Thick and thin models of the evolution of carbon dioxide on Mars     

Curtis V. Manning  Christopher P. McKay 《Icarus》2006,180(1):38-59

We present results from a new simulation code that accounts for the evolution of the reservoirs of carbon dioxide on Mars, from its early years to the present. We establish a baseline model parameter set that produces results compatible with the present (i.e., Patm?6.5 mbar with permanent CO₂ ice cap) for a wide range of initial inventories. We find that the initial inventory of CO₂ broadly determines the evolutionary course of the reservoirs of CO₂. The reservoirs include the atmosphere, ice cap, adsorbed CO₂ in the regolith, and carbonate rocks. We track the evolution of the free inventory: the atmosphere, ice cap and regolith. Simulations begin at 4.53 Gyr before present with a rapid loss of free inventory to space in the early Noachian. Models that assume a relatively small initial inventory (?5 bar) have pronounced minima in the free inventory of CO₂ toward the end of the Noachian. Under baseline parameters, initial inventories below ∼4.5 bar result in a catastrophic loss of the free inventory to space. The current free inventory would be then determined by the balance between outgassing, sputtering losses and chemical weathering following the end of the late bombardment. We call these “thin” models. They generically predict small current free inventories in line with expectations of a small present CO₂ ice cap. For “thick” models, with initial inventories ?5 bar, a surplus of 300-700 mbar of free CO₂ remains during the late-Noachian. The histories of free inventory in time for thick models tend to converge within the last 3.5 Gyr toward a present with an ice cap plus atmospheric inventory of about 100 mbar. For thick models, the convergence is largely due to the effects of chemical weathering, which draws down higher free inventories more rapidly than the low. Thus, thick models have ?450 mbar carbonate reservoirs, while thin models have ?200 mbar. Though both thick and thin scenarios can reproduce the current atmospheric pressure, the thick models imply a relatively large current CO₂ ice cap and thin models, little or none. While the sublimation of a massive cap at a high obliquity would create a climate swing of greenhouse warming for thick models, under the thin model, mean temperatures and pressures would be essentially unaffected by increases in obliquity.  相似文献   

Loss of water from Mars:: Implications for the oxidation of the soil     

H. Lammer  H.I.M. Lichtenegger  I. Ribas  E.F. Guinan  S.J. Bauer 《Icarus》2003,165(1):9-25

The evolution of the martian atmosphere with regard to its H₂O inventory is influenced by thermal loss processes of H, H₂, nonthermal atmospheric loss processes of H⁺, H₂⁺, O, O⁺, CO₂, and O₂⁺ into space, as well as by chemical weathering of the surface soil. The evolution of thermal and nonthermal escape processes depend on the history of the intensity of the solar XUV radiation and the solar wind density. Thus, we use actual data from the observation of solar proxies with different ages from the Sun in Time program for reconstructing the Sun's radiation and particle environment from the present to 3.5 Gyr ago. The correlation between mass loss and X-ray surface flux of solar proxies follows a power law relationship, which indicates a solar wind density up to 1000 times higher at the beginning of the Sun's main sequence lifetime. For the study of various atmospheric escape processes we used a gas dynamic test particle model for the estimation of the pick up ion loss rates and considered pick up ion sputtering, as well as dissociative recombination. The loss of H₂O from Mars over the last 3.5 Gyr was estimated to be equivalent to a global martian H₂O ocean with a depth of about 12 m, which is smaller than the values reported by previous studies. If ion momentum transport, a process studied in detail by Mars Express is significant on Mars, the water loss may be enhanced by a factor of about 2. In our investigation we found that the sum of thermal and nonthermal atmospheric loss rates of H and all nonthermal escape processes of O to space are not compatible with a ratio of 2:1, and is currently close to about 20:1. Escape to space cannot therefore be the only sink for oxygen on Mars. Our results suggest that the missing oxygen (needed for the validation of the 2:1 ratio between H and O) can be explained by the incorporation into the martian surface by chemical weathering processes since the onset of intense oxidation about 2 Gyr ago. Based on the evolution of the atmosphere-surface-interaction on Mars, an overall global surface sink of about 2×10⁴² oxygen particles in the regolith can be expected. Because of the intense oxidation of inorganic matter, this process may have led to the formation of considerable amounts of sulfates and ferric oxides on Mars. To model this effect we consider several factors: (1) the amount of incorporated oxygen, (2) the inorganic composition of the martian soil and (3) meteoritic gardening. We show that the oxygen incorporation has also implications for the oxidant extinction depth, which is an important parameter to determine required sampling depths on Mars aimed at finding putative organic material. We found that the oxidant extinction depth is expected to lie in a range between 2 and 5 m for global mean values.  相似文献   

黄、渤海海岸风沙地貌类型及其分布规律和发育模式   总被引：24，自引：0，他引：24  

傅命佐  徐孝诗  徐小薇 《海洋与湖沼》1997,28(1):56-65

于１９９０－１９９４年，对黄，渤海海岸风沙地貌，风沙沉积，风沙灾害和土地沙漠化现象进行详细的外业调查，测量和填图，在此基础上，利用ＧＩＳ技术原理，对海岸岗沙地貌进行系统的分类研究，对海岸风沙地貌分布规律和发育模式进行较深入的探讨，结果表明，研究区风沙地貌，风沙灾害和土地沙漠化现象主要分布在冬，春季气候干旱，风力强而持久，砂源丰富的渤海海岸和山东半岛半岸的砂质海岸地区，海岸沙丘和风成砂地总面积达７０  相似文献   

四川盆地南部中—上寒武统储层成岩作用   总被引：1，自引：0，他引：1  

杨伟  胡明毅  宋海敬  胡治华 《海相油气地质》2008,13(4)

四川盆地南部中—上寒武统(洗象池群)储层为一套碳酸盐岩局限台地沉积,其岩性为粗粉晶—细晶白云岩、砾屑白云岩、砂屑白云岩、鲕粒白云岩等。成岩作用主要有压实作用、胶结作用、白云石化作用、岩溶作用、破裂作用等,白云石化作用和岩溶作用是形成优质储层的关键。白云石化的机理为混合水白云石化。岩溶作用具有多期性,包括沉积期岩溶、风化期岩溶、埋藏期古岩溶和褶皱期古岩溶等,以风化期岩溶为主。压实作用和胶结作用破坏了大量的原生孔隙和次生孔隙。压实作用主要发生在浅埋藏期,它与埋藏期胶结一同作用使孔隙度由原来的15%左右骤降至2%～3%左右。随着后来的岩溶作用和破裂作用等,部分储层的孔隙度又扩大到4%～5%左右,以晶间孔和晶间溶孔为主要储集空间类型。  相似文献   

Origin and thermal evolution of icy satellites     

Angioletta Coradini  Costanzo Federico  Olivier Forni  Gianfranco Magni 《Surveys in Geophysics》1995,16(4):533-591

The paper reviews the problem of formation and evolution of the so-called regular satellites of the giant planets, and it consists of two parts: the first describes the possible origin of the satellites, the second studies their evolution, attempting to stress the relations of the present status of the satellites with their evolutionary history.The formation of regular satellite systems around giant planets is probably related to the formation of the central planet. Some characteristics of regular satellite systems are quite similar, and suggest a common origin in a disk present around the central body. This disk can originate through different mechanisms which we will describe, paying attention to the so-called accretion disk model, in which the satellite-forming material is captured. The disk phase links the formation of the primary body with the formation of satellites. The subsequent stages of the disk's evolution can lead first to the formation of intermediate size bodies, and through the collisional evolution of these bodies, to the birth of satellite embryos able to gravitationally capture smaller bodies.Given the scenario in which icy satellites may be formed by homogeneous accretion of planetesimals made of a mixtures of ice and silicates, if no melting occurs during accretion, the satellites have a homogeneous ice-rock composition. For the smaller satellites this homogeneous structure should not be substantially modified; only sporadic local events, such as large impacts, can modify the surface structure of the smaller satellites. For the larger satellites, if some degree of melting appears during accretion, a differentiation of the silicate part occurs, the amount of differentiation and hence the core size depending on the fraction of gravitational potential energy retained during the accumulation process. Melting and differentiation soon after the accretion, for the larger satellites, could also depend on the convective evolution in presence of phase transitions and generate an intermediate rock layer, considerably denser than the underlying, still homogeneous core, and unstable to overturning on a geologic time scale. Moreover the liquid water mantle could be a transient feature because the mantle would freeze over several hundred million years. For these large bodies the stable configuration is expected to be one consisting of a silicate core and a mantle of mixed rock and ice.  相似文献   

我国高碘卤水分布规律及其形成          下载免费PDF全文

孙大鹏 《盐湖研究》2006,14(2):7-16

根据国内外大量实际资料,从碘的分布情况及其所处的地质条件,结合石油和天然气形成过程、油气藏类型及其分布特点,探讨高碘卤水分布的规律及其形成条件,在此基础上指出了我国的找碘方向。  相似文献   

苍山5.2级地震异常群体时空演化特征   总被引：1，自引：0，他引：1  

刁守中  刘西林  华爱军 《东北地震研究》2002,18(2):1-9

在对 1 995年山东省苍山 5 2级地震异常筛选的基础上 ,分析了异常群体阶段性演化过程。结果表明 ,震前 1 0a左右震中周围出现小震小区域综合断层面解主压应力P轴偏转 (约 3 0°) ,震前 7a左右震中附近 3～ 4级地震增强集中及应变释放加速 ;震前 4a左右转为异常平静 ;震前 1a左右震中外围开始出现形变类前兆异常 ,前兆异常台站比和异常台项比约达 6%及 4%左右 ,异常比例偏少 ;震前约半年起 ,以震中附近地震波速比异常出现为起点 ,相继出现各类前兆异常 6条 ,短期前兆异常台站比和异常台项比分别约达 2 5 %和 1 7%左右 ,显示孕震进入短期阶段 ,但临震异常不明显。对由此获得的 5级地震预测启示进行了讨论。  相似文献   

非线性地球物理反演方法:回顾与展望   总被引：19，自引：13，他引：19  

杨文采 《地球物理学进展》2002,17(2):255-261

自20世纪90年代以来，非线性地球物理反演方法已走向成熟，这些方法包括线性化迭代法，仿真淬火法，遗传算法及联合反演方法等，线性化迭代反演基于开放物理系统状态发生相变的原理，要进一步改善模型参数化的技术和迭代过程的自组织；仿真淬火法与遗传算法基于自然过程的指数率或生物演化的优生率，可以相互结合以提高解估计的分辨率与置信度；联合反演要结合岩石物理性质的统计规律，才能取得兼容地质与综合方法的应用效果，地球动力学中的反问题不仅涉及偏微分方程系数项的求解，而且涉及初始条件或初始边界的求解，对地球动力学作用过程研究特别重要。  相似文献   

从化石记录看古人类起源和演化     

钱迈平 《江苏地质》2003,27(2):65-77,F003,T001,T002

古人类的起源及演化是一个极其复杂而远未解决的问题，目前掌握的重要化石材料包括：距今约5600万年的灵长类，约1700万年的人猿超科代表，620万年(?)-440万年的人科动物，以及约350万年(?)-200万年的古人类和人造石器等。中国是世界上古人类及与之演化相关的化石发现最多的国家之一，先后找到已知最早的高级灵长类——约4500万年前的曙猿化石，人猿超科的早期代表——l400万年和800万年前的古猿化石，240万年-200万年前的人造石器，200万年前的能人(?)化石，170万年前的直立人及28万年-20万年前的智人化石等。拟从迄今的化石记录人手勾勒出古人类起源及演化的大致轮廓。  相似文献   

A methane fuse for the Cambrian explosion: carbon cycles and true polar wander   总被引：1，自引：0，他引：1  

Joseph L. Kirschvink  Timothy D. Raub 《Comptes Rendus Geoscience》2003,335(1):65-78

The dramatic diversification of animal groups known as the Cambrian Explosion (evolution's ‘Big Bang’) remains an unsolved puzzle in Earth Science. The Vendian–Cambrian interval is characterized by anomalously high rates of apparent plate motion, interpreted as True Polar Wander (TPW), and by more than a dozen large, high-frequency perturbations in carbon isotopes that dwarf all others observed through the past 65 million years. We suggest that these biological, tectonic, and geochemical events are intimately related in the following fashion. First, tropical continental margins and shelf-slopes which formed during fragmentation of the supercontinent Rodinia accumulated massive quantities of isotopically-light organic carbon during Late Neoproterozoic time, as indicated by strikingly heavy isotope ratios in inorganic carbon during interglacial intervals. Second, an initial phase of Vendian TPW moved these organic-rich deposits to high latitude, where conditions favored trapping biogenic methane in layers of gas hydrate and perhaps permafrost. Continued sedimentation during Late Vendian time added additional hydrate/gas storage volume and stabilized underlying units until the geothermal gradient moved them out of the clathrate stability field, building up deep reservoirs of highly pressurized methane. Finally, a burst of TPW brought these deposits back to the Tropics, where they gradually warmed and were subjected to regional-scale thermohaline eddy variation and related sedimentation regime changes. Responding to the stochastic character of such changes, each reservoir reached a critical failure point independently at times throughout the Cambrian. By analogy with the Late Paleocene Thermal Maximum event, these methane deposits yield transient, greenhouse-induced pulses of global warming when they erupt. Temperature correlates powerfully with biodiversity; the biochemical kinetics of metabolism at higher temperature decrease generation time and maintain relatively rich and dense invertebrate populations. Repeated thermal pulses along with progressive disruption and alteration of global ocean circulation patterns by TPW could cause the increase in diversity that accompanied the radiation of metazoans. We suggest that a methane ‘fuse’ ignited the Cambrian Evolutionary Explosion.  相似文献