共查询到18条相似文献，搜索用时 125 毫秒
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模拟月壤是与月球月壤具有相似的矿物组成、化学成分和物理力学性质的地球物质,是月球样品的地球化学复制品.长白山龙岗火山群金龙顶子火山喷发的四海火山渣具有与阿波罗14号采集的月球样品相似的化学和矿物组成,并含有20%～40 %的玻璃物质.以四海火山渣为初始物质,研制成功CAS-1模拟月壤,并测量了CAS-1模拟月壤的主量和微量元素组成、矿物组成、密度、颗粒形态、粒度分布、抗剪性和复介电常数等参数.结果表明,CAS-1模拟月壤与Apollo 14号采集的月球样品具有相似的化学成分、矿物组成和物理力学性质,是一种理想的低钛玄武岩质模拟月壤. 相似文献
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雨海盆地是月球上研究程度最高的多环结构盆地,月球上古老的和年轻的玄武岩在盆地中均有分布,因此雨海是研究月海玄武岩岩浆活动的理想区域。为了更合理的厘定雨海地区的玄武质岩浆演化历史,本文主要结合岩石学、年代学等工作对本区玄武岩的充填期次进行重新划分。利用嫦娥一号IIM光谱数据进行岩石类型分布图编制,初步划分了5类不同钛含量的月海玄武岩;基于高分辨率100m LRO宽视角影像数据通过撞击坑尺寸-频率定年法(CSFD)对本区玄武岩单元模式年龄进行厘定,共划分35个玄武岩单元,发现本区在3.49~2.23Ga均有玄武质岩浆充填活动,具有多期次性。在建立不同类别玄武岩、形貌特征与模式年龄的对应关系基础上,将玄武岩充填划分为4个期次:极低钛玄武岩(3.49~3.20Ga)、低钛玄武岩(3.29~2.83Ga)、中钛玄武岩(3.13~2.52Ga)、(极)高钛玄武岩(2.92~2.23Ga)。本区地形地貌高程特征与不同表面年龄的玄武岩单元之间总体上呈现出一定的负相关性。因此在本区玄武质岩浆期次划分考虑上,不仅要考虑玄武岩的成分特征,更要考虑结合与玄武岩演化密切相关的年代学及形貌学特征,利用形貌、成分数据和年代学信息来共同约束玄武质岩浆期次划分及演化历史。 相似文献
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前人对峨眉山玄武岩的研究已经取得大量的研究成果,但对于一些关键科学问题如岩浆源区组成、源区温压条件等还存在分歧,或有待进一步探讨。本文报道了四川木里地区二叠纪苦橄岩和相关玄武岩的岩石学、地球化学和Sr-Nd同位素特征,并进一步探讨了苦橄岩和相关玄武岩的岩浆源区性质、岩浆形成条件。研究表明:四川木里地区二叠纪火成岩主要岩石类型为苦橄岩、高钛玄武岩和低钛玄武岩;苦橄质岩浆来源于地幔柱头部中心的高温区域(地幔柱轴部),岩浆主要起源于石榴石稳定域;高钛和低钛玄武质岩浆来源于地幔柱尾部,高钛玄武质岩浆主要起源于石榴石稳定域,而低钛玄武质岩浆起源于石榴石稳定域和尖晶石稳定域的过渡带;苦橄质和玄武质岩浆在上升过程中都不同程度混染了大陆岩石圈地幔物质,其中低钛玄武质岩浆可能有少量地壳物质的混染。 相似文献
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用于月面车辆力学试验的模拟月壤研究 总被引：9，自引：1，他引：8
研究月面环境下的车辆地面力学,对保证月球探测车辆的正常工作具有重要意义,而用于月面车辆力学试验的模拟月壤则影响其结果的准确度与可信度。用于月面车辆力学试验的模拟月壤,以月壤样本与JSC-1模拟月壤为参考标准,以吉林辉南县火山灰为主要原料、赤铁矿砂为辅料,通过调整试样的粒径分布与赤铁矿砂含量,使模拟月壤的比重、内摩擦角、凝聚力、承压特性、粒径分布、颗粒形态、矿物组成等参数接近JSC-1模拟月壤,并在月壤样本的参数变化范围之内,表明该模拟月壤可用于月面车辆力学试验研究。 相似文献
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新化高桥玄武质富钛古火山岩研究 总被引：1，自引：0，他引：1
高桥玄武质火山岩是一个化学成分独特的富钛基性火山岩。属震旦纪海底喷发的拉斑玄武岩,化学成分以富含TiO_2、MgO、Fe_2O_3+FeO特征。本文通过多方论证后指出:伴生的变辉绿岩属火山颈相,Ti的富集是蚀变作用的结果。 相似文献
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LI Yongquan LIU Jianzhong ZOU Yongliao OUYANG Ziyuan ZHENG Yongchun YUE Zongyu 《《地质学报》英文版》2011,85(5):1016-1021
Two new lunar mare soil simulants, NAO-2 and NAO-3, have been created in National Astronomical Observatories (NAO), Chinese Academy of Sciences. These two simulants were produced from low-titanium basalt and high-titanium basalt respectively. The chemical composition, mineralogy, particle size distribution, density, angle of internal friction, and cohesion of both simulants have been analyzed, indicating that some characteristics of NAO-2 and NAO-3 are similar to those of Apollo 14 and Apollo 11 landing site soils. NAO-2 and NAO-3 will be of great benefit to the scientific and engineering research on lunar soil. 相似文献
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L.J. Hallis M. Anand R.C. Greenwood I.A. Franchi 《Geochimica et cosmochimica acta》2010,74(23):6885-6899
To investigate the formation and early evolution of the lunar mantle and crust we have analysed the oxygen isotopic composition, titanium content and modal mineralogy of a suite of lunar basalts. Our sample set included eight low-Ti basalts from the Apollo 12 and 15 collections, and 12 high-Ti basalts from Apollo 11 and 17 collections. In addition, we have determined the oxygen isotopic composition of an Apollo 15 KREEP (K - potassium, REE - Rare Earth Element, and P - phosphorus) basalt (sample 15386) and an Apollo 14 feldspathic mare basalt (sample 14053). Our data display a continuum in bulk-rock δ18O values, from relatively low values in the most Ti-rich samples to higher values in the Ti-poor samples, with the Apollo 11 sample suite partially bridging the gap. Calculation of bulk-rock δ18O values, using a combination of previously published oxygen isotope data on mineral separates from lunar basalts, and modal mineralogy (determined in this study), match with the measured bulk-rock δ18O values. This demonstrates that differences in mineral modal assemblage produce differences in mare basalt δ18O bulk-rock values. Differences between the low- and high-Ti mare basalts appear to be largely a reflection of mantle-source heterogeneities, and in particular, the highly variable distribution of ilmenite within the lunar mantle. Bulk δ18O variation in mare basalts is also controlled by fractional crystallisation of a few key mineral phases. Thus, ilmenite fractionation is important in the case of high-Ti Apollo 17 samples, whereas olivine plays a more dominant role for the low-Ti Apollo 12 samples.Consistent with the results of previous studies, our data reveal no detectable difference between the Δ17O of the Earth and Moon. The fact that oxygen three-isotope studies have been unable to detect a measurable difference at such high precisions reinforces doubts about the giant impact hypothesis as presently formulated. 相似文献
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The basalt target rocks that have been converted to regolithacross the lunar maria are everywhere more feldspathic and lessmafic than the basalt hand specimens recovered from four Apollolanding sites, an effect not due to either horizontal or verticalmixing with adjacent highland materials. These crushed targetrocks need to be characterized by direct chemical and petrographicanalysis of the lithic fragments of basalt in the regolithsand by determination of the phase equilibria in and adjacentto these compositions at low pressure. Such data are availablefor the basalts of Mare Crisium and Mare Nubium (Luna 16, 24)and for Very Low Titanium basalt, first defined by three lithicfragments from the Apollo 17 core. These are all feldspathicbasalts, as are those from the Mare Tranquillitatis and OceanusProcellarum soils (Apollo 11, 12). Such data are lacking forthe principal basalt components at Mare Imbrium and Mare Serenitatis(Apollo 15, 17). The thoroughly investigated Apollo 17 landingsite at Taurus–Littrow, SE Mare Serenitatis, providesan example where other published information may be used toarrive at estimates of the composition of the feldspathic marebasalt that was the principal target material for regolith formation.This crushed basalt composition is that of a liquid close tobeing in simultaneous equilibrium with all of olivine, plagioclase,calcium-rich pyroxene, spinel, armalcolite and ilmenite at lowpressure. The simplest explanation would be that the basaltthat dominated the formation of the regolith comes from a differentflow unit than the hand specimens, but it strains credulitythat not a single hand specimen can be positively assigned tothat upper unit, and not a single soil sample can be positivelyidentified as having formed principally from the unit that providesthe hand specimens. KEY WORDS: cotectic; lithic fragment; lunar; target rock; regolith 相似文献
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The manned Apollo 11, 12, 14 and 15 and the automated Luna 16 lunar missions have provided us with lunar rock and regolith (soil) samples from a number of geologically distinct sites. The mare regions were sampled by Apollo 11, 12 and Luna 16, whereas Apollo 14 landed on a terrain with more relief, the Fra Mauro Formation which represents an ejecta blanket from the Imbrian Basin, and Apollo 15 touched down near the lunar highlands. The samples collected consist of a mixture, mainly of basalt, breccia and regolith (soil-particulate matter, generally < 1 cm in size). The basalts show considerable variation in texture, mineralogy and chemistry and probably represent fragments from various parts of relatively thin and extensive lava flows in the maria. The breccias represent regolith material which was indurated to varying degrees by impact events. The regolith is a product of the breakdown, again by impact, of coherent rock masses of basalt and breccia. 相似文献
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Mitsunobu Tatsumoto 《Geochimica et cosmochimica acta》1973,37(4):1079-1086
The concentrations of uranium, thorium and lead and the lead isotopic composition of Luna 20 soil were determined. The data indicate that the Luna 20 soil is mainly a mixture of highland anorthosites and low-K basalt, but little KREEP basalt. The U-Th-Pb systematics are discussed in comparison with other lunar soils, especially with Apollo 16 soils which were collected from a ‘typical’ highland region. The data fit well in the Apollo 16 soil array on a U-Pb evolution diagram, and they exhibit excess lead relative to uranium. This relationship appears to be a characteristic of highland localities. Considering the previous observations of lunar samples, we infer that lead enrichment in the soil relative to uranium occurred between 3.2 and 3.9 b.y. ago and that the soil was disturbed by ‘third events’ about 2.0 b.y. ago. A lunar evolution model is discussed. 相似文献
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中国嫦娥工程三期将进行月球样品的采集与返回,这是继美国Apollo和前苏联Luna之后,国际上最新的月球样品返回计划。月球样品的存储与管理方法将成为中国探月工程中亟待解决的重要问题之一。特别是如何最大程度地保持月球样品的科学研究价值,避免或减少可能的样品污染等问题,不仅为工程部门所关心,也是月球科学家所极为关注的问题。文中主要回顾和总结了美国Apollo月球样品的处理与保存方法,包括月球样品实验室简况、月球样品初步处理方法、月球样品初步测试分析及相关实验简介和月球样品的保存方法等内容,以期为中国月球样品的返回和地面存储提供有益的借鉴。 相似文献
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Highly radiogenic Pb isotope compositions determined for volcanic glass beads from the Apollo 14 soil sample 14163 are similar to those commonly determined for mare basalts and are correlated with chemical variations observed in the beads. This indicates that Pb unsupported by in-situ U decay has a similar origin in both glass beads and mare basalt samples and is likely to reflect variations of 238U/204Pb (μ) in the lunar mantle. An alternative explanation that this Pb is a result of late equilibration with the radiogenic Pb present in soil is less likely as it would imply that all other characteristics of glass beads such as their chemistry must also be a consequence of equilibration near the lunar surface. Regardless of the origin of unsupported Pb, observed variations of Pb isotope compositions in the glass beads and mare basalts appear to be a result of two component mixing between a primitive reservoir with a μ-value similar to the Earth’s mantle and KREEP with a μ-value in excess of several thousand. This range cannot be explained by the fractionation of major rock forming minerals from the crystallising Lunar Magma Ocean and instead requires substantial extraction of sulphide late in the crystallisation sequence. The proportion of sulphide required to produce the inferred range places limits on the starting μ of the Moon prior to differentiation, demanding a relatively high value of about 100-200. Low μ indicated by several basalt samples and previously analysed volcanic glass beads can be explained by the preservation of an early (but post Ferroan Anorthosite) sulphide rich reservoir in the lunar mantle, while a complete range of Pb isotope compositions observed in the glass beads and mare basalts can be interpreted as mixing between this sulphide rich reservoir and KREEP. 相似文献
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ZHANG Xiaoyu LI Chunlai L Chang Graduate University of Chinese Academy of Sciences Beijing China National Astronomical Observatories Chinese Academy of Sciences Beijing China 《中国地球化学学报》2009,28(2):204-211
In the second phase of the Chang’E Program an unmanned lunar rover will be launched onto the Moon. When ground scientists
get a full understanding of the chemical composition of lunar soil around the rover, they can make more detailed survey plans
for the rover and various payloads onboard so as to satisfy their scientific objectives. There is an obvious relationship
between the reflectance of lunar soil and its chemical characteristics. Both principal component analysis (PCA) and support
vector machine (SVM) models were applied to establishing the relationship between the reflectance spectra and chemical compositions
of lunar highland and mare soil samples sent back by Apollo missions 11, 12, 14, 15, 16 and 17 and measured by Lunar Soil
Characterization Consortium (LSCC). PCA was used to reduce and select the features of the reflectance spectra of lunar soil
samples. Then, these features were put into SVM to estimate the abundances of various chemical components in lunar soil. We
also compared the results of our measurement with those obtained by the SVM model [partial least squares (PLS)] and the principal
component regression (PCR) model reported in literature. Our studies showed that with the exception of TiO2, the results of prediction of the abundances of chemical compounds in lunar soil by our model are much more reliable than
those reported in literature. The reflectance spectra of lunar soil are closely related to the materials from which it was
derived. 相似文献