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1.
不同粒径的月球橄榄石二向性反射特征研究 总被引：1，自引：0，他引：1
研究月表矿物组成和分布,对于探测月表地质构造以及月球的起源和演化具有重要的意义。因此,物质成分探测一直是月球研究的重点课题之一。尽管人类已经能够从月球采集样品进行实验室分析,但遥感技术仍然是研究月球的主要手段。文中主要目的是模拟不同粒径下橄榄石的二向性反射特征。为此,首先提出模拟不同粒径下反射特征的方法,然后利用Hapke模型和Mie散射理论对不同粒径下富铁和富镁橄榄石的二向性反射特征进行了模拟。模拟结果显示,富镁橄榄石的二向性反射率较富铁橄榄石的反射率高。最后,分析了反射率差值和等效粒径的相关性。该结论为选择探月传感器的波段组合、识别橄榄石镁铁含量提供了理论依据,也为应用遥感数据的橄榄石的判别奠定了基础。 相似文献
2.
月表矿物含量反演是研究月球地质起源和演化的关键.太空风化作用普遍发生在月球表面,对矿物纯净光谱造成了不可忽视的影响,它弱化光谱吸收特征, 降低反射率,影响矿物含量遥感反演精度.基于Relab光谱库和Hapke辐射传输模型,将月表 4种矿物(单斜辉石、斜方辉石、斜长石、橄榄石)的二向性反射率转换成同向性的单次散射反照率,然后计算矿物的光学常数;再根据亚微观金属铁SMFe(submicroscopic metallic iron)的质量分数模拟6种不同程度太空风化效应,得到端元矿物的反射率光谱;最后基于上述方法,利用多端元线性分解方法和M3(moon mineralogy mapper,月球矿物绘图仪)高光谱数据反演不同风化程度下的矿物含量,得到月表虹湾地区辉石、斜长石、橄榄石3种矿物的含量分布.实验表明,利用多端元线性分解可以有效模拟太空风化效应对矿物光谱的影响,是研究太空风化效应影响下矿物识别及含量反演的一种行之有效的方法. 相似文献
3.
月壤厚度反演是我国月球探测的重要科学目标之一,其重要影响因素之一就是月球表面的有效反射率.前人在月壤厚度反演研究中使用了光滑月表反射率模型,使得月表水平极化反射率和水平极化反射率分别为0.063和0.028(观测角:30°).然而,月球表面是非常粗糙的,必须建立适合粗糙月球表面的有效反射率模型.因此,以嫦娥一号卫星微波辐射计数据的空间分辨率(3 GHz通道,56 km×56 km)为标准,利用每个微波辐射计像元范围内的激光高度计数据(8×8个)建立相应的粗糙月表模型.然后,基于Q/H模型,进行月球表面的有效反射率研究,生成了观测角为30°时月球表面水平极化有效反射率和垂直极化有效反射率分布图.结果表明,月球表面的粗糙性对月表反射率影响很大,使得水平极化反射率降低,局部地区降至0.050;垂直极化反射率增加,局部地区可达0.040,增幅达40%. 相似文献
4.
月表光度行为描述了月表物质反射的太阳光随入射、出射和太阳相角的变化,其反射率的不同取决于月壤颗粒大小、粒子形状、透明度、孔隙度、表面粗糙度等因素。为了分析月表光度行为,了解区域反射率差异原因,本文以Apollo16登月区为例,使用M3（moon mineralogy mapper）数据反演Hapke模型物理参数,并分析了Hapke模型光度参数对二向性反射率的影响程度。反演结果显示,本文研究区域光度参数b、hS变化很小,光度参数w有一定的变化;表明本文研究区域反射率不同主要是w的差异造成的。研究区域月壤中各类矿物颗粒的前向散射占主导地位,月壤结构和粒径总体相近,但在孔隙度、风化层填充物状态及表面粗糙度等因素中至少有一种因素存在差异。 相似文献
5.
研究识别嫦娥五号返回月壤样品颗粒的类型、含量、形貌、结构和成分特征,可为嫦娥五号着陆区月壤的成因与月球表面演化过程提供关键科学依据.利用扫描电镜-能谱仪、矿物自动定量分析系统和显微激光拉曼光谱仪对嫦娥五号表取月壤样品CE5C0400（YJFM00403）进行了系统研究,发现月壤颗粒组成多样,包括斜长石、单斜辉石和橄榄石等矿物、玄武岩碎屑、黏结物和玻璃球.颗粒表面和内部微观结构复杂,呈现各种破碎、表面附着堆积、微撞击坑、溅射物等形式的微米-纳米级的形貌特征.嫦娥五号月壤的微形貌特征记录了以微陨石撞击为主导的复杂太空风化过程:一方面反复的撞击作用使月壤颗粒破碎、粒度变细,另一方面撞击引发的局部熔融又使颗粒发生胶结,同时伴随含铁矿物分解形成微-纳米级单质铁颗粒.上述过程反复进行,导致月壤颗粒大小和物相组成复杂多变. 相似文献
6.
中红外光谱在月球探测中的应用 总被引：1，自引：0，他引：1
硅酸盐矿物的中红外光谱一般具有明显的CF特征和Reststrahlen吸收带,这些特征都与硅酸盐的组成密切相关,可以作为判别其组成的指示特征。月球表面的主要矿物有辉石、斜长石、钛铁矿和橄榄石,其中除了钛铁矿以外,都属于硅酸盐的范畴。如果充分利用月球表面硅酸盐的红外光谱特征,即CF特征和Reststrahlen吸收带,将可以用于探测VIS-NIR光谱无法完成的探测目标:钙长石、橄榄石、石英和碱性长石等。如果在嫦娥工程的后续探测器(如轨道器、月球车或者软着陆平台)上搭载中红外光谱仪对月表物质进行探测,将有利于成功实现对月球表面的矿物和岩石的精确探测,这也将是我国首次采用中红外光谱探测仪对月球进行系统的矿物与岩石探测。 相似文献
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8.
由于月球采样点较少,月壤真实数据稀缺,限制了对月球科学问题的进一步研究。较全面系统地采集月壤样品在近期很难完成,开展月壤光谱模拟工作是月壤实测光谱的必要有益补充,可以为研究月壤光谱特征提供大量数据。基于Hapke模型,我们选取RELAB光谱库的斜长石、单斜辉石、斜方辉石、橄榄石、单质铁、钛铁矿、火山玻璃、熔融玻璃等典型月壤矿物,运用牛顿插值和最小二乘优化的方法,模拟了LSCC月壤数据的一定粒径、单质铁含量、观测条件及矿物混合比例下的混合光谱。模拟光谱与实测光谱拟合较好,相关系数均大于0.99,均方根误差在10-3数量级;模拟矿物丰度与实测矿物丰度基本一致;模拟SMFe含量与相对成熟度指数Is/FeO线性关系明显;模拟粒径基本落在实测粒径组范围内。最后,文中讨论了光谱吸收中心波长、吸收面积等光谱特征参数的模拟精度,以及高精度模拟光谱时光学常数的计算方法。 相似文献
9.
月面环境与月壤特性研究的主要问题探讨 总被引：6，自引：0，他引：6
月面环境与月壤特性是月球探测和月球科学研究的重要基础,对它们的研究一直在不断加深,本文对月球表面地形地貌、热环境以及月壤特性三个方面的研究现状进行了总结,初步分析了这三个方面研究目前存在的一些主要问题：（1）地形地貌对月球定量遥感的影响以及南极艾特肯（SPA）盆地等地貌单元的年代学划分和成因演化;（2）月面热辐射、月表物理温度和热流等月面热环境特征的进一步探测和全面分析,以及其对地球反照率变化的响应;（3）月壤形成演化过程及空间风化作用,月球极区氢富集机制和水冰探测,以及月球资源开发利用。 相似文献
10.
首次对东昆仓复合造山带不同时代蛇绿岩主要造岩矿物橄槛石、辉石、斜长石进行了的矿物化学研究查明了不同蛇绿岩带在矿物成分上的差异,对清水泉蛇绿岩带和布青山蛇绿岩单辉石、斜方辉石、斜长石进行了矿物稀土、微量元素的研究,阐明了矿物稀土、微量元素与全岩稀土、微量元素的关系,证明了在以辉石为主的橄辉岩中珠稀土元素基本上代表了全岩的稀土元素。根据地幔岩石中矿物成分特征,对不同蛇绿岩带地幔类型进行了讨论,并根据实 相似文献
11.
LIU Bin LIU Jianzhong ZHANG Guangliang LING Zongcheng ZHANG Jiang HE Zhiping YANG Benyong ZOU Yongliao 《中国地球化学学报》2014,33(1):86-94
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 contri- butions 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 Fe~, 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 in- creasing of pyroxene＇s abundance. But the abundance of plagioclase correlates negatively with the spectral parame- ters 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. 相似文献
12.
The spectral reflectance features of rocks and minerals are correlated with their composition,col-or,grain size and surface state.Different wall rocks,altered rocks and ores have their spectral reflectance features,which are very helpful for the explanation of remote sensing data and searching for mineral deposits by remote sensing.After the treatment of spectrum data and searching for mineral deposits by remote sensing.After the treatment of spectrum data of rocks and ores and physical and chemical parameters in the mathematical statistics,we analyzed the laboratorial spectrum dataand put forward better wave bands(520-590,650-710,730-760,770-860,1560-1760,2200 and 2300-2400nm) for distinguishing rocks and ores. 相似文献
13.
WANG Xiang CHEN Jianping XU Yanbo ZHENG Yongchun YAN Bokun WU Yunzhao 《《地质学报》英文版》2015,89(6):1882-1894
Spectra are sensitive in detecting main minerals on the lunar surface from visible light to infrared light. Since spectral characteristics of minerals are closely related to their compositions and the maturity level of soil on the Moon, studying the compositions and distribution of elements and minerals on the lunar surface can help to understand the evolution of the Moon through remote sensing technology. The correlation between the spectral characteristics of Chang’e-1 interference imaging spectrometry (IIM) reflectance images and the mineral contents of LSCC (Lunar Soil Characterization Consortium) lunar surface mineral samples was discussed and the spatial distributions of FeO and Al2O3 contained in both pyroxene and plagioclase on LQ-4 were studied using the improved angle parameter method, MNF, and band ratio statistics. A comparison of the mapping results of the optical models by Lucey, Shkuractov and other researchers on Clementine and the gamma ray spectrometry data shows that the content error is within 0.6% for lunar mare areas and close to 1% for the highland areas. The tectonic framework on the lunar surface was also investigated. And based on integrated analysis of previous findings on topography of the lunar surface, Chang’e LAM, CCD and LOLA images and the gravity anomalies data (Clementine GLGM-2), the tectonic unit subdivision was established for LQ-4, the idea of subdividing the lunar tectonic units was proposed, and this will provide a good foundation for studying the lunar tectonic evolution. 相似文献
14.
Condensate objects observed in the lunar regolith are distinctly separated on the basis of morpho-logical and chemical characteristics
into droplets condensed during the expansion of an impact-generated vapor cloud and films condensed on the relatively cold
surface of mineral particles. Using the analyses of both condensate forms and experimental data on the evaporation of melt
corresponding to a typical lunar highland rock of the gabbro-anorthosite composition from Apollo 16 sample 68415.40, the temperature
conditions of vapor condensation during lunar impact events were estimated. The comparison of condensate compositions with
the analyses of vapors from the evaporation experiment showed that, compared with the compositions of droplet-type condensates,
the condensate rims were formed from a vapor with high contents of refractory CaO and Al2O3 and at very different condensation temperatures. The enrichment of vapor in CaO and Al2O3 could be attained only at high temperatures of melt evaporation (higher than ∼ 1850°C according to experimental data). The
estimated condensation temperatures of droplets are significantly lower, ∼1750–1500°C. Rim-type condensates were produced
by vapor quenching on the relatively cold surface of a solid mineral particle, which resulted in almost complete precipitation
of all major components of the silicate vapor without fractionation in accordance with their individual volatilities. 相似文献
15.
Mineral forms of iron oxide, such as hematite, goethite and jarosite, are important because they are widely distributed at the Earth’s surface and because they are used as indicators for mineral exploration. Iron oxide abundance in rocks containing these minerals can be estimated from the absorption depth at wavelengths of around 900 nm in a reflectance spectrum, but this depth is also affected by extraneous factors such as grain size and topography. This paper investigated the effect of grain size on reflectance spectra and proposed a method for estimating iron oxide abundance in surface rocks by using remotely sensed data with suppression of the effects of grain size and topography. Reflectance spectra were measured in a laboratory from rock powder samples of different grain sizes containing iron oxide minerals. While the reflectance increased with decreasing grain size, the presence of ferric iron caused the absorption depth to be almost constant at around 900 nm, irrespective of the chemical composition of the sample. In addition, the difference between the reflectance at 550 nm and 760 nm (Slope) was a function of grain size. Iron oxide abundance can be estimated accurately by MCR-900D, which is the maximum absorption depth at the absorption center after the effect of grain size and topography was suppressed by Slope and the continuum-removal method, which takes the ratio between the original spectrum and its continuum, respectively. Correlation of MCR-900D results with datasets of actual spectral and chemical iron oxide laboratory measurements revealed that the mineral forms also need to be considered. MCR-900D results were significantly correlated with rock samples classified as containing different forms of iron oxide minerals (hematite, goethite and jarosite). Finally, MCR-900D was applied to an AVIRIS dataset for the Cuprite site in Nevada, USA. The results represented the enrichment zones of iron oxide within hydrothermally altered areas. 相似文献
16.
Metamorphic and Thermal History of a Fore-Arc Basin: the Fossil Bluff Group, Alexander Island, Antarctica 总被引：2，自引：0，他引：2
The Himalia Ridge Formation (Fossil Bluff Group), AlexanderIsland is a 2·2-km-thick sequence of Upper Jurassic–LowerCretaceous conglomerates, sandstones and mudstones, derivedfrom an andesitic volcanic arc and deposited in a fore-arc basin.The metamorphic and thermal history of the formation has beendetermined using authigenic mineral assemblages and vitrinitereflectance measurements. Metamorphic effects include compaction,pore-space reduction, cementation and dissolution and replacementof detrital grains by clay minerals (smectite, illite/smectite,corrensite and kaolinite), calcite, chlorite, laumontite, prehnite,pumpellyite, albite and mica, with less common quartz, haematite,pyrite and epidote. The authigenic mineral assemblages exhibita depth-dependence, and laumontite and calcite exhibit a strongantipathetic relationship. Detrital organic matter in the argillaceouslayers has vitrinite reflectance values (Ro) ranging from 2·3to 3·7%. This indicates considerable thermal maturation,with a systematic increase in reflectivity with increasing depth.There is good correlation of metamorphic mineral assemblageswith chlorite crystallinity and vitrinite reflectance values—allindicating temperatures in the range of 140 ± 20°Cat the top of the sequence to 250 ± 10°C at the baseof the sequence. The temperatures suggest a geothermal gradientof 36–64°C/km and a most likely gradient of 50°C/km.It is suggested that this higher-than-average gradient for afore-arc basin resulted either from rifting during basin formationor from a late-stage arc migration event. KEY WORDS: Antarctica; diagenesis; fore-arc basin; low-temperature metamorphism; vitrinite reflectance 相似文献