共查询到19条相似文献，搜索用时 187 毫秒
1.
在海相蒸发岩矿床的地质-地球化学研究中,常应用盐类矿物中的微量元素来研究钾盐矿床的成因和成矿指示标志,Br、Rb就是其中很重要的2种微量元素。缺硫酸镁型钾盐矿床在成盐过程中会蒸发沉积形成氯化物型的盐类物质, Br、Rb按一定的规律分配到这些盐类物质中而不形成独立矿物。在盐类物质蒸发结晶过程中,Br、Rb在固_液相之间的分配主要受温度控制。文章通过Br和Rb的地球化学特征及微量元素分配的热力学分析,建立了Br、Rb在盐类矿物相中的分配系数与温度间的热力学函数模型:,并探讨了利用这些公式来计算出钾盐矿床结晶作用形成盐类物质时的古温度,这对研究钾盐矿床形成时的古环境、物质基础条件、物理化学条件等具有重要意义。 相似文献
2.
大浪滩盐湖蒸发盐嗜盐菌培养鉴定及其天体生物学意义 总被引：1，自引：0，他引：1
通过火星遥感及火星登陆测量都发现了火星上存在大量的含水硫酸盐,这些盐类的状态和演化也见证了近代火星表面环境条件的变化。大浪滩盐湖是柴达木盆地第二大盐湖,也是中国最为干旱的地区之一,而且大浪滩盐湖分布有与火星类似的硫酸盐盐类沉积。我们采集了蒸发盐表层盐壳,盐湖结晶盐以及剖面沉积盐类等样品,进行室内分离、培养及鉴定嗜盐菌研究。结果表明,大浪滩盐结晶及盐类沉积中分布有不同类型的嗜盐菌,主要类型为Virgibacillus,Oceanobacillus,Halobacillus,和Terribacillus等。大浪滩盐湖蒸发盐中内生嗜盐菌的分离鉴定,为探索火星高盐环境中生命存在的形式和机制提供一种类比模式。 相似文献
3.
罗布泊“大耳朵”湖区钾元素地球化学与富集机理 总被引：2，自引：0，他引：2
对罗布泊“大耳朵”干盐湖盐壳的沉积过程、钾元素空间分布特征及地下卤水化学性质进行了实地调查研究。“大耳朵”湖区地下卤水盐度为341 g/L左右,ρ(K+)变化于7.0～12.4 g/L,平均值9.61 g/L,高浓度富钾卤水通过毛细管上升和地表析盐,导致钾盐矿物在地表析出,地表盐壳的w(K+)变化于0～4.7 g/kg,平均含量2.05 g/kg,钾盐矿物主要包括光卤石、杂卤石和软钾镁钒。研究表明盐壳盐类矿物在干盐湖地表的聚集及地球化学分布特征与地下卤水的化学性质有着密切关系,盐壳沉积后期风蚀、雨淋、季节性的地表径流都会影响和重塑盐壳地球化学组成特征,钾盐矿物可作为盐壳增长发育的指示矿物。 相似文献
4.
在盐湖沉积演化过程中,钾镁盐在盐类矿物沉积的中晚期才开始结晶析出。因此,研究含盐系地层中盐类矿物的沉积地球化学特征,不仅可以从侧面获取岩盐的沉积物物质来源和成盐期古卤水蒸发浓缩程度等地球化学信息,而且可以直接揭示古盐湖期钾盐富集趋势及规律。目前,除在江陵凹陷的古近系沙市组等含盐系内发现了富钾卤水外,还在中-南部的钻孔盐矿盐岩中,发现了微量钾石盐和钾石膏,这些说明该凹陷古近纪具有成钾潜力。本文通过对SK3井蒸发岩特征研究及岩芯中K、Mg、Cl、Br离子含量与Br×103/Cl系数的垂向变化分析,揭示古盐湖浓缩演化与钾盐富集趋势,进一步揭示该层段沉积时期及所在凹陷古盐湖卤水钾的富集程度。 相似文献
5.
蒸发岩序列中氯化物盐的氯同位素分馏效应及应用——兼论塔里木盆地、柴达木盆地古代岩盐的沉积阶段 总被引：5，自引：0，他引：5
卤水蒸发析盐到晚期阶段,才有可能析出溶解度极大的钾盐类矿物,因此在一个成盐盆地要找到钾盐矿床,除判断物源特征外,还必须找到最晚沉积阶段的区域和层位。本文通过对实验室配制溶液和盐湖卤水蒸发析出的不同氯化物矿物、钾盐矿床沉积序列不同阶段盐类矿物对比分析,讨论了氯同位素的分馏规律。结果表明,不同蒸发浓缩阶段的氯化物盐,氯同位素发生显著分馏。一般钾盐沉积层位的石盐δ37Cl值小于0,钾石盐及其以后沉积的氯化物δ37Cl值小于-0.5‰,特别是钾石盐以后析出的氯化物更为偏负,光卤石一般小于-1.00‰,而钾盐沉积阶段之前早期沉积石盐的δ37Cl值显著偏正。因此,δ37Cl值是判断岩盐沉积阶段的有效指标。基于此,对塔里木库车盆地第三纪、莎车盆地白垩-第三纪部分代表性盐矿点以及柴达木盆地西部不同构造单元、不同层位第三纪岩盐沉积做了氯同位素分析。初步结果表明塔里木莎车盆地晚白垩世岩盐的沉积阶段明显晚于库车盆地第三纪沉积,特别是莎车盆地喀什次级凹陷δ37Cl值最低,大部分样品小于-0.5‰,推测该区成盐古卤水已浓缩到晚期或接近晚期钾盐沉积阶段,应是今后一重点开展钾盐找矿的区域。柴达木盆地油墩子、南翼山地区中新统、上新统蒸发岩沉积序列δ37Cl值普遍偏正,推测当时卤水浓缩演化可能只达到石盐沉积阶段,浓缩到后期阶段的富K+、Mg2+盐溶液随西部隆起迁移到柴达木盆地南部地区,因此认为第三纪地层虽然石盐沉积层位多,厚度大,但找到大规模钾盐矿床的可能性不大。 相似文献
6.
刚果(布)布谷马西钾盐矿床盐类矿物特征与成因研究 总被引：1，自引：0，他引：1
刚果(布)布谷马西钾盐矿床位于非洲大陆西部边缘,是白垩纪时期沉积的大型钾盐矿床。文章运用X射线衍射、薄片鉴定、扫描电镜和岩石地球化学等方法,识别出布谷马西钾盐矿的主要盐类矿物有硬石膏、石盐、光卤石、钾石盐、水氯镁石和溢晶石。盐类矿物的沉积顺序为:硬石膏→石盐→光卤石→钾石盐→水氯镁石或溢晶石。该矿区的成盐物质主要来源于海水,盐类沉积物中贫碳酸盐和硫酸盐矿物,可能与白垩纪"方解石海"的海水成分密切相关。矿区中的钾石盐主要是由光卤石淋滤形成。 相似文献
7.
8.
【研究目的】老挝钾盐矿床是世界上重要的钾盐矿床之一,开展该矿床钾盐析出阶段沉积环境研究对于深入理解钾盐成矿作用具有重要意义。【研究方法】钾盐矿层中的水不溶矿物比可溶盐类矿物保存了更多的原始信息,是研究成矿卤水演化的重要载体。本文以老挝万象盆地海夏峰矿区ZK16钻孔为研究对象,利用镜下鉴定、XRD及SEM等方法对该钻孔钾盐矿层的水不溶矿物开展了系统研究。【研究结果】分析结果表明,水不溶物中的主要矿物为硬石膏、方硼石、水氯硼钙石、石英、白云石、菱镁矿、方解石、白云母等,其中以硬石膏、方硼石是主要的水不溶矿物。自生石英及碎屑白云母的存在及其分布特征指示了钾盐在沉积过程中不同程度地受到陆相水体的影响。【结论】综合研究揭示,研究区钾盐沉积可以分为波动沉积、浅水沉积、稳定沉积和改造作用等4个不同阶段。 相似文献
9.
新疆库车盆地钾盐科探1井含盐系地球化学特征及找钾指示 总被引：2，自引：0，他引：2
在盐湖沉积演化过程中,钾盐矿物在盐类沉积的中晚期阶段才开始析出。因此,研究含盐系盐类的沉积地球化学特征,不仅可以从侧面获取岩盐的沉积物源和成盐古卤水蒸发浓缩程度等地球化学信息,而且更能揭示古盐湖钾盐富集趋势。文章通过对库车盆地钾盐科探1井钻取的岩芯样品进行高精度采样测试,得出岩盐中Mg×103/Cl、K×103/Cl、Li×103/Cl与K+、Mg2+、Li+、Ca2+、Cl-含量的垂向变化规律。并与库车盆地其他钻孔中的岩盐含钾性进行对比,同时,依据钻井剖面岩性特征,与潜江凹陷和大汶口凹陷含盐系剖面进行对比,论述研究区成盐的地球化学特征,对其钾盐成矿前景进行分析和评价。 相似文献
10.
黄建国 《沉积与特提斯地质》1993,(5):44-56
据记载,分布于上扬子区寒武系的石膏岩仅有零星资料。如今,大量蒸发岩如溶蚀角砾岩、硬石膏、石盐岩及富钾卤水等已被发现。沉积相经历了从盆地相、台地相到蒸发岩相的演化过程。在中、下寒武统中找到海退沉积序列。古构造-古地理背景是蒸发岩沉积的重要控矿条件之一。周边板块运动及塑性基底的褶皱,导致台缘隆起及台内坳陷的形成。岩相古地理图展示从碳酸盐、硫酸盐到氯化物盐类的“泪滴式”沉积相带。蒸发岩沉积于台缘隆起及礁生长进入堰塞潟湖至盐湖阶段。在稳定坳陷区沉积盆地中蒸发岩系发育;石盐岩较厚,其溴氯比值为0.2—0.4;古气候炎热、干燥;在蒸发岩体周围有沉积(封层)水及溶滤水,其含钾(K~+)量为0.10—4.76g/L;水文地球化学比值(如钾氯比值、钾盐比值及钾溴比值等)指示含钾异常;盐湖浓缩卤水达到氯化物盐类沉积阶段及相应的构造封闭程度;含盐地质标志广泛分布等等。鉴于上述,估计该区可能具备钾盐成矿条件。然而目的层埋藏太深,因此笔者建议,应在浅埋部位进行有效的成矿预测,为普查指出远景区。 相似文献
11.
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. 相似文献
12.
Ronald Amundson Stephanie Ewing Brad Sutter Oliver Chadwick Michelle Walvoord 《Geochimica et cosmochimica acta》2008,72(15):3845-3864
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. 相似文献
13.
Continental evaporites are deposits that originate from the evaporation of saline waters in the low areas of saline lakes from all continents, except Europe, and mainly consist of chloride, sulphate and potash minerals. In recent years, the discovery on the Martian surface of hydrated salt minerals, including sulphates and chlorides, interpreted as deriving from the desiccation of preexisting large bodies of water, such as lakes, has provided further convincing evidence of liquid water activity on the surface of Mars and, consequently, it has reinforced the plausibility of finding life. Because evaporites require short‐term aqueous processes for their formation, they can trap and preserve over geologic times a biological record made up of halophilic extremophiles—such as microalgae, bacteria, and their remains—that recent research on Earth has shown to be characterized by unexpectedly high biodiversity. This record may consist of varying types of fossils, including morphological fossils, chemofossils and biominerals. As a consequence, continental evaporite environments and their saline deposits are now a primary target for the near future astrobiology missions devoted to the search for fossil Martian life. Lacustrine evaporite deposits and minerals have, therefore, been identified as primary targets for the NASA–ESA joint programme of the Mars sample return, planned for the end of the current decade. Copyright © 2011 John Wiley & Sons, Ltd. 相似文献
14.
Schaefer MW 《Geochimica et cosmochimica acta》1993,57(19):4619-4625
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. 相似文献
15.
火星生命研究的进展与前景 总被引：3，自引：0，他引：3
关于火星是否存在或曾经存在生命的争论由来已久。有人以ALH84001火星陨石新鲜破裂面上的大量碳酸盐小球体和多环芳香烃（PAHs）为主要依据，推论火星至少在13～36亿 aBP前很可能有生命形态存在。然而，很多人认为ALH84001陨石的各种特性可以是非生物成因的。由于地球上的生物在超过115℃的温度下很难存活（火星可与之类比），争论的焦点逐渐集中在碳酸盐球体的形成温度上。也有研究者关注该陨石上有机物质的来源问题。对ALH84001陨石的综合学科研究提出了互相矛盾的证据。综述了自1996年以来在国外各种主要期刊上发表的关于 ALH84001陨石与火星生命的研究成果（也包括了一些对其他火星陨石的研究），认为目前尚不能断言火星生命存在与否。对火星继续深入探索以获取进一步的证据是十分必要的。以美国国家航空和宇航局（NASA）Odys sey宇宙飞船起始的火星探测计划将引发新一轮火星生命研究的热潮。 相似文献
16.
The assemblage clinopyroxene + magnesite was observed in Earth’s high-pressure metamorphic samples, and its stability in subducting slabs was confirmed by experiments. Recent studies also suggested that the fO2 variations observed in SNC meteorites can be explained by polybaric graphite-CO-CO2 equilibria in the Martian mantle. Although there is no direct evidence for the stability of the cpx + mc assemblage in Mars mantle, its high-pressure–high-temperature decomposition to cpx + fo + CO2 makes it a good analogue for the source of carbon metasomatism, in particular, to study nakhlites formation. Iron, which is present in the Earth’s and Martian mantles, may, however, influence the speciation of carbon. We performed experiments on a clinopyroxene + magnesite assemblage at 1.8 and 3.0 GPa and temperatures corresponding to the Earth’s and Martian mantles. The role of iron and of fO2 was investigated by (1) replacing all or part of the magnesite by siderite FeCO3, (2) adding Fe0 and (3) using graphite C capsules. A carbonate-silicate melt forms at both Earth and Mars conditions. Clinopyroxene and olivine are the main solid phases in the iron-free experiments. Fe2+ and Fe0 decrease their melting temperatures and increase the silicate fraction in the melt. The produced carbonate-silicate melts may be involved in the formation of some carbon-rich lavas on Earth (e.g., carbonatites, ultramafic lamprophyres, or kamafugites). Our results may also be used to interpret ophiolite samples or inclusions. In particular, we show that wüstite may form in equilibrium with carbonate-silicate melt in opx-(and silica-) poor regions of the mantle below 3 GPa. Our results also confirm the hypothesis of carbon metasomatism in the Martian nakhlites source. Immiscibility or reduction could explain the absence or rarity of C in Martian lavas. 相似文献
17.
在地球上,水是生命存在的基础之一.大量证据表明火星表面曾经存在液态水,而目前的火星表面环境不支持液态水的长期存在.因此,水可能以不同的状态赋存于火星的次表层.寻找火星次表层的水一直是火星探测的关键科学目标之一.次表层探测雷达,如探地雷达、探冰雷达,是了解地下物质结构的有效方法,近年来在地外天体上得到大量应用.在过去十余年,欧洲的火星快车(Mars Express)上搭载的火星次表层和电离层探测先进雷达(Mars Advanced Radar for Subsurface and Ionosphere Sounding,MARSIS)和美国火星勘测轨道飞行器(Mars Reconnaissance Orbiter,MRO)上搭载的浅表层雷达(Shallow Subsurface Radar,SHARAD)已在火星轨道上获取了大量数据,被广泛应用于研究火星的地下结构,尤其是地下水冰探测.我国的天问一号火星探测器也携带了高低频轨道探测雷达和高低频火星车探地雷达,有望在不同的顺轨向、交轨向和距离向分辨率上揭示火星次表层不同深部的结构.本文综述了轨道器次表层探测雷达的探测原理和优势,简要介绍了雷达数据的处理和解译方法,重点总结了 MARSIS和SHARAD近年来对火星水冰探测的最新进展,最后对天问一号环绕器雷达及其水冰探测作简要展望. 相似文献
18.
火星表面的古湖泊地貌能够反映火星古气候和古环境的特征及变化,对于研究火星是否曾经存在宜居环境具有重要意义.随着中国火星探测计划的提出和实施,详细了解火星古湖泊的研究进展尤为重要.总结了火星古湖泊的研究现状,重点阐述了当前对火星古湖泊的沉积地貌、矿物成分、形成年龄、分布特征等方面的研究进展.在综合分析前人研究成果的基础上,提出火星古湖泊研究中存在的主要问题,认为未来应着重在古湖泊的详细调查与地质填图、古湖泊的后期改造作用、其他类型古湖泊的识别分析以及火星与地球古湖泊的对比等方面开展研究. 相似文献
19.
《Comptes Rendus Geoscience》2007,339(14-15):917-927
Plate tectonics shaped the Earth, whereas the Moon is a dry and inactive desert, Mars probably came to rest within the first billion years of its history, and Venus, although internally very active, has a dry inferno for its surface. Here we review the parameters that determined the fates of each of these planets and their geochemical expressions. The strong gravity field of a large planet allows for an enormous amount of gravitational energy to be released, causing the outer part of the planetary body to melt (magma ocean), helps retain water on the planet, and increases the pressure gradient. The weak gravity field and anhydrous conditions prevailing on the Moon stabilized, on top of its magma ocean, a thick buoyant plagioclase lithosphere, which insulated the molten interior. On Earth, the buoyant hydrous phases (serpentines) produced by reactions between the terrestrial magma ocean and the wet impactors received from the outer solar system isolated the magma and kept it molten for some few tens of million years. The planets from the inner solar system accreted dry: foundering of wet surface material softened the terrestrial mantle and set the scene for the onset of plate tectonics. This very same process also may have removed all the water from the surface of Venus and added enough water to its mantle to make its internal dynamics very strong and keep the surface very young. Because of a radius smaller than that of the Earth, not enough water could be drawn into the Martian mantle before it was lost to space and Martian plate tectonics never began. The radius of a planet is therefore the key parameter controlling most of its evolutional features. 相似文献