Multiple emission angle surface-atmosphere separations of thermal emission spectrometer data

A method for separating the spectral signatures of the Martian surface and atmosphere was developed and is applied to multiple emission angle data returned from the MGS TES instrument. This method includes correlated-k and index gas removal algorithms that may be applied to all nadir-pointing TES data. Initial results have provided new and refined measurements of the spectral shapes of atmospheric dust and the Martian surface. Surface temperatures and atmospheric dust opacities are also retrieved with improved accuracy over single observation temperature and opacity retrievals. Low-albedo surfaces display absorptions consistent in both shape and depth with previous studies. These surfaces may be closely modeled using a combination of previously derived basalt, andesitic, and high-albedo surface spectral shapes. Short wavelengths display no significant absorptions, indicating both the coarse particulate nature of the surface and the lack of significant amounts of carbonate. Moderate- and high-albedo surfaces have spectral shapes distinctive of fine particulate silicate materials. No single material can match the entire high-albedo surface spectrum, though there are clear indications of a material that closely matches intermediate to calcic plagioclase and an emission peak at ∼1620 cm⁻¹ due to bound water. The lack of residual restrahlen silicate absorptions indicates that minerals such as olivine or pyroxene are not present in high-albedo surfaces at significant (but unknown) abundances. High-albedo surface results presented here are in agreement with and complementary to shorter wavelength observations. The Martian dust is composed of both primary and secondary minerals. Either chemical weathering has not completely altered its source material or the soil is a mixture of altered and unaltered sources. Further laboratory studies are needed to better establish detection limits and behavior of mineral mixtures of fine particulates in the thermal infrared portion of the spectrum.     

Extensive hydrated silica materials in western Hellas Basin,Mars

Near-infrared spectral data indicate the presence of hydrated, poorly crystalline silica where high bulk silica contents have been previously identified in Hellas Basin. No other aqueous phases are identified in these regions and the deposits may be nearly pure. The silica-bearing surfaces are sporadically exposed along a 650 km stretch of the western basin rim within a limited elevation range and display a variety of surface textures suggesting that the materials have been reworked, but not transported large distances. The high abundances and lack of associated aqueous phases indicate that high water to rock ratios were present in the region during the Noachian period but without elevated temperatures or for durations necessary for quartz diagenesis. The silica-bearing materials may have formed via direct precipitation from silica saturated groundwater sources, although other formation mechanisms are also plausible.     

西乡群三郎铺组和大石沟组火山岩U-Pb定年及岩石成因研究

三郎铺组不整合上覆于孙家河组之上,与大石沟组呈连续过渡关系,两者均为一套火山沉积岩系。三郎铺组火山岩主要为玄武岩和流纹岩,大石沟组火山岩包括玄武岩、安山岩、流纹岩。大石沟组流纹岩LA-ICPMS锆石U-Pb定年揭示流纹岩形成时代为803.0±5.3Ma,属新元古代岩浆作用产物。元素地球化学和三郎铺组特有的陆相火山岩结构表明火山岩形成大陆板内伸展环境,属亚碱性火山岩系。三郎铺组玄武岩和流纹岩组成双峰式火山岩套,微量元素比值对模拟结果表明玄武岩浆来源于岩石圈地幔中原始石榴石二辉橄榄岩的部分熔融,部分熔融程度约为7%; 三郎铺组流纹岩浆源岩可能为白勉峡组下部的玄武质岩石,岩浆起源于斜长石稳定的下地壳源区或部分熔融形成的原生岩浆在上升过程中,经历了较为显著的斜长石结晶分异作用过程。大石沟组玄武岩、安山岩和流纹岩具有相同的微量元素比值、ε(t)值和t_DM,为同一母岩浆分离结晶的产物。玄武岩浆起源于原始石榴石二辉橄榄岩约10%的部分熔融,玄武岩浆分离结晶后残余岩浆比例约70%时形成安山岩浆,残余岩浆比例约20%~30%时产生流纹岩浆; 分离结晶的主要矿物包括斜长石和铁钛氧化物。三郎铺组和大石沟组均是新元古代晚期大陆裂谷作用的岩浆响应。     

The role of aqueous alteration in the formation of martian soils

Martian equatorial dark regions are dominated by unweathered materials and it has often been assumed that they have not been significantly altered from their source lithology. The suite of minerals present is consistent with a basaltic composition and there has been no need to invoke additional processes to explain the origin of these compositions. We have begun to question this result based on detailed observations using a variety of datasets. Locally derived dark soils have a mineralogy distinct from that of adjacent rocky surfaces; most notably a lower olivine content. This pattern is common for many surfaces across the planet. Previous work using detailed measurements acquired within the Gusev Plains has shown that olivine dissolution via acidic weathering may explain chemical trends observed between rock rinds and interiors. Mineralogical trends obtained from rocks and soils within the Gusev Plains are more prominent than the elemental trends and support previous results that indicate that dissolution of olivine has occurred. However, clear differences are also present in elemental abundances that indicate a variety of inputs and processes are likely responsible for the formation of martian dark soils. Despite the potential complexity of source materials and processes, it appears that most martian dark regions have likely experienced aqueous alteration and chemical weathering appears to be closely linked to the mechanical breakdown of materials. Regardless of the responsible mechanism, there appears to be a general, though not perfect, correlation between elevated olivine abundance and high-thermal inertia surfaces on Mars.