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1.
液态水在火星地表的塑造过程中起到了重要的作用,形成了峡谷网、外流河道、古湖泊以及三角洲和冲积扇等多种多样的水成地貌,它们一直是火星探测与研究的热点和焦点.本文对火星水成地貌的探测历史、地形地貌特征、时空分布等方面的研究进展进行总结,探讨水成地貌对火星气候演化及天体生物学研究的指示意义.在此基础上,提出当前火星水成地貌研究存在的问题,认为需要在火星水成地貌的水源类型、水成地貌所指示的火星水环境特征、亚马逊纪水成地貌的成因、火星水成地貌与我国柴达木盆地地貌的类比等方面开展进一步研究,为更深入的认识火星水成地貌,了解火星气候变化及宜居性提供支持. 相似文献
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雅丹地貌是一种典型的风蚀地貌.多源遥感探测和就位探测均表明火星表面分布着大量的雅丹地貌,其形态特征和物质组成记录了火星气候环境变化的信息,是当前火星探测和研究的热点之一.本文对火星雅丹地貌的探测历史、分布、类型、几何特征、物质组成、年代学、发育过程及对古气候指示意义等方面的研究进展进行了总结,在此基础上,提出了当前火星雅丹地貌研究存在的主要问题,建议在未来研究中重点加强雅丹地貌定量化和比较行星学研究,并结合其物质组成、年代学等方面工作,探讨其发育过程与气候环境协同演化的机制,为深入认识火星雅丹地貌发育过程,了解火星古气候环境变化提供支持. 相似文献
3.
火星是太阳系中早期演化历史与地球非常相似的一颗行星,为了解火星的古气候环境以及火星是否存在过生命,火星的水环境历史一直是人们研究的热点问题.本文从火星历史上水对火星表面的改造痕迹介绍了水在火星演化过程中扮演的重要角色.水流、冰川、古湖泊与古海洋等与火星表面地形地貌演化以及矿物岩石形成与迁移过程等密切相关,它们的发育与消失受到火星古气候变迁的影响.关于火星古气候是暖湿还是干冷的问题一直存在争议,但是可以确定至少有短暂且持续的暖湿时期提供了水的活动条件.现今的火星表面寒冷干旱,但是火星的地下储存了冰层甚至可能有地下湖泊.随着近年来火星探测任务越来越频繁,人们将会在火星水演化历史上有更多新的发现. 相似文献
4.
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
5.
湖岸地貌不仅可以与湖相沉积物共同指示湖泊演化过程,同时还是具有较高观赏价值的地貌景观,因此成为重要的地质遗迹。内蒙古克什克腾世界地质公园达里诺尔园区保存了大量的地质遗迹,对湖泊演化及气候变化具有很好的指示意义。本研究从地貌角度出发,对达里诺尔园区代表古湖面的湖蚀穴、湖蚀凹槽、湖蚀柱和湖蚀崖等湖蚀地貌,湖岸堤和湖成阶地等湖积地貌,以及河流地貌和冰缘地貌进行详细的野外地质调查,通过剖面实测并与湖岸沉积物和湖心钻孔岩心进行对比,判断达里湖全新世以来湖水面的变化,进而重建湖泊的演化过程。湖蚀地貌表明,达里湖曾存在4期明显的高湖面,海拔高度分别为1303 m、1296 m、1288 m和1277 m;而在1280 m以下主要发育湖成阶地和湖岸堤等湖积地貌。被称为世界最窄河流耗来河的不断发育代表了湖水位不断下降的过程,古冰楔及其上覆的硅藻土的发育指示了一次湖退和一次湖进事件。该研究对季风边缘区湖泊演化历史的重建可提供参考。 相似文献
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古地貌恢复研究是油气储层预测的重要内容,古地貌恢复的准确性直接影响物源、古水流等沉积特征的判断.针对辽河滩海西部地区钻井分布不均的特点,在钻井资料地层厚度压实校正基础之上,提出利用地震资料进行井间古地貌趋势补偿,将钻井资料和地震资料有机地融合.通过在辽河滩海西部沙一段应用表明,该方法效果良好,能够较真实地反映古地貌分布特征. 相似文献
8.
古洪水事件重建是地貌学与环境变化领域的前沿性课题之一。高山峡谷基岩河段是古洪水重建的理想场所,通过系统梳理国内外文献,评述古洪水事件重建研究进展,认为识别古水位标志(palaeo-stage indicators)、系统建立流域尺度洪水综合地貌证据是古洪水重建的前提和基础。而不同类型的古洪水地貌证据中,古洪水滞流沉积物(slackwater deposits,SWD)是最完整的具有确切水位标志指示意义的高水位悬移质沉积物,而其他边滩坝体(bars)是指示洪水路径和水动力条件的低水位标志沉积物。基于这些洪水地貌证据与水位标志物指示,采用多种水力学模型重建古洪水规模。同时采用多种测年方法相互验证建立可靠完整的古洪水事件年代序列。从点到面建立古洪水事件数据库,提出不同成因类型古洪水事件的时空模式,系统揭示特大洪水发生规律及其演化趋势。其中,青藏高原周缘灾难性古洪水事件在形成年代、地貌证据和水文模拟等方面具有鲜明的时空特征与地貌效应,这些对认识全球末次冰期巨型洪水事件具有重要意义。在特定的时空尺度范围内评估极端洪水事件的地表过程与地貌效应,甚至大陆尺度灾难性古洪水研究已经拓展到行星尺度洪水地貌。此外,高山峡谷现代大洪水地貌原型观测对理解古洪水水文过程机制等具有重要的参考价值。 相似文献
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寻找地外生命是人类开展太阳系探测的根本出发点。火星是太阳系中最可能存在生命的天体之一。尽管海盗号开展的生物科学实验没有获得存在生命的确凿证据,但是近二十年的探测利用高分辨成像、光谱、质谱、雷达、中子分析等多方面的探测手段,获得了河流侵蚀地貌、古湖泊河流沉积物、水成矿物、极地冰盖、大气中水蒸气组分等一系列反映火星上有水的证据。这些发现暗示了火星过去或现在存在适宜生命繁衍的环境特征。大气甲烷、火星样品中有机物是下一步火星生命探测的重点。木星和土星的天然卫星,包括木卫二、土卫二和土卫六等在地外生命的研究中引起极大关注。木卫二上的盐水海洋环境被认为可能孕育生命,海洋中可能存在类似地球上的水热地质作用。土卫二南极存在细粒冰晶的喷射,且喷射物含有对于生命非常关键的液态水、氨气和其他碳氢化合物等。碳质球粒陨石存在大量可溶性有机物,其中包括多种构成蛋白质的氨基酸。星尘号和深度撞击任务的探测结果证实彗星所代表原始物质中含有大量的有机化合物,部分类型的氨基酸在碳质陨石和星际尘埃IDP颗粒相同,进一步支持了彗星与地球生命的起源之间存在联系。文中分析了太阳系生命探测中亟须解决的关键问题,包括系统建立地外生物标志化合物、发展适合太阳系探测的有机物分析技术、开展地球极端生命研究。最后呼吁我国在未来火星等天体探测任务中能增加有机物探测的相关载荷,及时介入太阳系生命探测,开拓深空领域。 相似文献
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柴达木盆地是我国境内首个火星类比区。其中,大柴旦红崖地区被选为中国“火星村”的建设地点。本研究从红崖地区的地质构造背景、气候环境、地形地貌、矿物岩石类型等方面开展了与火星的类比研究。研究表明,红崖地区位于柴达木盆地,其气候环境与干燥寒冷的现代火星类似。红崖核心区及周边具有多种类火星地貌,包括沙丘、河谷、树枝状结构、黑影区域、多边形结构和雅丹地貌等。红崖地区的岩石和土壤中存在多类火星矿物,包括石英、碳酸盐、石膏、石盐、斜长石、碱性长石和绿泥石等。红崖地区可为未来火星探测器和载荷的地面验证试验及相关的科普科教活动等提供天然实验场地。 相似文献
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The complexity of the age dating of the Pleistocene ice-dammed paleolakes in the Altai Mountains is a reason why geologists consider the Early Paleolithic archaeological sites as an independent age marker for dating geological objects. However, in order to use these sites for paleogeographic reconstructions, their locations, the character of stratification, and the age of stone artifacts need to be comprehensively studied. We investigate 20 Late Paleolithic archaeological sites discovered in the Chuya depression of the Russian Altai (Altai Mountains) with the aim of their possible use for reconstructions of the period of development of the Kurai–Chuya glacio-limnosystem in the Late Neopleistocene. The results of our investigation show that it is improper to use the Paleolithic archaeological sites for the dating of the existence period and the draining time of ice-dammed lakes of the Chuya Depression in the modern period of their study owing to a lack of quantitative age estimates, a wide age range of possible existence of these sites, possible redeposition of the majority of artifacts, and their surface occurrence. It is established that all stratified sites where cultural layers are expected to be dated in the future lie above the uppermost and well-expressed paleolake level (2100 m a.s.l.). Accordingly, there are no grounds to determine the existence time of shallower paleolakes. Since the whole stone material collected below the level of 2100 m a.s.l. is represented by surface finds, it is problematic to use these artifacts for absolute geochronology. The Late Paleolithic Bigdon and Chechketerek sites are of great interest for paleogeographic reconstructions of ice-dammed lakes. The use of iceberg rafting products as cores is evidence that these sites appeared after the draining of a paleolake (2000 m a.s.l.). At this time, the location of these archaeological sites on the slope of the Chuya Depression allows one to assume the existence of a large lake as deep as 250 m synchronously with the above paleolake or later. The location of the lowermost archaeological sites is evidence that a paleolake could have existed at an altitude below 1770 m a.s.l. in the Late Neopleistocene–Early Holocene. The absolute geochronology of the archaeological sites (cultural layers in multilayered sites, split surfaces on dropstones, etc.) can be useful for further reconstructions of the existence time, depths, and a number of ice-dammed lakes in the Kurai–Chuya system of depressions. 相似文献
12.
Martian exploration is the focus and hot topic of deep space exploration, and China implemented the first Martian exploration Program in 2020. Aeolian process is the most extensive and active landform process on the surface of Mars, and has been an important part of Martian research. Sustainable development of Martian aeolian geomorphology research requires the support of theoretical system and research methodology, and research methodology is a key issue when field observations are impossible. We analyzed the research methods of Martian aeolian geomorphology from three aspects: methodology, approach, and application of modern technology. Methodology must focus on the dialectical unity of induction and deduction, reductionism and holism. Research approach includes exploration and numerical simulation, and Mars-like aeolian geomorphology study on Earth is also a common approach. Taking full advantage of remote sensing observations and detection technologies is an important basis for the development of Martian aeolian research. Simulation experiments have been an important part of aeolian geomorphology research. Since the 1980s, the United States, Europe, and Japan have successively built Martian wind tunnels to study various aircrafts in Martian atmosphere. In the absence of field observation, wind tunnel experiment and numerical simulation play an important role in studying the evolution and formation process of aeolian landform and the Martian environment. 相似文献
13.
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
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迄今为止,人类已经通过火星轨道探测器、火星着陆器及火星漫游车在火星上发现了碳酸盐、硫酸盐及氯化物等一 系列的盐类矿物,尽管整体上火星盐类矿物组合与地球上基本一致,但在许多细节方面还是和地球上有所不同。文中首先 对于火星盐类认知的现状作了简要综述;基于地球火星蒸发盐沉积及成盐作用规律的对比,预测火星表面及次表面可能存 在着广泛分布的钾盐;此外,发现火星轨道伽玛光谱仪所获的火星表面 K 的分布与火星表面已探测到的氯化物的分布有比 较强的相关性,喻示火星表面氯化物沉积地区的卤水浓度已经接近或达到钾盐形成的条件,同时指出这些地区存在钾盐的 可能性很大。 相似文献
15.
Middle‐Late Pleistocene Glacial Lakes in the Grand Canyon of the Tsangpo River,Tibet 总被引：1，自引：0，他引：1
Many moraines formed between Daduka and Chibai in the Tsangpo River valley since Middle Pleistocene. A prominent set of lacustrine and alluvial terraces on the valley margin along both the Tsangpo and Nyang Rivers formed during Quaternary glacial epoch demonstrate lakes were created by damming of the river. Research was conducted on the geological environment, contained sediments, spatial distribution, timing, and formation and destruction of these paleolakes. The lacustrine sediments 14C (10537±268 aBP at Linzhi Brick and Tile Factory, 22510±580 aBP and 13925±204 aBP at Bengga, 21096±1466 aBP at Yusong) and a series of ESR (electron spin resonance) ages at Linzhi town and previous data by other experts, paleolakes persisted for 691~505 kaBP middle Pleistocene ice age, 75–40 kaBP the early stage of last glacier, 27–8 kaBP Last Glacier Maximum (LGM), existence time of lakes gradually shorten represents glacial scale and dam moraine supply potential gradually cut down, paleolakes and dam scale also gradually diminished. This article calculated the average lacustrine sedimentary rate of Gega paleolake in LGM was 12.5 mm/a, demonstrates Mount Namjagbarwa uplifted strongly at the same time, the sedimentary rate of Gega paleolake is more larger than that of enclosed lakes of plateau inland shows the climatic variation of Mount Namjagbarwa is more larger and plateau margin uplifted more quicker than plateau inland. This article analyzed formation and decay cause about the Zelunglung glacier on the west flank of Mount Namjagbarwa got into the Tsangpo River valley and blocked it for tectonic and climatic factors. There is a site of blocking the valley from Gega to Chibai. This article according to moraines and lacustrine sediments yielded paleolakes scale: the lowest lake base altitude 2850 m, the highest lake surface altitude 3585 m, 3240 m and 3180 m, area 2885 km2, 820 km2 and 810 km2, lake maximum depth of 735 m, 390 m and 330 m. We disclose the reason that previous experts discovered there were different age moraines dividing line of altitude 3180 m at the entrance of the Tsangpo Grand Canyon is dammed lake erosive decay under altitude 3180 m moraines in the last glacier era covering moraines in the early ice age of late Pleistocene, top 3180 m in the last glacier moraine remained because ancient dammed lakes didn’t erode it under 3180 m moraines in the early ice age of late Pleistocene exposed. The reason of the top elevation 3585 m moraines in the middle Pleistocene ice age likes that of altitude 3180 m. There were three times dammed lakes by glacier blocking the Tsangpo River during Quaternary glacial period. During other glacial and interglacial period the Zelunglung glacier often extended the valley but moraine supplemental speed of the dam was smaller than that of fluvial erosion and moraine movement, dam quickly disappeared and didn’t form stable lake. 相似文献
16.
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
17.
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。 相似文献
18.
The suggestion that radon could be used as a radioactive tracer of regolith-atmosphere exchanges and as a proxy for subsurface water on Mars, as well as its indirect detection in the Martian atmosphere by the rover Opportunity, have raised the need for a better characterization of its production process and transport efficiency in the Martian soil. More specifically, a proper estimation of radon exhalation rate on Mars requires its emanation factor and diffusion length to be determined. The dependence of the emanation factor as a function of pore water content (at 267 and 293 K) and the dependence of the adsorption coefficient on temperature, specific surface area and nature of the carrier gas (He, He + CO2) have been measured on a Martian soil analogue (Hawaiian palagonitized volcanic ash, JSC Mars-1), whose radiometric analysis has been performed. An estimation of radon diffusion lengths on Mars is provided and is used to derive a global average emanation factor (2-6.5%) that accounts for the exhalation rate inferred from the 210Po surface concentration detected on Martian dust and from the 214Bi signal measured by the Mars Odyssey Gamma Ray Spectrometer. It is found to be much larger than emanation factors characterizing lunar samples, but lower than the emanation factor of the palagonite samples obtained under dry conditions. This result probably reflects different degrees of aqueous alteration and could indicate that the emanation factor is also affected by the current presence of pore water in the Martian soil. The rationale of the “radon method” as a technique to probe subsurface water on Mars, and its sensitivity to soil parameters are discussed. These experimental data are useful to perform more detailed studies of radon transport in the Martian atmosphere using Global Climate Models and to interpret neutron and gamma data from Mars Odyssey Gamma Ray Spectrometer. 相似文献