马坑铁矿钻孔岩心红外光谱特征及蚀变分带特征研究

红外反射光谱技术可无损、快速、批量地识别出硅酸盐、硫酸盐、碳酸盐等矿物,近年来在矿物学研究、地质勘探与找矿、矿山选冶等方面取得了较显著进展。尤其是热红外波段（6000~14500nm）可识别出辉石、石榴子石、橄榄石等蚀变矿物以及长石、石英等造岩矿物,对于矽卡岩型、铜镍硫化物型以及石英脉型等矿床地质找矿、矿床成因研究等具有重要意义。本文通过对国家实物地质资料馆馆藏的马坑铁矿钻孔岩心进行短波-热红外反射光谱测量与分析,总结马坑铁矿各蚀变矿物光谱特征,并快速厘定了该矿床的蚀变矿物类型及组合特征。马坑铁矿蚀变矿物主要有石榴子石、辉石、碳酸盐、绿泥石、绢（白）云母、角闪石、绿帘石、蒙脱石、石膏等。石榴子石热红外光谱特征是在9199nm、9730nm、10500nm及11100nm处具有明显的反射特征,辉石热红外光谱特征主要是在11500nm和12150nm处具有明显的吸收特征。红外光谱分析表明蚀变矿物在空间上呈现出明显的分带性,蚀变矿物组合及分布严格受围岩岩性和热液交代的双重控制。通过红外反射光谱蚀变矿物组合特征研究,“石榴子石+辉石”可作为矽卡岩型矿床的标型矿物组合,蚀变分带特征也反映了主矿体从高温到低温的变化过程;结合矿床地质特征,推断出马坑铁矿为典型的层控矽卡岩型矿床。本研究可为矽卡岩型矿床的成矿规律认识和找矿勘探等方面提供科学支撑。     

我国冬季季节性积雪反照率的观测与模拟——以东北地区为例

应用了一种新的模式spectral albedo model for dirty snow,简称SAMDS,研究了不同参数对于积雪反照率的影响,结果表明：在天顶角固定为60°的条件下,新雪的粒径从50 μm增大到800 μm,使其宽波段反照率从0.92减小到0.78;相对于非球形的雪粒,球形雪粒的积雪反照率更低;吸光性颗粒物对光谱反照率的影响主要在可见光和紫外波段。此外,雪粒径的增大能使吸光性颗粒物的光吸收效应增强。结合东北地区的实测数据,我们发现SAMDS模拟的积雪宽波段反照率与实测结果较为一致。同时,SAMDS模式模拟结果表明,在东北地区,积雪中0.1~1 μg·g^-1的黑碳浓度导致积雪宽波段反照率减少2%~8%,造成的瞬时辐射强迫为9~35 W·m^-2。     

基于混合像元分解的火星南极矿物制图研究

对火星高光谱遥感数据进行混合像元分解,有助于获取像元内部火星表面矿物含量。端元光谱提取和光谱解混是混合像元分解的关键技术。以ORB0942_2轨道覆盖的火星南极地区作为研究区,应用纯净像元指数法（PPI）从影像中提取出端元光谱,并利用线性分解模型对影像中混合像元进行了分解,计算出其各端元组分的百分含量,获得了研究区水冰、石膏、钙镁橄榄石及紫苏辉石的相对含量分布图。     

火星陨石和火星表面泥岩中蚀变过程对比研究

火星次生含水蚀变矿物是火星地质历史时期水环境和气候演变历史的真实记录,一直以来都是火星探测、火星陨石研究的重点,是认识火星环境特征和气候演化的重要研究对象。文中对比研究了表土角砾岩NWA7034、火成堆晶岩MIL03346等两块最富蚀变矿物火星陨石,以及Gale撞击坑出露的Sheepbed泥岩3种岩石类型的蚀变程度及其蚀变矿物类型和组合,分析了层状硅酸盐、铁氧化物/氢氧化物、钙硫酸盐等蚀变矿物的成因及环境指示意义。发现这3类岩石的蚀变作用各不相同。火星陨石NWA7034的蚀变作用以氧化和加热作用为主,无蒸发盐类矿物。火星陨石MIL03346的蚀变程度最低,为后期水溶液进入缝隙而引发的,蚀变作用以橄榄石的伊利石化、裂隙和缝隙中填充次生矿物细脉为主。而火星Sheepbed泥岩经历了后期的等化学风化过程(isochemical weathering),次生过程包括成岩蚀变和成岩后蚀变两个阶段。其中,成岩过程中的蚀变以橄榄石蚀变为铁氧化物和蒙皂石矿物为主,成岩后以形成蒸发盐类矿物硫酸钙为主。以上3种岩石蚀变矿物组成差异反映了火星上不同地质背景中、不同气候条件下蚀变过程的复杂性。文中对火星含水矿物及部分典型矿物的形成条件和过程进行系统总结,这对于理解未来火星探测任务、识别含水矿物的形成、揭示火星水环境和地质历史具有重要指导意义。     

用陆地卫星TM数据区分硫酸盐、碳酸盐及含水硅酸盐矿物

对两个地区（一个是半干旱的昆士兰，另一个是干旱的西奈）获取的陆地卫星ＴＭ数据对地质填图及工业矿产勘查的贡献进行了评价。每种情况均是用波段比值及其它标准技术进行数据分析。含水硅酸盐、碳酸盐及硫酸盐矿物作为一组矿物，可以通过它们在ＴＭ７波段上的吸收特征而与其它矿物区分开。然后用对数剩余值技术将ＴＭ数据还原成近似反射率并以假波谱的形式进行研究，这种波谱分析可以改进区分效果。在西奈可将含水硅酸盐矿物与碳酸盐矿物区分开。在昆士兰，能区分出含水硅酸矿物和硫酸盐矿物。尽管ＴＭ的波段宽、数量少，但还是能进行区分，表明ＴＭ数据的波谱特性还没有完全开发。     

基于ASTER VNIR SWIR多光谱遥感数据识别与提取干旱地区岩性信息——以西南天山柯坪隆起东部为例

ASTER多光谱遥感数据目前可以用于岩石矿物资源信息的识别和提取。本研究尝试利用ASTER 可见光近红外（VNIR）和短波红外（SWIR）的多光谱遥感数据提取干旱地区的岩石与矿物信息。基于新疆天山西南缘柯坪隆起东部不同地层单元岩石的化学组成和矿物成份以及VNIR SWIR谱域光谱吸收特征的分析,我们采用相关吸收波段深度（RBD）和波段比值（BR）方法对研究区的多光谱遥感数据进行图像处理,有效区分和识别了白云岩、石灰岩、砂岩以及阿克苏群的蓝片岩—绿片岩和砂质片岩。白云岩的CO2-3吸收谱带中心波长位于232〖KG*3〗μm,与灰岩的CO2-3 吸收谱带中心波长位置235 μm相比,具有向短波长方向移动的特点,据此可以利用RBD7、RBD8分别有效的识别白云岩和灰岩; 长英质岩石显示Al OH和Fe3+ VNIR SWIR吸收特征,而基性 超基性岩石显示Fe2+ 和Fe、Mg OH特征,利用不同的铁价态和次要矿物可以区分它们：ASTER band2/band1代表了含Fe3+ 矿物分布信息、ASTER band5/band4代表了含Fe2+ 矿物分布信息、RBD6可以估计Al OH矿物的丰度; 砂质/泥质片岩含较多的多硅白云母、绿泥石、黑硬绿泥石以及风化后表面覆盖的其它粘土矿物,在221 μm（band 6）存在有特征的吸收谱带,并且在165 μm（band 4）具有较高的反射率,而蓝片/绿片岩在221 μm（band 6）反射率较高,不具有明显特征吸收谱带,同时其在165 μm（band 4）反射率较低,因此蓝片/绿片岩ASTER band4/band6 比值低。应用ASTER band4/band6波段比值可以有效的区分开砂质/泥质片岩与蓝片岩/绿片岩。     

红外光谱在铁镁硅酸盐矿物类质同象研究中的应用

本文通过对柘榴石、辉石、角闪石和云母等铁镁质矿物的化学成分、光学性质和其它物性及红外吸收光谱的研究,试图找出它们的内在联系,以便用于研究矿物的类质同象变化规律。所测的矿物红外吸收光谱为中红外4000～400cm~(-1)波段的谱带特征,一般认为该波段主要是表现为硅酸盐中阴离子团的振动区。 从1、2图中可以看出所测矿物的谱带特征,铁镁硅酸盐谱带基本可分为三个波段,第一波段1100—800cm~(-1)据G.R.Hunt,J.W.Salisbury(1974),提出的硅酸盐光谱振动模式,该波段均为O—Si—O,Si—O—Si的非对称伸缩振动区。所以它们共同特点     

青海省阿尔金黄石山地区近红外蚀变矿物填图

利用近红外光谱对羟基(OH-)等敏感的特性,可以区分多种蚀变矿物及其矿物的不同结晶度,如舍羟基之硅酸盐矿物(绿帘石、闪石等),碳酸盐矿物(方解石、白云石等),层状硅酸盐中单矿物(粘土矿物、绿泥石、蛇纹石等),硫酸盐矿物(明矾石、黄钾铁矾、石膏等)等;矿物的结晶度不同,其红外吸收峰形也不相同,而矿物的结晶度标志着矿化作用...     

月球风暴洋火山口暗物质矿物反演及地质意义

月表主要矿物的空间分布是研究月球起源及演化等科学问题的重要信息之一.以风暴洋地区为例, 根据不同矿物光谱在可见光-近红外波段的吸收特征, 使用印度M3(moon mineralogy mapper)数据, 应用波谱特征拟合法(SFF)反演了火山口附近暗物质区域的单斜辉石、斜方辉石、橄榄石和尖晶石等铁镁质矿物的分布, 反演结果显示: 风暴洋地区提取的铁镁质矿物分布较集中, 其中辉石含量较多, 橄榄石和尖晶石含量相对较少.另外着重分析了橄榄石、尖晶石与周围矿物的关系及其地质意义.将提取结果与Lucey用于Clementine影像的光学模型填图结果进行对比显示, 提取的橄榄石分布集中, 但不存在大尺度的分布, 这与本文的研究区域面积有关; 就位置而言, 二者具有较好的一致性.      

东乌珠穆沁及渭源中铁陨石岩石学特征及其分类

对我国东乌珠穆沁及渭源２个中铁陨石的岩石学进行了研究,根据其硅酸盐基质的再结晶程度,我们将东乌珠穆沁陨石划分为类型Ｉ的中铁陨石,渭源陨石划分为类型Ⅲ的中铁陨石。东乌珠穆沁中铁陨石主要分布于细粒基质中的富斜方辉石碎屑及金属Ｆｅ－Ｎｉ组成,其硅酸盐质显示轻微的再结晶作用,渭源中铁陨石强烈风化并形成大量褐铁矿,该陨石主要由斜方辉石,斜长石组成,并有少量普通辉石,磷镁钙石,鳞石英及铁的氧化物;硅酸盐矿物广     

Sulfates on Mars: A systematic Raman spectroscopic study of hydration states of magnesium sulfates

The martian orbital and landed surface missions, OMEGA on Mar Express and the two Mars Explorations Rovers, respectively, have yielded evidence pointing to the presence of magnesium sulfates on the martian surface. In situ identification of the hydration states of magnesium sulfates, as well as the hydration states of other Ca- and Fe- sulfates, will be crucial in future landed missions on Mars in order to advance our knowledge of the hydrologic history of Mars as well as the potential for hosting life on Mars. Raman spectroscopy is a technique well-suited for landed missions on the martian surface. In this paper, we report a systematic study of the Raman spectra of the hydrates of magnesium sulfate. Characteristic and distinct Raman spectral patterns were observed for each of the 11 distinct hydrates of magnesium sulfates, crystalline and non-crystalline. The unique Raman spectral features along with the general tendency of the shift of the position of the sulfate ν₁ band towards higher wavenumbers with a decrease in the degree of hydration allow in situ identification of these hydrated magnesium sulfates from the raw Raman spectra of mixtures. Using these Raman spectral features, we have started the study of the stability field of hydrated magnesium sulfates and the pathways of their transformations at various temperature and relative humidity conditions. In particular we report on the Raman spectrum of an amorphous hydrate of magnesium sulfate (MgSO₄·2H₂O) that may have specific relevance for the martian surface.     

Ar-Ar chronology of the Martian meteorite ALH84001: evidence for the timing of the early bombardment of Mars

ALH84001, a cataclastic cumulate orthopyroxenite meteorite from Mars, has been dated by Ar-Ar stepped heating and laser probe methods. Both methods give ages close to 3,900 Ma. The age calculated is dependent on assumptions made about 39Ar recoil effects and on whether significant quantities of 40Ar from the Martian atmosphere are trapped in the meteorite. If, as suggested by xenon and nitrogen isotope studies, Martian atmospheric argon is present, then it must reside predominantly in the K-rich phase maskelynite. Independently determined 129Xe abundances in the maskelynite can be used to place limits on the concentration of the atmospheric 40Ar. These indicate a reduction of around 80 Ma to ages calculated on the assumption that no Martian atmosphere is present. After this correction, the nominal ages obtained are: 3940 +/- 50, 3870 +/- 80, and 3970 +/- 100 Ma. by stepped heating, and 3900 +/- 90 Ma by laser probe (1 sigma statistical errors), giving a weighted mean value of 3,920 Ma. Ambiguities in the interpretation of 39Ar recoil effects and in the contribution of Martian atmospheric 40Ar lead to uncertainties in the Ar-Ar age which are difficult to quantify, but we suggest that the true value lies somewhere between 4,050 and 3,800 Ma. This age probably dates a period of annealing of the meteorite subsequent to the shock event which gave it its cataclastic texture. The experiments provide the first evidence of an event occurring on Mars coincident with the time of the late heavy bombardment of the Moon and may reflect a similar period of bombardment in the Southern Highlands of Mars. Whether the age determined bears any relationship to the time of carbonate deposition in ALH84001 is not known. Such a link depends on whether the temperature associated with the metasomatic activity was sufficient to cause argon loss from the maskelynite and/or whether the metasomatism and metamorphism were linked in time through a common heat source.     

Mars,our neighbour

If we consider the solar system, our closest neighbour in terms of similarity is undoubtedly Mars. The planet has many features in common with the Earth, first discovered by the space probe Mariner in 1971. Since then, Mars has been subject to increasing interest by astronomers and geologists alike, and new data will start arriving when the six‐wheeled car‐sized rover named Curiosity begins rolling across the surface of Mars in August 2012. But how much do we already know about the ‘Red Planet?’ The aim of this article is to make information on Mars more available to the lay reader at a time when the ‘Red Planet’ is under the spotlight.     

Saltation threshold on Earth, Mars and Venus

New formulations valid for wide ranges of particle diameter and density and gas density are presented for prediction of saltation threshold speed for small particles. A low-air-density wind tunnel was used to extend the range of previous investigations and to separate the effects of Reynolds number and interparticle forces of cohesion. The new formulations are used to predict saltation threshold for atmospheric conditions on the surface of the Earth, Mars, and Venus.     

Experimental stability of magnesium sulfate hydrates that may be present on Mars

Since the Viking missions in 1976, magnesium sulfates have been predicted to exist on the surface of Mars. Recent orbital measurements suggest that Mg-sulfates are rather ubiquitous on the martian surface. Chemical analyses by landers support the inference that Mg-sulfate hydrates may be one source of the significant quantities of equatorial near-surface hydrogen observed by the neutron and γ-ray spectrometers on the Mars Odyssey spacecraft. The present study was undertaken to examine stability relations among the various Mg-sulfate hydrates. Using saturated salt solutions to control water-vapor pressure at temperatures of 3, 23, 50, 63, and 75 °C, Mg-sulfate phases were allowed to equilibrate from 2 to 3 months to see which hydration states were formed or were stable. Starting materials consisted of hexahydrite (6H₂O), starkeyite (4H₂O), kieserite (1H₂O), a second monohydrate-polymorph available as a chemical reagent, and an anhydrous MgSO₄ reagent. Products created in this study included these minerals, along with epsomite (7H₂O), sanderite (2H₂O), amorphous MgSO₄ (1-2H₂O), several previously undescribed phases, one of which was quite persistent (2.4H₂O), and trace amounts of pentahydrite (5H₂O). As expected, Mg-sulfate stability is strongly dependent on water vapor pressure and temperature. Lower temperatures favor the more hydrated Mg-sulfates. However, the MgSO₄ system was found to be surprisingly complicated and is strongly dominated by metastability, sluggish kinetics, and reaction pathways. Unexpected results were frequently encountered, in addition to the formation of previously undescribed phases. Several of the hydrates also show significant metastable extensions, such that phase boundaries can only be approximated. For example, kieserite, which has been reported on Mars from OMEGA data, in addition to having a distinct stability region, is resistant to transformation and persists throughout temperature-RH space until very high relative humidities are achieved. Results of this study show that MgSO₄ hydrates in addition to epsomite, hexahydrite, and kieserite can persist and should not be overlooked when assessing possible Mg-sulfate minerals that can occur on Mars.     

The bulk composition of Mars

An accurate assessment of the bulk chemical composition of Mars is fundamental to understanding planetary accretion, differentiation, mantle evolution, the nature of the igneous parent rocks that were altered to produce sediments on Mars, and the initial concentrations of volatiles such as H, Cl and S, important constituents of the Martian surface. This paper reviews the three main approaches that have been used to estimate the bulk chemical composition of Mars: geochemical/cosmochemical, isotopic, and geophysical. The standard model is one developed by Wänke and Dreibus in a series of papers, which is based on compositions of Martian meteorites. Since their groundbreaking work, substantial amounts of data have become available to allow a reassessment of the composition of Mars from elemental data, including tests of the basic assumptions in the geochemical models. The results adjust some of the concentrations in the Wänke–Dreibus model, but in general confirm its accuracy. Bulk silicate Mars has roughly uniform depletion of moderately volatile elements such as K (0.6 × CI), and strong depletion of highly volatile elements (e.g., Tl). The highly volatile elements are within uncertainties uniformly depleted at about 0.06 CI abundances. The highly volatile chalcophile elements are likewise roughly uniformly depleted, but with more scatter, with normalized abundances of 0.03 CI. Bulk planetary H₂O is much higher than estimated previously: it appears to be slightly less than in Earth, but D/H is similar in Earth and Mars, indicating a common source of water-bearing material in the inner solar system. K/Th ranges from ∼3000 to ∼5000 among the terrestrial planets, a small range compared to CI chondrites (19,000). FeO varies throughout the inner solar system: ∼3 wt% in Mercury, 8 wt% in Earth and Venus, and 18 wt% in Mars. These differences can be produced by varying oxidation conditions, hence do not suggest the terrestrial planets were formed from fundamentally different materials. The broad chemical similarities among the terrestrial planets indicate substantial mixing throughout the inner solar system during planet formation, as suggested by dynamical models.     

Aqueous geochemistry on early Mars

A geochemical cycle model is presented for the interaction between the atmosphere, hydrosphere, and regolith of Mars. It was developed to study how this interaction might have produced the present Martian environment from a primitive Martian environment much like that of the primitive Earth. The model is a simple system, consisting of an unweathered starting material (calcium-bearing and magnesium-bearing silicates), a CO2 atmosphere, an ocean of water in contact with both the atmosphere and the unweathering starting material, and both calcite and dolomite precipitates. Several interesting points arise from this model. A 1-bar CO2 atmosphere can be removed by carbonate precipitation alone in about half a billion years. This is roughly fifty times longer than earlier estimates, which were not based on time-varying models (Fanale et al., 1982; Carr, 1986; Pollack et al., 1987). One of the chief problems in Martian geology has been how to explain the large number and wide variety of surface features that were apparently formed by aqueous erosion. This longer atmospheric lifetime may be enough to explain the large number of channels seen on older Martian terrain. If the atmosphere started out with more than 1 bar of CO2, it would take correspondingly longer to remove it. If there should be no other means to remove CO2 from the atmosphere, this long time constant would indicate that the atmosphere could never have contained more than a few bars of CO2, or else there would still be remnants present today. The increase in alkalinity of the ocean as the atmosphere disappears, even without the effects of reduction in the amount of water available, indicates that evaporite deposits may have formed on Mars. If these deposits are still present, they may even yet contain some liquid water.     

A Comparative Analysis of Evaporate Sediments on Earth and Mars：Implications for the Climate Change on Mars

The knowledge of Martian salts has gone through substantial changes during the past decades. In the 70th of last century, Viking landers have noticed the existence of salts on Mars. Several salt species have been suggested from then on, such as sulfates and chlorides. However, their origin was a mystery due to the lack of observations. The recent explorations and related studies at the beginning of this century revealed that the crustal composition of Mars is similar to that of Earth, and it was hypothesized that almost one third of Martian surface was covered by oceans and lakes in the early stage of Mars. The huge water bodies may have dissolved a large quantity of ions from Martian primary rocks during the whole Noachian and Hesperian epoch. After the enormous drought event happened during the late Hesperian and the early Amazonian, these dissolved ions have formed huge salts deposits and most of them were preserved on Mars until today. To date, carbonates, sulfates, chlorides have all been detected by orbital remote sensing and by landers and rovers. However, the salt mineral assemblages on Mars seems to have some differences from those on Earth, e.g., rich in sulfates and lack of massive carbonates. To explain this difference, we propose that most of the surface carbonates precipitated from the ancient oceans may have been dissolved by the later ubiquitous acidic fluids originated from the global volcanism in the Hesperian era, and formed the enormous sulfate deposits as detected, and this hypothesis seems to be supported by the evidence that most of the sulfate deposits distribute around the Tharsis volcanic province while the survived carbonates located far from it. This process can release most of the carbon on Mars to the atmosphere in the form of CO2 and then be erased by the late heavy bombardments, which might have profound influence on the climate change happened in the Hesperian age. The positive correlation between the GRS results of the potassium distributions and the distribution of chlorides on Mars, together with the high Br concentration measured from the evaporate sediments at two Mars exploration rover landing sites, indicate that the brines in the regions where the chlorides deposited may have reached the stage for potassium salts deposition, thus we propose for the first time that potassium salts deposits might be prevalent in these regions.     

Unique Aeolian Bedforms of Mars: Transverse Aeolian Ridges

Transverse Aeolian Ridges (TARs) are among the unique aeolian bedforms of Mars, which witnessed a series of investigation for the last two decades thanks to the high-resolution remote sensing data. This paper summarized the understanding with respect to distribution, morphology, sedimentology, formation hypotheses and formation time of TARs. It is suggested that TARs are a kind of aeolian bedforms with meter-scale height and decameter-scale wavelength. TARs are primarily distributed in the equator and low-latitude regions, being rare in high and mid-latitude regions, and more popular in the south hemisphere than in the north hemisphere. Higher albedo and symmetric cross-sections are the most outstanding features of TARs, being analogous to the megaripples and reversing dunes on the Earth. The grain-size distribution of TARs’ sediments is generally bimodal, with granule cover and low thermal inertia. Three formation hypotheses were proposed for TARs: Megaripple hypothesis, reversing dune hypothesis and dust induration hypothesis, with more evidences supporting the megaripple hypothesis. Similar to dunes, TARs are geologically recent morphology on Mars, but generally predate dunes, formed in the last few million years so that most TARs are indurated or lithified and are immobile. However, contemporary mobileTARs are also developed in some regions. The unique features of TARs make them the mostenigmatic aeolian bedforms of Mars. It is proposed that high-resolution information on TARs sedimentology and integrated regional surveying should be listed in the priorities of future Mars exploration with respect to TARs study.     

On the in situ aqueous alteration of soils on Mars

Early (>3 Gy) wetter climate conditions on Mars have been proposed, and it is thus likely that pedogenic processes have occurred there at some point in the past. Soil and rock chemistry of the Martian landing sites were evaluated to test the hypothesis that in situ aqueous alteration and downward movement of solutes have been among the processes that have transformed these portions of the Mars regolith. A geochemical mass balance shows that Martian soils at three landing sites have lost significant quantities of major rock-forming elements and have gained elements that are likely present as soluble ions. The loss of elements is interpreted to have occurred during an earlier stage(s) of weathering that may have been accompanied by the downward transport of weathering products, and the salts are interpreted to be emplaced later in a drier Mars history. Chemical differences exist among the sites, indicating regional differences in soil composition. Shallow soil profile excavations at Gusev crater are consistent with late stage downward migration of salts, implying the presence of small amounts of liquid water even in relatively recent Martian history. While the mechanisms for chemical weathering and salt additions on Mars remain unclear, the soil chemistry appears to record a decline in leaching efficiency. A deep sedimentary exposure at Endurance crater contains complex depth profiles of SO₄, Cl, and Br, trends generally consistent with downward aqueous transport accompanied by drying. While no model for the origin of Martian soils can be fully constrained with the currently available data, a pedogenic origin is consistent with observed Martian geology and geochemistry, and provides a testable hypothesis that can be evaluated with present and future data from the Mars surface.