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Return to the Moon:New perspectives on lunar exploration

Science Bulletin 2024年第13期69卷 2136-2148页

作者： Yangting Lin Wei Yang Hui Zhang Hejiu Hui Sen Hu Long Xiao Jianzhong Liu Zhiyong Xiao Zongyu Yue Jinhai Zhang Yang Liu Jing Yang Honglei Lin Aicheng Zhang Dijun Guo Sheng Gou Lin Xu Yuyang He Xianguo Zhang Liping Qin Zongcheng Ling Xiongyao Li Aimin Du Huaiyu He Peng Zhang jinbin cao Xianhua Li Key Laboratory of Earth and Planetary Physics Institute of Geology and GeophysicsChinese Academy of SciencesBeijing 100029China State Key Laboratory for Mineral Deposits Research and School of Earth Sciences and Engineering Nanjing UniversityNanjing 210023China State Key Laboratory of Geological Processes and Mineral Resources School of Earth SciencesChina University of GeosciencesWuhan 430074China Institute of Geochemistry Chinese Academy of SciencesGuiyang 550002China Planetary Environmental and Astrobiological Research Laboratory School of Atmospheric SciencesSun Yat-sen UniversityZhuhai 519082China National Space Science Center Chinese Academy of SciencesBeijing 100190China Deep Space Exploration Laboratory/CAS Key Laboratory of Crust-Mantle Materials and Environments University of Science and Technology of ChinaHefei 230026China Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space SciencesShandong UniversityWeihai 264209China Technology and Engineering Center for Space Utilization Chinese Academy of SciencesBeijing 100094China School of Space and Environment Beihang UniversityBeijing 100191China

Lunar exploration is deemed crucial for uncovering the origins of the Earth-Moon system and is the first step for advancing humanity’s exploration of deep *** the past decade,the Chinese Lunar Exploration Program(CLEP),also known as the Chang’e(CE)Project,has achieved remarkable *** has successfully developed and demonstrated the engineering capability required to reach and return from the lunar ***,the CE Project has made historic firsts with the landing and on-site exploration of the far side of the Moon,along with the collection of the youngest volcanic samples from the Procellarum KREEP *** achievements have significantly enhanced our understanding of lunar *** on this success,China has proposed an ambitious crewed lunar exploration strategy,aiming to return to the Moon for scientific exploration and *** plan encompasses two primary phases:the first crewed lunar landing and exploration,followed by a thousand-kilometer scale scientific expedition to construct a geological cross-section across the lunar *** the limitations of current lunar exploration efforts and China’s engineering and technical capabilities,this paper explores the benefits of crewed lunar exploration while leveraging synergies with robotic *** study refines fundamental lunar scientific questions that could lead to significant breakthroughs,considering the respective engineering and technological *** research lays a crucial foundation for defining the objectives of future lunar exploration,emphasizing the importance of crewed missions and offering insights into potential advancements in lunar science.

关键词： Crewed lunar exploration Water and volatiles Composition and structure of lunar interior Volcanic activity and evolution of lunar mantle Space weathering and radiation environments Exploration technology

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Magnetospheric Physics in China

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空间科学学报 2018年第5期38卷 694-762页

作者： cao jinbin YANG Junying Space Science Institute School of Space and Environment Beihang UniversityBeijing 100191

In the past two years, much progress has been made in magnetospheric physics by using the data of Double Star Program, Cluster, THEMIS, RBSP, Swarm, MMS, ARTEMIS, MESSENGER missions etc., or by computer simulations. This paper briefly reviews these works based on papers selected from the 227 publications from January 2016 to December 2017. The subjects cover most sub-branches of magnetospheric physics,including geomagnetic storm, magnetospheric substorm, magnetic reconnection, solar wind-magnetosphereionosphere interaction, radiation belt, plasmasphere, outer magnetosphere, magnetotail, geomagnetic field,auroras, and currents.

关键词：物理中国计算机模拟相互作用出版物暴风雨磁气圈报纸

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Magnetospheric Physics in China:2020-2021

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空间科学学报 2022年第4期42卷 628-652页

作者： cao jinbin YANG Junying Space Science Institute School of Space and EnvironmentBeihang UniversityBeijing 100191 Key Laboratory of Space Environment Monitoring and Information Processing Ministry of Industry and Information TechnologyBeijing 100191

In the past two years,many progresses were made in magnetospheric physics by the data of OMNI,SuperMAG networks,Double Star Program,Cluster,THEMIS,RBSP,DMSP,DEMETER,NOAA,Van Allen Probes,GOES,Geotail,Swarm,MMS,BeiDa,Fengyun,ARTEMIS,MESSENGER,Juno,Chinese Mars ROVER,MAVEN,Tianwen-1,Venus Express,Lunar Prospector e.g.,or by computer *** paper briefly reviews these works based on 356 papers published from January 2020 to December *** subjects covered various sub-branches of Magnetospheric Physics,including solar wind-magnetosphere-ionosphere interaction,inner magnetosphere,outer magnetosphere,magnetic reconnection,planetary magnetosphere.

关键词： Solar wind-magnetosphere-ionosphere interaction Inner magnetosphere Outer magnetosphere Magnetic reconnection Planetary magnetosphere

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Spatial distribution of ion polytropic index joint-modulated by temperature anisotropy and MHD disturbances in the southern high latitude magnetosheath

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Science China(Technological Sciences) 2018年第3期61卷 381-388页

作者： PANG XueXia cao jinbin DENG ZeChao JIA PengYing School of Space and Environment Beihang University Hebei Key Lab of Optic-electronic Information and Materials College of Physics Science and Technology Hebei University

Using the Cluster data from 2001 to 2010, we studied spatial distribution of effective ion polytropic index in the southern high latitude magnetosheath, and joint-modulation of ion polytropic index by temperature anisotropy and MHD disturbances. The magnetosheath ions generally experience various polytropic processes with different polytropic index. The median polytropic indexes of magnetosheath ions in the GSE X-Y plane decrease toward the bow shock. Near the magnetopause, the median polytropic indexes are basically between isothermal and adiabatic except in the duskside flank close to the terminator. The analysis of correlation coefficient of perturbed ion number density with parallel magnetic field CC_δnδB_‖ and ion temperature anisotropy parameter A_T, indicates that the dominant MHD disturbance near magnetopause is slow mode with larger ion temperature anisotropy, and there are various modes of MHD disturbances with insignificant ion temperature anisotropy near the bow *** polytropic index modulated by slow mode disturbances is generally larger than that modulated by fast mode disturbances, and the larger ion temperature anisotropy, the larger polytropic index. The median polytropic indexes modulated jointly by slow mode disturbances and the strong ion temperature anisotropy can be larger than 1.0, while those modulated by fast mode disturbances and weak temperature anisotropy can be even possibly close to zero. Moreover, because of pronounced dusk-favored asymmetry of ion temperature anisotropy, the median polytropic index in the dawnside flank of the magnetosheath near the terminator is smaller than that in the duskside flank of the magnetosheath. The good correspondence between the distributions of median polytropic indexes and ion temperature anisotropy and MHD disturbances indicates that the ion temperature anisotropy and MHD disturbances determine the distribution of the polytropic index in the magnetosheath.

关键词： polytropic index magnetosheath temperature anisotropy

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The response of plasma parameters and energy transport in the plasma sheet to interplanetary magnetic field B_z

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Science China(Technological Sciences) 2021年第7期64卷 1528-1534页

作者： REN GanMing cao jinbin YANG Jian DUNLOP Malcolm Wray School of Space and Environment Beihang UniversityBeijing100191China Key Laboratory of Space Environment Monitoring and Information Processing of MIIT Beijing102206China

We use 9 years data of Cluster to study the dependencies of plasma parameters and energy transport in the plasma sheet on the lasting time of northward/southward interplanetary magnetic field(IMF). The plasma parameters and energy transport in the plasma sheet always respond to the change of IMF direction by more or less time. The ion density starts to increase/decrease remarkably at 80 min after northward/southward IMF turning. The ion temperature starts to decrease at 25 min after northward IMF turning, whereas it starts to increase at 80 min after southward IMF turning. The earthward convection velocity within15 min after northward IMF turning almost equals to that within 15 min period after southward IMF turning. However at time greater than 15 min after southward IMF turning, the earthward convection velocity under southward IMF starts to remarkably increase. The response time(15 min) of magnetospheric convection velocity is well consistent with the response times of nightside ionospheric convection to southward IMF turning. The enthalpy flux is larger than kinetic flux by about three orders of magnitudes, and thus the enthalpy flux plays a dominant role in the plasma sheet energy transport. The enthalpy flux does not weaken immediately after northward IMF turning. The enthalpy flux within 15 min after northward IMF turning is comparable to or even slightly larger than that within 15 min after southward IMF. The enthalpy flux starts to decrease at times greater than15 min after northward IMF turning, whereas it starts to increase at times greater than 15 min after southward IMF turning. The result that the enhanced energy transport during the 15 min period after northward IMF turning may explain previous observation that substorms frequently occur shortly after northward IMF turning.

关键词： plasma sheet energy transport enthalpy flux response time

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The source of tropospheric tides

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Earth and Planetary Physics 2020年第5期4卷 449-460页

作者： Xing Li WeiXing Wan jinbin cao ZhiPeng Ren Key Laboratory of Earth and Planetary Physics Institute of Geology and GeophysicsChinese Academy of SciencesBeijing 100029China School of Space and Environment Beihang UniversityBeijing 100083China Key Laboratory of Space Environment Monitoring and Information Processing Ministry of Industry and Information TechnologyBeijing 100083China Beijing National Observatory of Space Environment Institute of Geology and GeophysicsChinese Academy of SciencesBeijing 100029China Innovation Academy for Earth Science Chinese Academy of SciencesBeijing 100029China University of the Chinese Academy of Sciences Beijing 100049China

With the method of Hough mode decomposition(HMD),the tidal sources of the three main tidal components,namely,the migrating components DW1(diurnal westward propagating wavenumber 1)and SW2(semidiurnal westward propagating wavenumber 2)and the non-migrating component DE3(diurnal eastward propagating wavenumber 3),at the tropospheric altitudes(1–12 km)and in the latitude range of±60°,were obtained from National Centers for Environmental Prediction(NCEP)Climate Forecast System Reanalysis(CFSR)data during the interval from 1988 to *** analyzed these sources in detail at 6 km and obtained the main properties of their yearly *** DW1 source was found to present a weak seasonal variation in the lower latitudes(about±10°–15°).That is,the amplitudes of the DW1 sources were larger in the summer months than in the winter months,and DW1 presented semi-annual variation near the equator(±10°)such that the DW1 source was larger at the equinoxes than at the *** addition,the SW2 source was symmetric and was stronger in the southern hemisphere than in the northern *** SW2 source presented remarkable annual and semi-annual variation such that the amplitudes were largest during the March equinox months and larger during the June solstice *** contrast,DE3 appeared mainly around the equatorial latitudes within about±30°.The DE3 source presented remarkable semiannual variation that was larger around the solstices than the equinoxes in the southern hemisphere,and it was opposite in the northern *** HMD,we found that the tropospheric tides were primarily dominated by some leading propagating Hough modes,specifically,the(1,1),(2,3),and(3,3)modes;the influences of the other Hough modes were *** consequences of an El Niño–Southern Oscillation modulation of tidal amplitudes for the energy and momentum budgets of the troposphere may now be expected to attract *** summary,the above yearly variations of the main tidal sources and

关键词： tropospheric tides Hough mode decomposition yearly variations

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Wavenumber-4 spectral component extracted from TIMED/SABER observations

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Earth and Planetary Physics 2020年第5期4卷 436-448页

The wavenumber spectral components WN4 at the mesosphere and low thermosphere(MLT)altitudes(70–10 km)and in the latitude range between±45°are obtained from temperature data(T)observed by the Sounding of the Atmosphere using Broadband Emission Radiometry(SABER)instruments on board the National Aeronautics and Space Administration(NASA)’s Thermosphere–Ionosphere–Mesosphere Energetics and Dynamics(TIMED)spacecraft during the 11-year solar period from 2002 to *** analyze in detail these spectral components WNk and obtain the main properties of their vertical profiles and global *** report that all of the wavenumber spectral components WNk occur mainly around 100 km altitude,and that the most prominent component is the wavenumber spectral component WN4 *** these long duration temperature data with results of previous investigations,we have found that the yearly variation of spectral component WN4 is similar to that of the eastward propagating non-migrating diurnal tide with zonal wavenumber 3(DE3)at the low latitudes,and to that of the semi-diurnal tide with zonal wavenumber 2(SE2)at the mid-latitudes:the amplitudes of the A4 are larger during boreal summer and autumn at the low-latitudes;at the mid-latitudes the amplitudes have a weak peak in *** addition,the amplitudes of component WN4 undergo a remarkable short period variation:significant day-to-day variation of the spectral amplitudes A4 occurs primarily in July and September at the *** summary,we conclude that the non-migrating tides DE3 and SE2 are likely to be the origins,at the low-latitudes and the mid-latitudes in the MLT region,respectively,of the observed wavenumber spectral component WN4.

关键词： TIMED observations wavenumber spectral components non-migrating tides short period variation

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Progress of Double Star Program

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空间科学学报 2006年第Z1期26卷 7-13页

作者： LIU Zhenxing cao jinbin Center for Space Science and Applied Research Chinese Academy of Sciences Beijing 100080 China Center for Space Science and Applied Research Chinese Academy of Sciences Beijing 100080 China

The Double Star Programme (DSP) is the first joint space mission between China and ESA. The mission, which is made of two spacecraft, is designed to investigate the magnetospheric global processes and their response to the interplanetary disturbances in conjunction with the Cluster mission. The first spacecraft, TC-1 (Tan Ce means "Explorer"), was launched on 30 December 2003, and the second one, TC-2, on 25 July 2004 on board two Chinese Long March 2C. Due to the importance of and success of DSP, both CNSA and ESA approved the extension of DSP. This paper presents DSP mission and some important scientific results made based on the data of DSP.

关键词： Double Star Program, Magnetosphere

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Differences between onset times of bursty bulk flows (BBFs) of two Cluster satellites in the magnetotail

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Science China(Technological Sciences) 2012年第5期55卷 1178-1183页

作者： cao jinbin WANG ZhiQiang MA YuDuan CAI CunLin Space Science Institute School of AstronauticsBeihang UniversityBeijing 100191China Key Laboratory for Space Weather/CSSAR Beijing 100190China Graduate University Chinese Academy of SciencesBeijing 100080China

This paper, using the dataset of BBFs （bursty bulk flows） observed by two Cluster satellites C1 and C4, studies the difference between onset times of BBFs observed by C1 and C4. It is found that the onset time differences of most of BBFs observed by Cl and C4 are smaller than 60 s. The average onset time difference of BBFs of CI and C4 is 68.5 s. The probabilities of onset time difference of BBFs of C1 and C4 larger than 30, 60, 90 and 120 s are respectively 55%, 35%, 27% and 23%. The largest onset time difference of BBFs of C1 and C4 decreases with the increase of earthward component of maximum velocities of BBFs. The onset time difference of BBFs of C1 and C4 results from the velocity inhomogeneity inside the flow channel of BBF, which may be produced in propagation path and/or in source region of BBFs. Such a wide range of onset time difference of BBFs suggests that the velocity inhomogeneity inside the flow channel of BBF is various. These results are very important to the current study of substorm research based on THEMIS data because they indicate that it is impossible to determine the onset time of BBF with a single satellite.

关键词： bursty bulk flows (BBFs) onset time difference substorm

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Magnetospheric Physics in China: 2012–2014

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空间科学学报 2014年第5期34卷 605-647页

作者： cao jinbin YANG Junying Space Science Institute School of Astronautics Beihang University

In the past two years, many progresses have been made in magnetospheric physics by using the data of Double Star Program, Cluster, THEMIS and RBSP missions, or by computer simulations. This paper briefly reviews these works based on papers selected from the 126 publications from March 2012 to March 2014. The subjects cover various sub-branches of magnetospheric physics,including geomagnetic storm, magnetospheric substorm and magnetic reconnection.

关键词： Magnetospheric physics Cluster Double Star THEMIS

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