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火星快车OMEGA高光谱探测矿物组成的新进展 总被引：1，自引：0，他引：1
主要介绍"火星快车(Mars Express)"搭载的"可见光及红外矿物制图光谱仪(OMEGA)"及其采集数据的特点、大气校正方法和矿物识别研究的新进展."经验传输函数法"(ETF)是目前O-MEGA数据大气校正普遍采用的方法.OMEGA数据已经成功揭示了火星表面矿物和组成的多样性和复杂性.OMEGA检测到与水蚀变相关的层状硅酸盐矿物绿脱石、绿泥石和蒙脱石等主要分布于古老的诺亚期的露头上,这些层状硅酸盐矿物可能是火成岩矿物长期持续与液态水系统作用的结果.含水硫酸盐类矿物石膏、水镁矾和多水硫酸盐等水合化学沉积矿物在亮色调层状地层区的发现,表明火星表面有大量与水作用相关的蒸发盐的存在.火星表面缓慢风化形成的无水铁氧化物主要分布于北半球铁镁质含量低的低地(lowland)地区.OMEGA可以识别辉石和橄榄石,能够区分高钙辉石和低钙辉石.高钙辉石主要分布于Hesperian期的低反照率的火山岩分布地区、黑色沙丘和撞击坑喷射物分布区;低钙辉石主要分布于老的诺亚期的亮色调露头分布区.OMEGA在反照率变化大的极地冰盖地区可以识别水冰和CO2冰.水冰主要利用1.08 μm、1.25 μm、1.51μm和2.0μm特征吸收波段来识别.水冰各吸收特征波段的吸收强度与水冰的粒度呈正相关.CO2冰主要利用1.43 μm、2.0 μm和2.6 μm特征吸收波段来识别. 相似文献
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C.WEIHS Mathematical Applications Information Services R-.Z. CIBA-GEIGY Ltd. CH- Basel Switzerland 《地理学报(英文版)》1993,(5)
Exploratory data analysis(EDA)is a toolbox of data manipulation methods for looking at data to seewhat they seem to say,i.e.one tries to let the data speak for themselves.In this way there is hope thatthe data will lead to indications about'models'of relationships not expected a priori.In this respect EDAis a pre-step to confirmatory data analysis which delivers measures of how adequate a model is.In thistutorial the focus is on multivariate exploratory data analysis for quantitative data using linear methodsfor dimension reduction and prediction.Purely graphical multivariate tools such as 3D rotation andscatterplot matrices are discussed after having introduced the univariate and bivariate tools on which theyare based.The main tasks of multivariate exploratory data analysis are identified as'search for structure'by dimension reduction and'model selection'by comparing predictive power.Resampling is used tosupport validity,and variables selection to improve interpretability. 相似文献
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本文讨论了一种模糊度估算的优化方法－OMEGA(Opgimal method for estimating GPS ambiguities）方法。该方法基于经典的最小二乘搜索过程，首先通过对改化后观测向量的估算，达到了收缩模糊度搜索空间，加快模糊度正确性验证之目的；然后进行矩阵分解，改进了模糊度残差二次型的计算方法，加快模糊度搜索速度。实算结果表明，该方法较一般最小二乘过程效率提高了60％。 相似文献
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R. Melchiorri P. Drossart B. Bézard A. Gendrin N. Manaud 《Planetary and Space Science》2006,54(8):774-783
Spectral images of Mars obtained by the Mars Express/OMEGA experiment in the near infrared are the result of a complex combination of atmospheric, aerosol and ground features. Retrieving the atmospheric information from the data is important, not only to decorrelate mineralogical against atmospheric features, but also to retrieve the atmospheric variability. Once the illumination conditions have been taken into account, the main source of variation on the CO2 absorption is due to the altitude of the surface, which governs atmospheric pressure variation by more than an order of magnitude between the summit of Olympus Mons down to the bottom of Valles Marineris. In this article we present a simplified atmospheric spectral model without scattering, specially developed for the OMEGA observations, which is used to retrieve the local topography through the analysis of the CO2 band. OMEGA atmospheric observations increase the horizontal resolution compared to MOLA altimetry measurements, and therefore complement the mineralogical studies from the same instrument. Finally, residual variations of the pressure can be related to atmospheric structure variation. 相似文献
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