基于地震多属性融合的断层识别与评价——以塔里木盆地SHB地区碳酸盐岩缝洞型储层为例

塔里木盆地SHB地区的深部碳酸盐岩缝洞型储层主要发育于断裂破碎带,大多表现为断裂破碎形成的裂缝和后期溶蚀形成相互连通的断溶体.因此,断层的识别与精细评价成为该区缝洞型储层识别评价的基础.考虑到研究区处于沙漠腹部,深部地层的地震反射能量相对较弱,用单一地震属性难以实现断裂带的识别.本文针对研究区地震资料的地质-地球物理特...     

缝洞型储层随钻测井自适应有限元法数值模拟

缝洞型碳酸盐岩储层具有强烈的非均质性及储集空间预测难度大的特点,利用随钻电阻率测井方法对缝洞进行准确识别和划分,是当前研究的热点问题.利用一种先进的高精度自适应有限元方法和几何精确的曲边单元造型技术可以模拟缝洞型储层的随钻测井响应.本文通过研究仪器在不同半径缝洞的模拟测井响应及缝洞填充与坍塌导致的机械填充对测井结果的影响,给出了用于识别缝洞大小和填充程度的缝洞型储层的测井响应特征.研究结果为缝洞型碳酸盐岩储层的识别与划分提供了理论依据.     

基于地震成像数据稀疏反演的不连续及非均质地质体检测方法

本文针对油气藏储层预测中的不连续及非均质地质信息识别问题,研究基于地震成像数据的稀疏反演方法.由于该类地质体的地震响应特征为弱信号,因此利用平面波破坏滤波器由地震成像数据中去除强反射同相轴.在此基础上,对剩余的地震数据进行非线性加强滤波,并构建L1稀疏反演模型.为有效求解L1模型,采用非光滑泛函L1范数逼近和拟牛顿求解算法.该方法考虑稀疏先验信息,能够提高反演结果信噪比.缝洞模型测试验证该方法在检测断点、微断裂、散射点等小尺度地质体上的有效性,塔北缝洞型碳酸盐岩储层预测的应用效果进一步证实该方法的实用性.     

青西油田碳酸盐岩裂缝性储层地球物理预测技术的应用

白云岩成岩收缩晶间孔、洞、缝与构造网状缝相互沟通可以组成良好的油气储层，但是这种复杂裂缝—孔隙型储层分布随机性强、发育程度和差异性大，储层预测难度大。本文以中国西部酒泉盆地青西油田下白垩统下沟组湖相白云岩裂缝—孔隙型储层为例，提出地球物理综合预测碳酸盐岩裂缝的方法。本文描述了综合地球物理方法预测碳酸盐岩裂缝储层的实施和应用效果。     

碳酸盐岩岩溶型储层综合预测

塔里木盆地碳酸盐岩岩溶型储层广泛分布于塔北、塔中、巴楚等地区，是塔里木盆地碳酸盐岩勘探的重点，也是塔里木油田增储上产的主要层系之一。由于埋藏深度大、反射信号较弱、信噪比较低，更由于岩溶型储层非均质性严重，使得储层预测的难度增大。通过多年的攻关研究，从碳酸盐岩风化壳储层的地球物理响应特征出发，逐步探索并建立了技术、岩溶型储层测井评价技术、岩溶型储层地震描述技术、应变量分析技术为手段的溶型储层综合评价技术。在塔北、以地质概念模型为基础，以基于层序格架的潜山古地貌恢复塔中等地区应用中取得了良好的地质效果，相继获得了工业油气流。本文介绍了该技术在塔北轮古西地区的具体实施和应用效果。     

最小二乘逆时偏移在碳酸盐岩缝洞型储层成像中的应用

碳酸盐岩缝洞型储层是我国西部探区重要的储层,包含较多的孔、洞、缝,其波场信息复杂,常规偏移成像对其成像效果不佳,这已成为制约勘探发展的重要因素.为此本文推导并实现了基于反演思想的高精度最小二乘逆时偏移成像方法,并将其推广应用到碳酸盐岩缝洞型储层.通过对三个基于西部探区实际地质情况建立的典型模型的成像试算,可以发现:与常规逆时偏移结果进行对比,最小二乘逆时偏移能够准确的刻画出裂缝溶洞的位置、形状、大小,验证了该方法在碳酸盐岩缝洞型复杂地质模型的保幅性和成像精度方面的优势.     

南中国海深水区典型火山发育地震反射特征研究

海洋油气勘探尤其是深水勘探面临着三高难题——高成本、高风险、高技术.如何对储层进行准确预测,是地球物理工作者及地球物理技术亟待解决的问题.本文对火山机构喷发机理及其地球物理特征进行分析,结合邻近工区在火山发育特征规律的认识成果,针对南中国海深水区目标区内典型火山发育,运用常规地震时间切片、剖面分析及沿层均方根振幅属性和沿层小时窗三维地震镂空显示等技术,分析了目标火山发育情况、火山岩喷溢情况、地震反射特征及岩相分布,并建立了该类型火山发育特征、岩相分布规律以及空间展布规律及变化特征的认识.本文的研究成果为该地区准确识别火山发育及预测其分布规律提供了参考,尤其是在钻井少的情况下进行地质异体常识别和储层预测,有利于该地区石油天然气勘探工作以及区域地质认识.     

阵列声波测井处理新技术在碳酸盐岩储层评价方面的应用

为了更深入的研究阵列声波测井资料在缝洞型碳酸盐岩储层评价中的应用,针对阵列声波中不同探测距离、不同分辨率的信息开发了三种新技术.通过对纵波进行频散分析形成了纵波频散谱的处理方法,并建立了根据频散谱的方差对碳酸盐岩储层非均质性进行评价的方法,对于井周裂缝、溶洞的识别及储层类型划分有指导意义;利用井壁斯通利波传播特性,建立了定量计算斯通利波能量衰减的方法,对于评价过井缝洞有重要作用;利用阵列声波反射波信息形成了全新的声波远探测处理方法,通过对井旁反射信息的定量表征建立了井旁缝洞发育程度的定量评价方法.阐述了这些方法的基本原理及适用条件,拓展了阵列声波测井资料在碳酸盐岩储层评价方面的应用.     

准噶尔盆地腹部隐蔽油气藏物理模拟及地震响应特征

准噶尔盆地腹部侏罗系以隐蔽油气藏为主,地震资料在目的层分辨率较低、地震反射特征不清晰,制约了对该区的低幅构造、岩性圈闭的识别和评价.本文根据侏罗系的沉积特点,建立河流、（扇）三角洲沉积体系地质模型,制作尖灭体、透镜体、河道砂、浊积体等地质体的三维物理模型,通过实验测试方法,研究地层条件下岩石物理性质的变化特征,系统研究储层地球物理参数变化的总体规律,并结合测井资料,采用波场物理模拟方法,研究波场响应特征与储层参数变化之间的规律,分析各种情况下的波场特征、属性特征.     

涪陵地区飞仙关组储层地球物理响应特征及正演模拟

涪陵地区位于"开江-梁平海槽"西侧,存在发育高能相带的地质背景,飞仙关组主要发育白云岩储层和鲕粒灰岩或颗粒灰岩储层.采用地质-地球物理互馈结合的方法,对该区飞仙关组储层开展了地球物理响应特征及正演模拟的研究,结果表明:白云岩储层速度相对致密白云岩有所降低,降低幅度有限,仍高于致密灰岩,在地震剖面上表现为低频强振幅特征;地震响应分析结果显示,迭瓦状前积之上的波谷反射可能是鲕粒灰岩或颗粒灰岩储层发育的有利位置,正演模拟证实,滩顶对应波谷,滩底对应波峰,孔隙发育差异和储层厚度的不同造成振幅强弱有别,滩体延伸长度的不同,可分别形成长轴状与短轴状迭瓦状前积,滩体叠置地方振幅减弱.通过地震异常平面规律的刻画,认为长轴状强振幅迭瓦状前积在研究区最有利,是优先考虑的勘探有利区.     

Point-defect formation parameters in olivine

The formation internal energy and volume of the point-defect species in olivine are derived for a number of approximate charge-neutrality conditions. The formation parameters of an effectively charged point defect are a function of the approximate condition of charge neutrality. Since the approximate charge-neutrality condition depends upon the partial pressure of oxygen and the activity of enstatite in olivine, changes in the magnitude of these thermodynamic-state variables result in different values of the formation parameters if the charge-neutrality regime is altered. The fractional change in the formation internal energies of the energetically unfavorable defects, such as Si vacancies, is small between the charge-neutrality regions while the fractional change for the favorable defects, such as Mg vacancies, is large.     

Core formation in terrestrial planets

Calculations of the radial distribution of the energy released in core formation indicate that the cores of all the terrestrial planets may be expected to receive a disproportionate share of the gravitational energy released. Since the model of the process used in these calculations favors transfer of energy to the mantle, it is likely that other reasonable models of the process will result in even more energy being deposited in the cores of the early planets. The calculations also show that it is necessary for a certain amount of core phase to separate and accumulate, before the energy released by gravitational settling is sufficient to supply the latent heat of fusion of the core phase. The amount of melting required to reach this point varies according to the total mass of the planet, and mass fraction of core, but is not particularly great (<5% for the Earth to ～ 37% for the Moon). In the case of the Moon, this amount of segregation, although large, amounts to a surface layer about 260 km thick, similar to the proposed depth of early wholesale melting. Core separation in terrestrial planets appears to be a self-sustaining process even for fairly small bodies, provided that a small amount of a dense potential core phase is present. Although it seems likely to occur rapidly (within 10⁶–10⁷ years) even for small (Moon-size) bodies, detailed kinetic models will be necessary to specify the time scale.     

Star formation timescales in M82

Richard de Grijs reviews the picture of starbirth presented in this nearby, prototype starburst galaxy, a well-studied example of processes that must be widespread in the early universe.
The last tidal encounter between M82 and M81, some 500 Myr ago, had a major impact on what was probably an otherwise normal, quiescent disk galaxy. It caused a concentrated burst of star formation in the form of massive star clusters that decreased rapidly, within a few 100 Myr. The current starburst in the centre of the galaxy is likely to arise from large-scale propagating star formation. Alternatively, it may be related to late infall of tidally disrupted debris from M82 itself. Star formation here overall may, in fact, come from a combination of these two mechanisms, in the sense that the star formation in the active core is actively propagating, whilst the overall evolution of the starburst depends on tidal debris raining back onto the disk of the galaxy, giving rise to the present-day starburst.     

Diamond formation in metal–carbonate interactions

Reduced silicon alloyed with Fe metal was shown to chemically react with FeCO₃ siderite at pressures of 10–25 GPa and temperatures of 1700–1800 °C according to2 FeCO_{3 siderite}+3 Si _{in metal}=2 Fe _{in metal}+3 SiO2 stishovite+2 C_diamondSince no carbon seeds were introduced, the only source of carbon for diamond formation was the carbonate phase. This observation provides a mechanism of diamond formation, possibly relevant to the early Earth. Thermodynamic modelling of the observed reactions shows that the stishovite/silicon oxygen fugacity buffer is far more reducing than the carbonate/diamond equilibrium, implying that, at Earth mantle conditions, no silicon-bearing metal can coexist with carbonates. Diamond formation by reactions between carbonates and highly reducing metal phases containing significant amounts of silicon might have occurred in the early Earth upon mixing of oxidized and reduced accretion components at pressures and temperature exceeding 10 GPa and 1700 °C.     

Crater formation in soils by raindrop impact

The process of crater formation by the impact of water drops on soil, sand and various other target material was studied. Craters of various shapes and sizes were observed on different target materials or conditions, ranging from circumferential depression to completely hemispherical shape. Crater shape was dependent upon target material, its ?ow stress or shear strength and the presence and thickness of water on the surface. Between 5 and 22 per cent of impact energy was spent on cratering, but the relationship between crater volume and kinetic energy of a raindrop was curvilinear, indicating a lower ef?ciency of impact energy in removing target material as the energy increases. Impact impulse, on the other hand, showed a more linear relationship with crater volume, and the ratio of impulse over crater volume (I/V) remained constant for the entire range of drop sizes, impact velocities, and surface conditions used in this study. Surface shear strength, represented by the penetration depth of fall‐cone penetrometer, appeared to be a key factor involved in this process. An equation was developed which related crater volume to cone penetration depth and impact impulse. Crater volume, which appeared to be a better indicator of the total amount of material dislodged by a raindrop than splash amount, can thus be predicted using this equation. Copyright © 2004 John Wiley & Sons, Ltd.     

Pathways of birnessite formation in alkali medium

Birnessite, widely distributed in soils, sediments and ocean manganese nodules, is a common layered manganese oxide. It consists of sheets of hydrated cations between sheets of MnO6 octahedra[1,2]. The formations of a variety of manganese oxides are closely related with birnessite, most of those form di- rectly or indirectly from birnessite [3―7]. In natural en- vironment, birnessite has a high surface activity and potential, and plays a significant role in adjusting and controlling the avai…     

The formation of deep topsoils in Orkney

The Soil Survey for Scotland, in their mapping of the soils in Orkney, identified a deep top phase of the Bilbster Series. This soil is distinguished by having a topsoil usually in excess of 75 cm and it occurs almost exclusively on the Mainland of Orkney, especially in the west round Marwick and Skaill Bays. An anthropogenic origin to this soil is proposed and the present study is designed to investigate the particular processes of formation which have led to the increase in soil depth. Results from transect and grid surveys indicate how the soil is thickest adjacent to old farms. The historical literature suggests a wide range of possible inputs from seaweed and calcareous sand to turves after they had been used as bedding for cattle. Analytical results support the last process as the dominant one and an accumulation rate of c.1 mm/yr is proposed.     

Iron oxide formation in artificial ground waters

Artificial ground water containing 40 mg/l Ca and varying concentrations of Fe(II), Fe(III) and Si were rapidly oxidized with air. The ferrihydrite forming is similar to those found in natural Finish ground waters.     

Effects of core formation

Two sets of earth models have been generated which simulate the process of core formation in the earth. The results allow the evaluation of the distribution of energy release by core formation and thus an estimate of the early temperature profile following core formation. The process itself is likely to have taken 20 Ma or less, although a longer induction period during which some metal phase exists as a melt is probable. Much of the energy (half or more) ends up in a hot core with the mantle relatively cold. These results suggest the occurrence of mantle wide convection, leading to homogenization and the possible stripping of some elements from the mantle.