|
|
|
题名
|
作者
|
年代
|
出处
|
被引量
|
| 1 | Preliminary results of FeO mapping using Imaging Interferometer data from Chang'E-1显示文摘Information about the variability,and spatial distribution of iron abundance is important to understand lunar geological history and for future resource utilization. In this paper we present a preliminary model to produce an iron abundance map using images taken by an Imaging Interferometer on board the satellite Chang'E-1. Compared with the Clementine UVVIS images,the images from the Chang'E-1 satellite also allowed for the extraction of FeO abundance distributions on the Moon. However,the prelimi-nary model results suggest an underestimation of ~2 wt.% for the FeO content of the mare region and an overestimation of ~3 wt.% for the highland region. | LING ZongCheng ZHANG Jiang LIU JianZhong ZHANG WenXi BIAN Wei REN Xin MU LingLi LIU JianJun LI ChunLai | 2011 | Chinese Science Bulletin2011，56，4： | 15 |
| 2 | Preliminary results of TiO_2 mapping using Imaging Interferometer data from Chang'E-1显示文摘The distribution of titanium abundance on the lunar surface is important knowledge for lunar geologic studies and future resource utilization.In this paper,we develop a preliminary model based on'ground truths'from Apollo and Luna sample-return sites to produce a titanium abundance map from Chang’E-1 Imaging Interferometer(IIM) images.The derived TiO2 abundances are validated with Clementine UVVIS results in several regions,including lunar highlands neighboring the Apollo 16 landing site,and high-Ti and low-Ti maria near the standard site of Mare Serenitatis(MS2) .The validation results show that TiO2 abundances modeled with Chang’E-1 IIM data are overestimated for highlands(~0.7 wt.%) and low-Ti maria(~1.5 wt.%) and underestimated for high-Ti maria(~0.8 wt.%). | LING ZongCheng ZHANG Jiang LIU JianZhong ZHANG WenXi ZHANG GuangLiang LIU Bin REN Xin MU LingLi LIU JianJun LI ChunLai | 2011 | Chinese Science Bulletin2011，56，20： | 10 |
| 3 | Photometric modeling of the Moon using Lommel-Seeliger function and Chang'E-1 IIM data显示文摘The imaging interferometer(IIM)aboard the Chang’E-1 lunar orbiter is the first multispectral imaging spectrometer for Chinese lunar missions.Before science applications(e.g.,FeO and TiO2mapping)of the IIM raw data,the radiance variation due to changes in illumination and viewing geometry has to be removed from the radiometrically calibrated IIM Level 2A images.To achieve this,we fit the IIM Level 2A radiance data with a Lommel-Seeliger photometric model consisting of an exponential term and a fourth order polynomial in the phase function,without distinguishing between lunar maria and highlands.The exponential and the fourth order polynomial parameters are derived separately by fitting to two datasets divided at a solar phase angle threshold,avoiding a decrease in the phase function close to zero phase angle.Different phase angle thresholds result in coincident fitting curves between 20°and 75°,while large discrepancies occur at other phase angles.Then the derived photometric model is used to normalize the IIM Level 2A data to radiance values at an incidence and phase angle of 30°and emission angle of 0°.Our photometric model is validated by comparing two photometrically normalized IIM radiance spectra covering the same areas,showing a relative deviation consistent with the IIM preflight calibration. | ZHANG Jiang LING ZongCheng ZHANG WenXi REN Xin LI ChunLai LIU JianZhong | 2013 | Chinese Science Bulletin2013，58，36： | 3 |
| 4 | Correlation analysis and partial least square modeling to quantify typical minerals with Chang'E-3 visible and near-infrared imaging spectrometer's ground validation data显示文摘In 2013, Chang'E-3 program will develop lunar mineral resources in-situ detection. A Visible and Near-infrared Imaging Spectrometer(VNIS) has been selected as one payload of CE-3 lunar rover to achieve this goal. It is critical and urgent to evaluate VNIS' spectrum data quality and validate quantification methods for mineral composition before its launch. Ground validation experiment of VNIS was carried out to complete the two goals, by simulating CE-3 lunar rover's detection environment on lunar surface in the laboratory. Based on the hyperspectral reflectance data derived, Correlation Analysis and Partial Least Square(CA-PLS) algorithm is applied to predict abundance of four lunar typical minerals(pyroxene, plagioclase, ilmenite and olivine) in their mixture. We firstly selected a set of VNIS' spectral parameters which highly correlated with minerals' abundance by correlation analysis(CA), and then stepwise regression method was used to find out spectral parameters which make the largest contributions to the mineral contents. At last, functions were derived to link minerals' abundance and spectral parameters by partial least square(PLS) algorithm. Not considering the effect of maturity, agglutinate and Fe0, we found that there are wonderful correlations between these four minerals and VNIS' spectral parameters, e.g. the abundance of pyroxene correlates positively with the mixture's absorption depth, the value of absorption depth added as the increasing of pyroxene's abundance. But the abundance of plagioclase correlates negatively with the spectral parameters of band ratio, the value of band ratio would decrease when the abundance of plagioclase increased. Similar to plagioclase, the abundance of ilmenite and olivine has a negative correlation with the mixture's reflectance data, if the abundance of ilmenite or olivine increase, the reflectance values of the mixture will decrease. Through model validation, better estimates of pyroxene, plagioclase and ilmenite's abundances are given. It is concluded that VNIS has the capability to be applied on lunar minerals' identification, and CA-PLS algorithm has the potential to be used on lunar surface's in-situ detection for minerals' abundance prediction. | LIU Bin LIU Jianzhong ZHANG Guangliang LING Zongcheng ZHANG Jiang HE Zhiping YANG Benyong ZOU Yongliao | 2014 | Chinese Journal Of Geochemistry2014，33，1： | 3 |
| 5 | Mineralogy of Chang’e-4 landing site:preliminary results of visible and near-infrared imaging spectrometer显示文摘The exploration of mafic anomaly in South Pole-Aitken(SPA,the largest confirmed)basin on the Moon provides important insights into lunar interior.The landing of Chang’e-4(CE-4)and deployment of Yutu-2 rover on the discontinuous ejecta from Finsen crater enabled in-situ measurements of the unusual mineralogy in the central portion of SPA basin with visible and near-infrared imaging spectrometer(VNIS).Here we present detailed processing procedures based on the level 2B data of CE-4 VNIS and preliminary mineralogical results at the exploration area of Yutu-2 rover.A systematic processing pipeline is developed to derive credible reflectance spectra,based on which several spectral and mineral indices are calculated to constrain the mafic mineralogy.The mafic components in the soils and boulder around CE-4 landing site are concluded as clinopyroxene-bearing with intermediate composition and probably dominated by pigeonite although the possibility of mixing orthopyroxen(OPX)and calcic clinopyroxene(CPX)also exists.These mineralogical results are more consistent with a petrogenesis that the CE-4 regolith and rock fragment are derived from rapid-cooling magmatic systems and we interpret that the materials at the CE-4 landing site ejected from Finsen crater are probably recrystallized from impact melt settings. | Jian CHEN Zongcheng LING Le QIAO Zhiping HE Rui XU Lingzhi SUN Jiang ZHANG Bo LI Xiaohui FU Changqing LIU Xiaobin QI | 2020 | Science China(Information Sciences)2020，63，4： | 2 |
| 6 | Solid-gas carbonate formation during dust events on Mars显示文摘For half a century,Mars missions have gathered abundant geological evidence for a wet,warm climate in the early history of Mars more than 3 billion years ago,including various fluvial landforms and exposed aqueous alteration minerals.It was supposed that Mars once had a dense,CO_(2)-rich atmosphere.However,present-day Mars has a much thinner atmosphere dominated by CO_(2). | Wenshuo Mao Xiaohui Fu Zhongchen Wu Jiang Zhang Zongcheng Ling Yang Liu Yu-Yan Sara Zhao Hitesh G.Changela Yuheng Ni Fabao Yan Yongliao Zou | 2023 | National Science Review2023，10，4： | 0 |
| 7 | Compositions and possible sources of lunar meteorite NWA 4884显示文摘1 Introduction Lunar mare basalts represent the products of partial remelting of deep mantle sources and provide windows into the compositions of lunar interior.Nine Apollo andLuna missions returned large amounts of mare basaltic samples,while remote sensing suggests that sampled basalts may cover only a small number of the lunar | CHEN Jian LING Zongcheng LI Bo SUN Lingzhi ZHANG Jiang HUANG Yihang WU Zhongchen NI Yuheng LIU Jianzhong | 2017 | Acta Geologica Sinica(English Edition)2017，91，S1： | 0 |
| 8 | Lunar absolute reflectance as observed by Chang'E-1 Imaging Interferometer显示文摘Lunar absolute reflectance, which describes the fraction of solar radiation reflected by the Moon, is fundamental for the Chang'E-1 Imaging Interferometer(IIM) to map lunar mineralogical and elemental distributions. Recent observations made by the Spectral Irradiance Monitor(SIM) onboard the Solar Radiation and Climate Experiment(SORCE) spacecraft indicate that temporal variation in the solar radiation might have non-negligible influence on reflectance calculation, and the SIM measurements are different from the two previously used solar irradiances, i.e., ATLAS3 and Newkur. To provide reliable science results, we examined solar irradiance variability with the SIM daily observations, derived lunar absolute reflectances from the IIM 2A radiance with the SIM, ATLAS3 and Newkur data, and compared them with the Chandrayaan-1 Moon Mineralogy Mapper(M3), the Robotic Lunar Observatory(ROLO) and the Kaguya Multispectral Imager(MI) results. The temporal variability of the SIM solar irradiance is 0.25%–1.1% in the IIM spectral range, and less than 0.2% during the IIM observations. Nevertheless, the differences between the SIM measurements and the ATLAS3 and Newkur data can respectively rise up to 8% and 5% at particular IIM bands, resulting in discrepancy between which might affect compositional mapping. The IIM absolute reflectance we derived for the Moon using the SIM data, except for the last two bands, is consistent with the ROLO and the MI observations, although it is lower. | ZHANG Jiang LING ZongCheng LIU JianZhong WU ZhongChen LI Bo NI YuHeng | 2015 | Science China(Physics,Mechanics & Astronomy)2015，58，8： | 0 |
| 9 | A lunar time scale from the perspective of the Moon’s dynamic evolution显示文摘A geologic time scale is a chronological system that separates the geological strata of a planetary body into different units in temporal sequence and shows its progressive evolution.The time scale of the Moon was established a half-century ago during the telescopic-early Apollo exploration era,using data with limited spatial coverage and resolution.The past decades have seen a wide array of studies,which have significantly extended our understanding of global lunar geologic evolution.Based on a comprehensive review of lunar evolution with respect to the dynamical changes,we propose two major updates to the current lunar time scale paradigm to include the evolution of both endogenic and exogenic dynamic forces now known to have influenced early lunar history.Firstly,based on the temporal interplay of exogenic and endogenic processes in altering the Moon,we defined three Eon/Eonothem-level units to represent three dynamical evolutionary phases.Secondly,the pre-Nectarian System is redefined and divided as the magma ocean-era Magma-oceanian System and the following Aitkenian System beginning with the South Pole-Aitken basin.The ejecta of this basin,Das Formation,was deposited on the primordial lunar crust as the oldest stratum produced from exogenic processes.The updated lunar time scale,facilitated by the post-Apollo exploration and research advances,provides an integrated framework to depict the evolution of the Moon and has important implications for the geologic study of other terrestrial planets. | Dijun GUO Jianzhong LIU James WHEAD Fuqin ZHANG Zongcheng LING Shengbo CHEN Jianping CHEN Xiaozhong DING Jinzhu JI Ziyuan OUYANG | 2024 | Science China Earth Sciences2024，67，1： | 0 |
您所在的机构暂未开通此部分的功能，请联系管理员