6 ?) wavebands. The continuum imaging mode obtains full-Sun photospheric images at around 6689 ?. In this paper, we present detailed calibration procedures for the CHASE/HIS science data, including the dark-field and flat-field correction, slit image curvature correction, wavelength and intensity calibration, and coordinate transformation. The higher-level data products can be directly used for scientific research. | Ye Qiu ShiHao Rao Chuan Li Cheng Fang MingDe Ding Zhen Li YiWei Ni WenBo Wang Jie Hong Qi Hao Yu Dai PengFei Chen XiaoSheng Wan Zhi Xu Wei You Yuan Yuan HongJiang Tao XianSheng Li YuKun He Qiang Liu | 2022 | Science China(Physics,Mechanics & Astronomy)2022，65，8： | 3 |
| 5 | Two kinds of tube elements for transient thermal-structural analysis of large space structures 显示文摘 | XUE Mingde DING Yong | 2004 | International Journal for Numerical Methods in Engineering2004，59，10： | 1 |
| 6 | High temperature oxidation and ablation behaviors of HfB_(2)-SiC/SiC coatings for carbon/carbon composites fabricated by dipping-carbonization assisted pack cementation显示文摘To improve the uniformity and the content of HfBin Hf B-Si-based ceramic coating and alleviate the damage of substrate,and then enhance the high-temperature(1700°C)oxidation and cyclic ablation resistances of carbon/carbon composites,a close-knit double layer HfB_(2)-SiC/SiC coatings with a mosaic structure and high content of HfBwere prepared by a novel dipping-carbonization assisted pack cementation methods(DPC–HS/S).In contrast,a HfB_(2)-SiC/SiC coatings were also fabricated by pack cementation(PC–HS/S).Results revealed that the oxidation and ablation protective performances of the DPC–HS/S coatings were superior to those of PC–HS/S coatings.After 30 thermal cycles between 1500°C and room temperature,the mass gain of the coated sample was 0.78%,and the mass loss was 1.65%after oxidation at 1700°C for 156 h.Moreover,under an oxyacetylene torch ablation for 180 s(3 cycles),the linear ablation rate of the DPC–HS/S coated specimen was 1.62μm/s,which was much lower than that of PC–HS/S coated specimen(3.08μm/s). | Lei Zhou Jiaping Zhang Dou Hu Qiangang Fu Wuqing Ding Jiaqi Hou Bing Liu Mingde Tong | 2022 | Journal of Materials Science & Technology2022，，16： | 1 |
| 7 | Two kinds of tube elements for transient thermal-structural analysis of large space structures 显示文摘 | XUE Mingde DING Yong | 2004 | Int J Numerical Methods in Engineering2004，59，10： | 1 |
| 8 | Evolution of the Toroidal Flux of CME Flux Ropes during Eruption显示文摘Coronal mass ejections(CMEs)are large-scale explosions of the coronal magnetic field.It is believed that magnetic reconnection significantly builds up the core structure of CMEs,a magnetic flux rope,during the eruption.However,the quantitative evolution of the flux rope,particularly its toroidal flux,is still unclear.In this paper,we study the evolution of the toroidal flux of the CME flux rope for four events.The toroidal flux is estimated as the magnetic flux in the footpoint region of the flux rope,which is identified by a method that simultaneously takes the coronal dimming and the hook of the flare ribbon into account.We find that the toroidal flux of the CME flux rope for all four events shows a two-phase evolution:a rapid increasing phase followed by a decreasing phase.We further compare the evolution of the toroidal flux with that of the Geostationary Operational Environmental Satellites soft X-ray flux and find that they are basically synchronous in time,except that the peak of the former is somewhat delayed.The results suggest that the toroidal flux of the CME flux rope may be first quickly built up by the reconnection mainly taking place in the sheared overlying field and then reduced by the reconnection among the twisted field lines within the flux rope,as enlightened by a recent 3D magnetohydrodynamic simulation of CMEs. | Chen Xing Xin Cheng Mingde Ding | 2020 | The Innovation2020，1，3： | 1 |
| 9 | Editorial显示文摘The Chinese Hα Solar Explorer(CHASE) was successfully launched on October 14, 2021 as the first solar space mission of China National Space Administration(CNSA). The CHASE mission, dubbed “Xihe” in Chinese(Goddess of the Sun), is designed to test a newly developed satellite platform and to spectroscopically observe the Sun at the Hα line, which is one of the most important optical lines reflecting the dynamics of solar activities in the lower atmosphere. | Cheng Fang MingDe Ding Chuan Li PengFei Chen Wei Zhang | 2022 | Science China(Physics,Mechanics & Astronomy)2022，65，8： | 0 |
| 10 | On the standard of Penaeus orientalis culture pond building显示文摘On the basis of the practical experiences and scientific results in the large scale building of Penaeus orientulis culture pond in the past years, this article puts forward for the first time the main principles and designing standard in the culture pond building from the environmental, ecological, social and economic considerations. It probes systematically into main requirements of the designing scale, farm site selection, arrangement of farm site area, engineering of the pond building, pumping station, water supply and drainage canals and electricity supply engineering of the culture pond. | Li Mingju, Shi Ding, Li Mingde,Institute of Marine Culture of Shandong Province , Qingdao, ChinaZhang YongFishery Design Institute of shandong Province China | 1993 | Acta Oceanologica Sinica1993，12，2： | 0 |
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