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1.
对火星陨击坑壁上发育的冲沟进行研究,分析其成因和控制因素并进而探讨火星表面附近发生的地质过程,是当今火星研究的重要课题之一。采用分形理论对火星南半球中纬度9个陨击坑壁内不同方位发育的冲沟沟头形态进行了研究,结果表明沟头的分维值与冲沟发育程度呈显著的正相关关系。冲沟沟头的分维值大小分布与冲沟的方位关系密切,面向极地的冲沟分维值较大,面向赤道的冲沟分维值较小。陨击坑内不同方位冲沟所处位置的局部气候因素差异控制了水量的大小,从而造成陨击坑内不同方位冲沟发育程度和分维值大小的差异。研究结果为强调火星气候因素控制了冲沟形成的地表冰雪积累/融化成因模式提供了佐证。 相似文献
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玉兔二号月球车在嫦娥四号着陆区发现了许多坑缘呈破碎石块状的小型撞击坑,其直径大多在亚米级,过去对于这种小尺度撞击坑的研究大多源于Apollo、Surveyor、Ranger系列任务,然而当时获取的影像质量较低,且并未覆盖月球背面.小尺度撞击坑在月球表面分布十分广泛,与月球最表层的演化密切相关,因此对其展开研究具有重要的意义.本文利用嫦娥四号任务获取的高分辨率全景影像,统计了8、9、11～15月昼影像中新鲜撞击坑的直径、频数、深度等信息,并根据这些撞击坑和周围石块的形态特征,推测这些坑应该形成于不同方向的二次撞击事件,这为揭示玉兔二号月球车行进途中观测物质的来源提供了重要信息.小型二次撞击坑从深径比中难以与一次撞击坑区分,且一般处于饱和状态,因此应避免使用小尺寸的撞击坑进行定年. 相似文献
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地月系统不同成因环形构造及其影像特征 总被引：2，自引：0，他引：2
环形构造是一种常见的地质现象,特别是在月球上分布更为普遍。本文论述了三种成因的环形构造,即:侵入岩成因的环形构造,火山成因的环形构造,以及小天体撞击形成的撞击坑。文中详细介绍了它们的成因与结构特征,指出侵入岩成因的环形构造主要由岩浆冷凝收缩形成,在遥感影像上主要表现为影像色调的不同;火山成因的环形构造为火山口,在遥感影像上具有环形结构;而小天体撞击形成的撞击坑形态复杂,如碗形坑、中心锥环形坑与多环撞击坑,撞击坑的坑沿外缓内陡,遥感影像上表现为环形或弧形构造,有些撞击坑具有辐射纹。 相似文献
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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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人工降雨条件下冲沟型泥石流起动试验研究 总被引：1，自引：0，他引：1
下垫面以位于贡嘎山东坡的熊家沟为模型,开展了不同降雨强度条件下冲沟型泥石流起动的模拟试验,初步研究了冲沟型泥石流的形成机理和演化特征.试验研究表明:(1)在强降雨条件下,水体入渗速度、不同深度土体含水量变化与降雨强度呈反比例关系,降雨强度越大,越不利于水体入渗,而有利于坡面汇流、冲沟径流和下切侵蚀; (2)在强降雨和径流条件下,土体破坏方式、破坏程度以及泥石流形成机理表现出差异性.相对较小雨强降雨条件下,土体破坏方式以滑坡为主,泥石流形成模式表现为滑坡液化与转化起动,雨强较大降雨条件下,土体破坏方式以侵蚀垮塌为主,泥石流形成模式为洪流席卷垮塌体和沟床揭底; (3)起动试验中泥石流阵性特征明显.在强降雨条件下,雨强与泥石流的规模、黏度之间没有正相关性,雨强越大,泥石流黏度越小,试验中多出现的是高含砂洪流,而相对较小雨强作用下由土体液化转化形成的泥石流黏度较大.试验现象和结果与熊家沟泥石流起动、发生过程具有较高的一致性. 相似文献
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江西信江盆地晚白垩世风成沙丘的发现及其古风向 总被引：7，自引：3，他引：7
长期以来,江西信江盆地晚白垩世圭峰群塘边组(K2t)均定为水成沉积,本文的研究结果则认为属风成沉积.沉积结构、构造和石英沙颗粒表面特征研究结果表明,该组的主体岩性为紫红色中-细粒净砂岩,基本不含泥质和云母等悬移质,大型高角度平板状交错层理发育,层系厚度巨大,风成沙丘前积层特征明显,石英沙磨圆度好,在电子显微镜下普遍可见风成沙特有的碟形撞击坑、新月形撞击坑和毛玻璃化表面特征,属于风成沙丘沉积.古流向恢复表明,信江盆地以西风为主,东北风为次,同时见有少量东南风与西北风.根据当时的古地理格局及地表风带模式判断,研究区位于当时的北半球西风带和东北信风带之中,同时可能存在东南向和西北向的古季风. 相似文献
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月球表面环形构造主要有撞击坑、火山口和月海穹窿3种,其中撞击坑分布最广泛,是研究月表环形构造的主要内容。由于月表撞击坑数量大、种类多及其形成伴随着整个月球地质的演化过程,因此这种月表地形地貌比较完整地记录了月球表面地貌随时间的改造过程以及改造类型。文中通过研究撞击坑遥感影像及形貌特征,总结归纳为简单型、碗型、平底型、中央隆起型、同心环型、复杂型及月海残留型7种撞击坑类型,用来描述月表典型区域撞击坑的形态特征。从结构和物质两方面进行了月表典型区域撞击坑的形态地貌参数提取,综合利用嫦娥一号CCD 影像数据、LROC数据,得到了该区域撞击坑形态数据(坑底、坑唇、坑壁、坑缘、溅射物覆盖层、中央峰)和形态测量数据(直径、深度、地理位置)。研究发现,LQ 4地区的撞击坑分布可分为月陆区和月海区,月陆区的撞击坑多以中小型撞击坑为主,其分布密度极高,形成年代较早,月海区撞击坑多为年轻的撞击坑,分化程度较低,分布密度也较低。 相似文献
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风沙地貌分为风积地貌和风蚀地貌两大范畴,风积地貌即指各种沙丘.沙丘地貌虽然是风沙堆积的产物,但其形态和类型是风沙蚀积时空变化规律的表现,在堆积形成之后,风蚀作用在沙丘形态塑造过程中有时会具有重要作用,从而形成独特的侵蚀型沙丘.但由于有悖于传统风积地貌的理解,侵蚀型沙丘长期被忽视.然而,在火星沙丘地貌的形态和分布规律研究中,已发现大量的与地球常见沙丘地貌具有微妙差异的沙丘地貌形态,并将其归咎于沙源供应不充分的发育环境.重温法国学者Mainguet沙丘分类方案中关于侵蚀型沙丘的论述,以及经典风沙地貌学理论关于沙丘形态控制因素的概念框架,明确指出研究侵蚀型沙丘的必要性.系统分析了火星沙丘地貌形态特征后,初步辨认出火星的10种侵蚀型沙丘,分析其形态特征、发育环境及可能的形成机制.地球干旱区广袤的盐碱地是极有可能发育侵蚀型沙丘的地区,具有类似火星沙源供应不足的环境,在中国柴达木盆地沙漠中发现了多种侵蚀型沙丘地貌.据此推断,侵蚀型沙丘在地球上比较普遍,其研究对发展风沙地貌学理论具有重要意义,对中国未来的火星探测与研究具有参考意义. 相似文献
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撞击坑统计定年法的基本原理是首先得到月球表面撞击坑密度分布的一般规律(即产率函数),然后将其应用到Apollo和Luna任务采样的区域中,得到大干特定直径(常用1 km)的撞击坑密度,然后在该密度和样品的同位素年龄之间建立函数关系(即年代函数).在对没有样品的地质单元进行年龄分析时,首先从遥感影像解译撞击坑,然后根据产率函数求解大于指定直径撞击坑的密度,最后将其代入年代函数中求解该区域的地质年龄.根据其它行星与月球撞击环境的差异等因素,该方法已经推广到其它行星表面地质年龄的研究中.本文详细分析了撞击坑统计定年方法的原理,以及在应用中需要注意的问题. 相似文献
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The 27.2 km diameter Tooting crater is the best preserved young impact crater of its size on Mars. It offers an unprecedented opportunity to study impact-related phenomena as well the geology of the crust in the Amazonis Planitia region of Mars. For example, the nearly pristine condition enables the partial reconstruction of the sequence of events for crater formation, as well as facilitates a comparison to deposits seen at the Ries crater in Germany. High-resolution images taken by the High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX) on the Mars Reconnaissance Orbiter spacecraft have revealed a wealth of information on the distribution of features within the crater and beyond the rim: a large central peak, pitted material on the floor and terrace blocks, lobate flows interpreted to be sediment flows, impact melt sheets, four discrete layers of ejecta, and an asymmetric secondary crater field. Topographic data derived from the Mars Orbiter Laser Altimeter (MOLA) and stereo HiRISE and CTX images show that the central peak is ～1100 m high, the lowest point of the crater floor is 1274 m below the highest part of the rim, and the crater rim has ～600 m of variability around its perimeter. Layering within the cavity walls indicates ～260 m of structural uplift of the target material, which constitutes ～35% of the total relief of the rim. Abundant evidence is found for water flowing down the cavity walls, and on the surface of the ejecta layers, both of which took place sometime after the impact event. Thickness measurements of the ejecta layers reveal that the continuous blanket is remarkably thin (～3–5 m) in some places, and that the distal ramparts may be ～60 m high. Crater counts made on the ejecta layers indicate a model age of <3 Ma for the formation of Tooting crater, and that the target rocks have a model age of ～240–375 Ma. It is therefore possible that this may be the source of certain basaltic shergottite meteorites ejected at ～2.8 Ma that have crystallization ages which are comparable to those of the basaltic lava flows that formed the target materials for this impact event. The geology and geomorphology of Tooting crater may help in the interpretation of older large impact craters on Mars, as well as the potential role of target volatiles in the impact cratering process. 相似文献
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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
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2个火星探测器着陆区均为平原地貌, 但形态特征、物质结构和动力过程都有明显差异。勇士号着陆区主要为风蚀区,而机遇号着陆区主要为风积区;前者为板状砾质平原,后者是基岩出露的波状砂质平原。可能常年有主风向,它们属于无表水环境下极干旱的风成地貌,缺少融冻过程,风化速度远低于地球环境。地貌结构与物质都证明,火星过去曾有液态水存在。限于着陆区环境及探测器功能,如果水存在于地下深部,这两个探测器很难发现。 相似文献
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根据汇水面积、松散物质储量、沟坡坡度、主沟纵坡降等4项泥石流沟易发性判断特征指标,利用数理统计方法,对甘肃省河西地区20个县、区、市的587条泥石流沟现状进行了分析研究. 结果表明：河西地区泥石流多发育在南北山地的前山走廊地带,泥石流沟分布密度稀疏,属于泥石流稀疏地区. 在泥石流沟易发性主要特征指标方面,研究区汇水面积指标处于偏轻微程度,松散物质储量指标处于中等程度,沟坡坡度指标处于严重程度,主沟纵坡降指标处于中等以下程度. 在泥石流沟易发性评价结果方面区域总体属于泥石流地质灾害低易发-中易发区域. 在全球气候变暖的背景下,研究区内强降水情况发生频率呈现增强趋势,应积极开展极端天气影响下河西地区泥石流发展趋势和干旱、半干旱地区植被特征与泥石流易发性之间的相关关系研究. 相似文献
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Joanna Kozakiewicz 《Earth Science Informatics》2018,11(2):257-272
Image analysis methods are commonly employed to determine the size and shape of particles. Although commercial and non-commercial tools enable detection and measurement of grains from images, they do not provide good results in the case of images acquired during extensive in situ Martian investigations. Within the confines of the Mars Exploration Rover (MER) mission and the Mars Science Laboratory (MSL) mission thousands of images of sand grains were captured, and hitherto, they are the only source of ground-truth data on Martian sand particles. Therefore, a new approach is proposed to analyze such images. The semi-automatic algorithm allows fast detection and measurement of the size and shape of Martian grains from images obtained by the Microscopic Imager (MI) and the Mars Hand Lens Imager (MAHLI). The method was evaluated on 76 images of terrestrial and Martian deposits. The results for the terrestrial samples were compared to those from sieve analysis, as well as with ImageJ and Malvern Morphologi G3 systems. The method provides similar results to those from the other methods. It does not have any limitation on the size of grains, and permits separation of touching particles. 相似文献
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ABSTRACT A mudflow-like deposit resting on the bottom of the East Gorgonum Crater (Mars; 37.4°S, 168.0°W) may provide new insight regarding the debate on the existence of water over the Martian surface. Because water in a mudflow is confined to a porous medium, we analyse this case from the perspective of non-equilibrium systems. Fluids confined to porous media behave in a special way, the system being ruled by kinetic restrictions, which alter the expected thermodynamic equilibrium. These non-equilibrium conditions allow the existence of pure liquid water to temperatures as low as − 40 °C, and even less if the system includes brines. Thus, application of the triple point diagram of water on the Martian surface may constitute a simplistic approach if we are dealing with confined, and yet moving, water in the form of a mudflow. We further suggest that the V-shaped channels excavated alongside the mudflow may have been caused by water rejected by syneresis from the moving sediment. We finally indicate that the series of deeply entrenched channels and debris aprons that occur only in the northern half of the crater might be related to the regional slope, which decreases in altitude to the south. 相似文献
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《Sedimentology》2018,65(1):96-122
This paper characterizes the detailed sedimentology of a fluvial sandbody on Mars for the first time and interprets its depositional processes and palaeoenvironmental setting. Despite numerous orbital observations of fluvial landforms on the surface of Mars, ground‐based characterization of the sedimentology of such fluvial deposits has not previously been possible. Results from the NASA Mars Science Laboratory Curiosity rover provide an opportunity to reconstruct at fine scale the sedimentary architecture and palaeomorphology of a fluvial environment on Mars. This work describes the grain size, texture and sedimentary facies of the Shaler outcrop, reconstructs the bedding architecture, and analyses cross‐stratification to determine palaeocurrents. On the basis of bedset geometry and inclination, grain‐size distribution and bedform migration direction, this study concludes that the Shaler outcrop probably records the accretion of a fluvial barform. The majority of the outcrop consists of large‐scale trough cross‐bedding of coarse sand and granules. Palaeocurrent analyses and bedform reconstruction indicate that the beds were deposited by bedforms that migrated towards the north‐east, across the surface of a bar that migrated south‐east. Stacked cosets of dune cross‐bedding suggest aggradation of multiple bedforms, which provides evidence for short periods of sustained flow during Shaler deposition. However, local evidence for aeolian reworking and the presence of potential desiccation cracks within the outcrop suggest that fluvial deposition may have been intermittent. The uppermost strata at Shaler are distinct in terms of texture and chemistry and are inferred to record deposition from a different sediment dispersal system with a contrasting provenance. The outcrop as a whole is a testament to the availability of liquid water on the surface of Mars in its early history. 相似文献
19.
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