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Primary scientific results of Chang'E-1 lunar mission

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Science China Earth sciences 2010年第11期53卷 1565-1581页

作者： OUYANG ZiYuan1,2, li ChunLai1, ZOU Yongliao1, ZHANG HongBo1, Lü Chang1, liU JianZhong1, liU JianJun1, ZUO Wei1, SU Yan1, WEN WeiBin1, BIAN Wei1, ZHAO BaoChang{4. WANG JianYu4. YANG JianFeng{4. CHANG Jin5, WANG HuanYu6, ZHANG Xiaohui7, WANG ShiJin7, WANG Min1, REN Xin1, MU lingli1, KONG DeQing1, WANG XiaoQian1, WANG Fang1, GENG liang1, ZHANG ZhouBin1, ZHENG Lei1, ZHU XinYing1, ZHENG YongChun1, li JunDuo1, ZOU XiaoDuan1, XU Chun1, SHI ShuoBiao1, GAO YiFei1 & GAO GuanNan1 1 National Astronomical observatories, chinese academy of sciences, beijing 100012, China 2 Institute of Geochemistry, chinese academy of sciences, Guiyang 550002, China {4.Xi’an Institute of Optics and Precision Mechanics, chinese academy of sciences, Xi’an 710119, China 4.Shanghai Institute of Technical Physics, chinese academy of sciences, Shanghai 20008{4. China 5 purple mountain observatory, chinese academy of sciences, nanjing {24., China 6 Institute of High Energy Physics, chinese academy of sciences, beijing 10004., China 7 Center for Space Science and Applied Research, chinese academy of sciences, beijing 100190, China 1. National Astronomical observatories Chinese Academy of Sciences Beijing 100012 China2. Institute of Geochemistry Chinese Academy of Sciences Guiyang 550002 China3. Xi’an Institute of Optics and Precision Mechanics Chinese Academy of Sciences Xi’an 710119 China4. Shanghai Institute of Technical Physics Chinese Academy of Sciences Shanghai 200083 China5. Purple Mountain Observatory Chinese Academy of Sciences Nanjing 210008 China6. Institute of High Energy Physics Chinese Academy of Sciences Beijing 100049 China7. Center for Space Science and Applied Research Chinese Academy of Sciences Beijing 100190 China

The strategic plan for the development of the unmanned chinese Lunar Exploration Program is characterized by three distinct stages: "orbiting around", "landing on" and "returning from" the Moon. The first chinese lunar probe, Chang'E-1, which was successfully launched on October 24.h, 2007 at Xichang Satellite Launch Center, and guided to crash on the Moon on March 1st, 2009, at 52.3.°E, 1.50°S, in the north of Mare Fecunditatis, is the first step towards the "orbiting around" stage. The Chang'E-1 mission lasted 4.5 days, exceeding the expected life-span by about four months. A total of 1.3. TB raw data was received from Chang'E-1. It was then processed into 4.TB scientific data products at various levels. Many scientific results have been obtained by analyzing these data, including especially the "global lunar image from the first chinese lunar explora- tion mission". All scientific goals of Chang'E-1 have been achieved. It provides much useful materials for further advances of lunar sciences and planetary chemistry. Meanwhile, these results will serve as a firm basis for future chinese lunar missions.

关键词： lunar orbiter Chang’E-1 scientific data results

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边缘耀斑中HeI 1083.的加宽计算

天文学报 2002年第1期43卷 41-47页

作者：黎辉尤建圻中国科学院紫金山天文台南京210008 中国科学院国家天文台北京100012

讨论了ＨｅＩ１０８３０Ａ的Ｄｏｐｐｌｅｒ和Ｓｔａｒｋ加宽机制以及各种加宽参数的计算，并得到以下一些结论：辐射阻尼对ＨｅＩ１０８３０Ａ的加宽作用与Ｄｏｐｐｌｅｒ效应相比可以忽略；在公认的耀斑电子密度（Ｎｅ＝３... 详细信息

讨论了ＨｅＩ１０８３０Ａ的Ｄｏｐｐｌｅｒ和Ｓｔａｒｋ加宽机制以及各种加宽参数的计算，并得到以下一些结论：辐射阻尼对ＨｅＩ１０８３０Ａ的加宽作用与Ｄｏｐｐｌｅｒ效应相比可以忽略；在公认的耀斑电子密度（Ｎｅ＝３．２ ×１０１３ｃｍ－３）的情况下，所有阻尼项均不可能产生可以觉察的加宽；直到Ｎｅ＝１０１５ｃｍ－３，各种阻尼对线心半宽的增加都不起作用，其值最多在１０－３的量级，因此；线心都可以看作是Ｄｏｐｐｌｅｒ加宽；当Ｎｅ＞１０１４ｃｍ－３时，Ｓｔａｒｋ加宽，特别是电子碰撞的Ｓｔａｒｋ加宽将在ＨｅＩ１０８３０Ａ的加宽中起主要作用；如要Ｓｔａｒｋ加宽谱线的线翼比纯Ｄｏｐｐｌｅｒ加宽大１－２倍，则阻尼加宽半宽与。可以相比拟；如果用Ｓｔａｒｋ加宽来解释１９８９年边缘耀斑的观测轮廓，则电子密度将达１０～（１７）ｃｍ－３，与氦原子的碰撞阻尼（γ３）造成的加宽对Ｉ１２和Ｉ３两分量明显不同，它们对Ｉ１２的影响比对Ｉ３的影响大近一个量级，我们的观测显示Ｉ１２和Ｉ３线翼的延伸基本一样，因而我们的观测

关键词：太阳耀斑谱线加宽激发电离氢线加宽机制

有摄圆型限制性三体问题平动点稳定的充要条件及应用

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天文学报 2005年第1期46卷 37-45页

作者：舒斯会陆本魁陈务深刘福窑中国科学院紫金山天文台

给出了一个判断有摄圆型限制性三体问题平动点稳定性的充要条件.该条件只依赖于平动点变分方程的特征方程系数的一个简单关系,使用很方便.用所得到的条件, 讨论了任意外力摄动对经典圆型限制性三体问题三角平动点稳定性的影响和惯性阻... 详细信息

给出了一个判断有摄圆型限制性三体问题平动点稳定性的充要条件.该条件只依赖于平动点变分方程的特征方程系数的一个简单关系,使用很方便.用所得到的条件, 讨论了任意外力摄动对经典圆型限制性三体问题三角平动点稳定性的影响和惯性阻力摄动对Robe圆型限制性三体问题主要平动点的稳定性的影响.

关键词：动点充要条件平动变分方程摄动特征方程外力限制性稳定性系数

A comparison of co-temporal magnetograms obtained with the Huairou magnetograph and the Spectro-Polarimeter on board Hinode

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Science China(Physics,Mechanics & Astronomy) 2009年第11期52卷 1707-1712页

作者： WANG Dong ZHANG Mei li hui ZHANG HongQi Key Laboratory of Solar Activity National Astronomical ObservatoryChinese Academy of SciencesBeijing 100012China purple mountain observatory Chinese Academy of SciencesNanjing 210008China

We have compared a set of co-temporal magnetograms obtained with the Solar Magnetic Field Tele-scope (SMFT) of the Huairou Solar Observing Station (HSOS) and with the Spectro-Polarimeter of the Solar Optical Telescope (SP/SOT) on board Hinode to check the linear calibrations of SMFT vector magnetograms. The comparison shows that the currently used calibration coefficients of the SMFT have under-estimated the flux density and that a center-to-limb variation of the calibration coefficients was not taken into account by previous calibrations.

关键词： atmosphere magnetic fields magnetic fields

The column density structure of Orion A depicted by N-PDF

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Research in Astronomy and Astrophysics 2020年第4期20卷 139-155页

作者： Yue-hui Ma Hong-Chi Wang Chong li Ji Yang purple mountain observatory and Key Laboratory of Radio Astronomy Chinese Academy of SciencesNanjing 210033China University of chinese academy of sciences Beijing 100049China School of Astronomy and Space Science University of Science and Technology of ChinaAnhui 230026China

We have conducted a large-field simultaneous survey of 12 CO,13.CO and C18O J=1-0 emission toward the Orion A giant molecular cloud(GMC)with a sky coverage of4.4.deg2 using the purple mountain observatory(PMO)-13.7 m mil{3.meter-wavelength *** use the probabi{3.ty distribution function of the column density(N-PDF)to investigate the distribution of molecular hydrogen in the Orion A *** H2 column density,derived from the 13.O emission,of the GMC is dominated by a log-normal distribution in the range from4.1021 to1.5×1023.cm-2 with excesses both at the low-density and high-density *** excess of the low-density end is possibly caused by an extended and low-temperature(10 K)component with velocities in the range of 5-8 km *** with the northern sub-regions,the southern sub-regions of the Orion A GMC contain less gas with column density in NH2>1.25×1022 *** dispersions of the N-PDFs of the sub-regions are found to correlate with the evolutionary stages of the clouds across the Orion A *** structure hierarchy of Orion A GMC is explored with the DENDROGRAM algorithm,and it is found that the GMC is composed of two *** structures except one in the tree have virial parameters less than 2,indicating self-gravity is important on the spatial scales from0.3.to4.*** power-laws and departures from lognormal distributions are found at the high-density end of N-PDFs for active star-forming regions,the N-PDFs of structures in the Orion A GMC are predominantly lognormal on scales from R0.4.to 4.pc.

关键词： ISM:clouds ISM:individual objects(Orion A) ISM:structure stars:formation surveys turbulence

基于半球形瞬时撞击坑的近地天体撞击诱发海啸的深水波模型

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天文学报 2024年第5期65卷 110-120页

作者：李妙蕾史建春马月华张瑞利赵海斌唐梦辉杨大陶中国科学院紫金山天文台行星科学重点实验室南京210023 中国科学技术大学天文与空间科学学院合肥230026 中国科学院上海天文台上海200030 南京大学物理学院南京210093 中国科学院比较行星学卓越创新中心合肥230026 国防科工局重大专项工程中心北京100101

采用初始扰动为半球形瞬时撞击坑作为初始条件,建立了近地天体撞击诱发海啸的深水波模型,应用到特定情形下(小行星直径为14. m、撞击速度与密度采用车里雅宾斯克陨击参数、撞击区域平均海洋深度采用太平洋平均水深4.km)研究了近地天体... 详细信息

采用初始扰动为半球形瞬时撞击坑作为初始条件,建立了近地天体撞击诱发海啸的深水波模型,应用到特定情形下(小行星直径为14. m、撞击速度与密度采用车里雅宾斯克陨击参数、撞击区域平均海洋深度采用太平洋平均水深4.km)研究了近地天体撞击海洋诱发海啸的波高最大值随距离和时间的演化情况.对比不同的瞬时撞击坑模型和传播模型对海啸波高的影响发现:半球形瞬时撞击坑诱发的海啸危害比抛物形瞬时撞击坑更大;相对于深水波模型,浅水波模型给出撞击诱发海啸的规模较大;对于中等尺寸(直径在几百米范围内)的小行星,研究其撞击海洋诱发海啸,更适合采用瞬时撞击坑形状为半球形的深水波模型.

关键词：小行星:普通地球流体力学方法:解析

The dynamical architecture and habitable zones of the quintuplet planetary system 55 Cancri

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Research in Astronomy and Astrophysics 2009年第6期9卷 703-711页

作者： Jiang-hui Ji Hiroshi Kinoshita lin liu Guang-Yu li purple mountain observatory Chinese Academy of Sciences Nanjing 210008 China National Astronomical observatories Chinese Academy of Sciences Beijing 100012 China National Astronomical observatory Mitaka Tokyo 181--8588 Japan Department of Astronomy Nanjing University Nanjing 210093 China

We perform numerical simulations to study the secular orbital evolution and dynamical structure of the quintuplet planetary system 55 Cancri with the self-consistent orbital solutions by Fischer and coworkers. In the simulations, we show that this system can be stable for at least 108 yr. In addition, we extensively investigate the planetary configuration of four outer companions with one terrestrial planet in the wide region of 0.790AU 〈 a 〈 5.900AU to examine the existence of potential asteroid structure and Habitable Zones （HZs）. We show that there are unstable regions for orbits about 4.1, 3.1 and 5：2 mean motion resonances （MMRs） of the outermost planet in the system, and several stable orbits can remain at 3.2 and 1：1 MMRs, which resembles the asteroid belt in the solar system. From a dynamical viewpoint, proper HZ candidates for the existence of more potential terrestrial planets reside in the wide area between 1.0 AU and 2.3.AU with relatively low eccentricities.

关键词： celestial mechanics -- methods n-body simulations -- planetary systems -- stars individual (55 Cancri)

Einstein Probe discovery of EP24.4.8a:A peculiar X-ray transient with an intermediate timescale

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Science China(Physics,Mechanics & Astronomy) 2024年

作者： Wenda Zhang Weimin Yuan Zhixing ling Yong Chen Nanda Rea Arne Rau Zhiming Cai Huaqing Cheng Francesco Coti Zelati lixin Dai Jingwei Hu Shumei Jia Chichuan Jin Dongyue li Paul O’Brien Rongfeng Shen Xinwen Shu Shengli Sun Xiaojin Sun Xiaofeng Wang Lei Yang Bing Zhang Chen Zhang Shuang-Nan Zhang Yonghe Zhang Jie An David Buckley Alexis Coleiro Bertrand Cordier liming Dou Rob Eyles-Ferris Zhou Fan Hua Feng Shaoyu Fu Johan P. U. Fynbo Lluis Galbany Saurabh W. Jha Shuaiqing Jiang Albert Kong Erik Kuulkers Weihua Lei Wenxiong li Bifang liu Mingjun liu Xing liu Yuan liu Zhu liu Chandreyee Maitra Alessio Marino Itumeleng Monageng Kirpal Nandra Jeremy Sanders Roberto Soria lian Tao Junfeng Wang Song Wang Tinggui Wang Zhongxiang Wang Qingwen Wu Xuefeng Wu Dong Xu Yanjun Xu Suijian Xue Yongquan Xue Zijian Zhang Zipei Zhu Hu Zou Congying Bao Fansheng Chen Houlei Chen Tianxiang Chen Wei Chen Yehai Chen Yifan Chen Chenzhou Cui Weiwei Cui Yanfeng Dai Dongwei Fan Ju Guan Dawei Han Dongjie Hou Haibo Hu Maohai Huang Jia Huo Zhenqing Jia Bowen Jiang Ge Jin Chengkui li Junfei li Long{14. li Maoshun li Wei li Zhengda li Tianying lian Congzhan liu Heyang liu Huaqiu liu Fangjun Lu Laidan Luo Jia Ma Xuan Mao Haiwu Pan Xin Pan liming Song {14. Sun Yunyin Tan Qingjun Tang Yihan Tao Hao Wang Juan Wang Lei Wang Wenxin Wang Yilong Wang Yusa Wang Qinyu Wu Haitao Xu Jingjing Xu Xinpeng Xu Yunfei Xu Zhao Xu Changbin Xue Yulong Xue Ailiang Yan Haonan Yang Xiongtao Yang Yanji Yang Juan Zhang Mo Zhang Wenjie Zhang Zhen Zhang Zhen Zhang Ziliang Zhang Donghua Zhao Haisheng Zhao Xiaofan Zhao Zijian Zhao Hongyan Zhou Yilin Zhou Yuxuan Zhu Zhencai Zhu Institut d’Estudis Espacials de Catalunya (IEEC) Max Planck Institute for Extraterrestrial Physics Innovation academy for Microsatellites chinese academy of sciences Department of Physics University of Hong Kong School of Physics and Astronomy University of Leicester School of Physics and Astronomy Sun Yat-sen University National Astronomical observatories Department of Physics Anhui Normal University Shanghai Institute of Technical Physics chinese academy of sciences Physics Department Tsinghua University Nevada Center for Astrophysics University of Nevada Las Vegas Department of Physics and Astronomy University of Nevada Las Vegas chinese academy of sciences South African Astronomical observatory Department of Astronomy University of Cape Town Department of Physics University of the Free State Universite' Paris Cite' CNRS Astroparticule et Cosmologie Universite' Paris Cite' CEA Paris-Saclay School of Astronomy and Space sciences IRFU/DAp-AIM Department of Astronomy Guangzhou University Cosmic Dawn Center (DAWN) Niels Bohr Institute University of Copenhagen Department of Physics and Astronomy Rutgers the State University of New Jersey Institute for Cosmic Ray Research University of chinese academy of sciences The University of Tokyo ESA/ESTEC Noordwijk 2201 AZ The Netherlands Department of Astronomy School of Physics Huazhong University of Science and Technology INAF-Osservatorio Astrofisico di Torino Sydney Institute for Astronomy School of Physics Key Laboratory of Particle Astrophysics The University of Sydney Department of Astronomy Xiamen University Institute for Frontiers in Astronomy and Astrophysics beijing Normal University Department of Astronomy University of Science and Technology Hefei School of Astronomy and Space sciences University of Science and Technology of China Institute of High Energy Physics Institute of Deep Space sciences Deep Space Exploration Laboratory Department of Astronomy School of Physics and Astronomy Yunnan University Shanghai Astronomical observatory chinese academy of Science

We report the discovery of a peculiar X-ray transient,EP24.4.8a,by Einstein Probe （EP） and follow-up studies made with EP,Swift,NICER,GROND,ATCA and other ground-based multiwavelength *** new transient was first detected with Wide-field X-ray Telescope （WXT） on board EP on April 8th,2024.manifested in an intense yet brief X-ray flare lasting for *** flare reached a peak flux of 3.9×10-9erg cm-2s-1in 0.5-4.keV,3.0 times brighter than the underlying X-ray emission detected throughout the *** and more precise follow-up observations by EP/FXT,Swift and NICER confirmed the finding of this new *** X-ray spectrum is non-thermal in 0.5-10 keV,with a power-law photon index varying *** X-ray light curve shows a plateau lasting for4.,followed by a steep decay till becoming undetectable10 d after the initial *** on its temporal property and constraints from previous EP observations,an unusual timescale in the range of 7-23.d is found for EP24.4.8a,which is intermediate between the commonly found fast and long-term *** counterparts have been found in optical and near-infrared,with the earliest observation at 17 h after the initial X-ray detection,suggestive of intrinsically weak emission in these *** demonstrate that the remarkable properties of EP24.4.8a are inconsistent with any of the transient types known so far,by comparison with,in particular,jetted tidal disruption events,gamma-ray bursts,X-ray binaries and fast blue optical *** nature of EP24.4.8a thus remains an *** suggest that EP24.4.8a may represent a new type of transients with intermediate timescales of the order of10 *** detection and follow-ups of more of such objects are essential for revealing their origin.

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The calibration and initial results of the HeI D3.line flash spectrum obtained during the 2008 total solar eclipse

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Science China(Physics,Mechanics & Astronomy) 2009年第11期52卷 1799-1805页

作者： li hui JI HaiSheng NI HouKun ZHANG HaiYing ZHANG YaNan liU HongRui DENG YuanYong WANG DongGuang DU QiuSheng ZHOU Tuanhui li JingWei SHEN JinHua purple mountain observatory 2 Nanjing 210008China nanjing Institute of Astronomical Optics&Technology Nanjing 210042China National Astronomical observatories of China Beijing 100012China

The flash spectra in the HeI D3.line were obtained during the 2008 total solar eclipse. This paper describes the instrument and the calibration of the obtained flash spectrum, and presents our initial results. The average integrated intensity is Eave = 8.13.1013.erg·cm-1· s-1·ster-1 at h = 1100 km, which confirms that the HeI D3.emission is negatively correlated with the solar activity. The surface brightness reaches a maximum of F ave = 8.25×105 erg·cm-2·s-1·ster-1 at about h ≈ (1290 ± 75) km and then decreases exponentially with height when h >1800 km with an exponential index β = 1.63.10-8 cm-1.

关键词： total solar eclipse flash spectrum spectral line