岩石电学性质实验研究方向展望

分析了岩心电性实验的内涵,介绍了油藏条件下岩石电学性质的研究现状以及对岩心电性实验方法的冲击.结合目前对不同地层特性岩石的电学性质的认识,就复杂储层评价的岩心电性实验方法、岩心电性实验技术装备、岩心电性实验技术规范化、岩心数值实验方法等方面对岩心电性实验的研究方向做了展望,认为：①岩心电性实验方法应立足于储层岩石的岩性、物性、孔隙结构、非均质性等地层特性;②系统地模拟和控制储层的温度、压力、润湿性条件、毛管与电性平衡等油藏条件,并使各种相关技术规范化,是其发展的必然趋势;③岩心数值实验方法可能作为实验室岩心电性实验的辅助手段之一在储层含油性评价中发挥作用.     

煤层气成藏的宏观动力能条件及其地质演化过程--以山西沁水盆地为例

煤层气成藏维系于其能量平衡系统,宏观上受控于“四场互动”过程,核心是能量的有效传递及其地质选择过程。以沁水盆地为例,对构造动力能、热动力能、地下水动力能等宏观动力能的地质演化过程进行了深入探讨,阐明了不同宏观动力能对煤层气成藏的控制作用。结果表明:研究区构造动力能及其演化总体经历了4个阶段;热动力能及其演化和由其控制的煤化作用同样经历了4个阶段;地下水动力能及其演化包括3个阶段。其中,燕山中期的剧烈岩浆活动是宏观动力能条件演化的关键时期。以构造动力能为主线,将其他能量场贯穿起来,可知宏观动力能与煤层气成藏之间的耦合关系如下:盆地北部阳泉—寿阳区域,是煤层气成藏有利区域之一,但不利于煤层气高产;盆地南部晋城—阳城及沁水北部区域,不仅是煤层气成藏有利区域,而且利于煤层气高产;盆地中部沁源地区是煤层气成藏和高产的有利区域;盆地东部的屯留—襄垣区域是煤层气成藏有利区域之一,但不利于煤层气高产。     

Diagenesis and Restructuring Mechanism of Oil and Gas Reservoir in the Marine Carbonate Formation,Northeastern Sichuan:A Case Study of the Puguang Gas Reservoir

Abstract: Based on the technology of balanced cross-section and physical simulation experiments associated with natural gas geochemical characteristic analyses, core and thin section observations, it has been proven that the Puguang gas reservoir has experienced two periods of diagenesis and restructuring since the Late Indo-Chinese epoch. One is the fluid transfer controlled by the tectonic movement and the other is geochemical reconstruction controlled by thermochemical sulfate reduction (TSR). The middle Yanshan epoch was the main period that the Puguang gas reservoir experienced the geochemical reaction of TSR. TSR can recreate the fluid in the gas reservoir, which makes the gas drying index higher and carbon isotope heavier because C2+ (ethane and heavy hydrocarbon) and 12C (carbon 12 isotope) is first consumed relative to CH4 and 13C? (carbon 13 isotope). However, the reciprocity between fluid regarding TSR (hydrocarbon, sulfureted hydrogen (H2S)?, and water) and reservoir rock results in reservoir rock erosion and anhydrite alteration, which increases porosity in reservoir, thereby improving the petrophysical properties. Superimposed by later tectonic movement, the fluid in Puguang reservoir has twice experienced adjustment, one in the late Yanshan epoch to the early Himalayan epoch and the other time in late Himalayan epoch, after which Puguang gas reservoir is finally developed.     

川西马鞍塘组礁滩特征和含油气性初探

四川盆地西缘上三叠统马鞍塘组发育一套礁滩组合,部分推覆到地表,部分埋藏在地下。研究表明,这套礁滩有丰富的油源条件,有一定的储集能力、良好的圈闭条件,是油气富集的非常有利的区域,虽然受到多期构造运动的改造,但不能排除地下存在油气藏的可能性,因此有油气勘探的潜力。     

南海张裂过程及其对晚中生代以来东南亚构造的启示——IODP建议书735-Full介绍

南海的形成揭示了大陆边缘张裂和盆地形成的复杂模式,尽管已经进行了广泛研究,但是关于基底岩石和深海盆沉积层的精确年代数据还很缺乏,这使得对南海张裂年代的估计存在很大的误差,对张裂机制和历史的各种假设没有得到验证.同时只有对南海的张裂过程有了精确地分析与刻画,才能更好地理解西太平洋边缘海盆地的形成以及它们在印支块体受印度-欧亚板块碰撞而向东南挤出、青藏高原隆升中可能起到的作用.2009年正式提交的国际综合大洋钻探计划(IODP)建议书735-Full建议在南海深海盆内的4个站位上实施钻探.这4个站位分布在南海盆地4个不同的次级构造单元上(南海东北部、西北次海盆、东部次海盆和西南次海盆),这样的站位设计会确保完成本建议书的整体研究目标,即揭示南海的张裂历史和它对晚中生代以来东南亚构造的启示.位于南海盆地最东北部的站位有助于确定该区域地壳的属性和验证古南海是否存在,位于西北次海盆的站住可能会提供南海的最早张裂年代,另外2个分别位于东部次海盆和西南次海盆的站位将重点确定2个次海盆的绝对年龄、基底矿物成分与磁化率以及2个次海盆的相对张裂次序.这些站位的水深大约在2 910～4 400 m,钻探深度预计到海底以下大约700～2 200 m,总的钻透深度为5 959 m,其中5 359 m穿透沉积层,另外600 m或400 m钻入基底.所有这些站位的位置是由已有的地球物理观测数据所确定,目前计划收集更多的地质与地球物理数据以满足IODP对井位调查数据的要求.     

黄土高原泥流灾害成因及特征

黄土泥流是戴土地区一类重要的灾害地貌过程,是泥石流的一个特殊类型,是水土流失的一种特殊形式,也是山地环境恶化、水土流失极严重的标志。本文在对黄土泥流这一黄土高原特有的严重水土流失现象的分布、成因、物质组成、动静力学性质、堆积形态等全面系统研究的基础上,对其和一般泥石流与高含沙水流做了初步对比和分析,揭示了黄土泥流灾害的形成规律、运动机制和沉积特征。     

流体包裹体在油气地质地球化学中的应用

流体包裹体研究是油气形成和成藏定量化研究的重要手段。本文总结了油气藏中流体包裹体的地质地球化学意义及其在石油、天然气研究中的应用,探讨了烃源岩和储层流体包裹体在确定源岩演化、沉积环境、有机母质类型、成熟度、油气运移充填期次等方面的应用,指出目前流体包裹体油气地球化学研究应关注的几个前沿方向：①在流体包裹体分析实验技术中,单个包裹体分析技术在油气地质定量化研究中具有重要的作用;②通过有机包裹体自然剖面与模拟实验对比研究烃类流体运移分馏,为建立油气成藏过程地球化学示踪指标提供基础参数;③通过储层中不同期次有机包裹体的化学组成、同位素组成、生物标志化合物与圈闭中已经聚集成藏的油气地球化学特征的对比研究,确定圈闭中油气的成因、来源和充填过程;④有机包裹体成烃作用研究为碳酸盐岩生烃和深层油气成因理论提供依据;这些方向的研究成果为深化油气理论、提高勘探水平具有重要意义。     

东营凹陷高青-平南断裂带幔源流体活动特征及其成藏效应

东营凹陷高青-平南断裂带为幔源流体运移的主要通道,该幔源流体主要为岩浆(岩)和CO2气体。高青-平南断裂带幔源流体活动方式和活动强度存在着时间和空间上的差异,该断裂带在古近纪-新近纪至少经历了四期富CO2幔源流体活动。高青-平南断裂带富CO2幔源流体对油气成藏的影响主要表现在：①直接形成无机CO2气藏;②通过能量——热的作用和物质,即CO2的加入,影响水-岩相互作用的强度和方向,从而改善油气储集层的物性;③在一定程度上提高源岩的排烃效率,增加油气的运移速率。     

藏北改则--班戈地区下白垩统多巴组的高频旋回沉积特征与盆地性质

西藏北部改则——班戈地区的下白垩统多巴组中所发育的Ⅴ级旋回表现出3种垂向沉积序列:潮坪相碎屑岩沉积序列(Ⅰ)、浅海相碳酸盐岩沉积序列(Ⅲ)和碳酸盐岩、陆源碎屑岩混合沉积序列(Ⅱ)。其中序列Ⅰ-1和Ⅲ是正常的沉积水体向上变浅的沉积序列,而序列Ⅱ具有明显的陆源碎屑先进积后退积的特征,可进一步分成3个亚类:Ⅱ-1、Ⅱ-2和Ⅱ-3。横向上从南部物源区向北呈Ⅰ→Ⅱ-1→Ⅱ-2→Ⅱ-3→Ⅲ的变化过程。结合盆地构造背景和沉积特征,本文提出多巴组高频旋回的形成与弧背盆地南部冲断带的冲断作用相对应。冲断作用期,物源区粗碎屑物质大量进积,大于盆地基底沉降速率,沉积水体逐渐变浅;冲断间歇期,物源区碎屑物质的供应迅速减少,基底沉降速率逐渐大于碎屑物质的进积速率,沉积水体又有所加深。     

The thermal structure and the location of the snow line in the protosolar nebula: Axisymmetric models with full 3-D radiative transfer

The precise location of the water ice condensation front (‘snow line’) in the protosolar nebula has been a debate for a long time. Its importance stems from the expected substantial jump in the abundance of solids beyond the snow line, which is conducive to planet formation, and from the higher ‘stickiness’ in collisions of ice-coated dust grains, which may help the process of coagulation of dust and the formation of planetesimals. In an optically thin nebula, the location of the snow line is easily calculated to be around 3 AU, subject to brightness variations of the young Sun. However, in its first 5-10 myr, the solar nebula was optically thick, implying a smaller snowline radius due to shielding from direct sunlight, but also a larger radius because of viscous heating. Several models have attempted to treat these opposing effects. However, until recently treatments beyond an approximate 1 + 1D radiative transfer were unfeasible. We revisit the problem with a fully self-consistent 3D treatment in an axisymmetric disk model, including a density-dependent treatment of the dust and ice sublimation. We find that the location of the snow line is very sensitive to the opacities of the dust grains and the mass accretion rate of the disk. We show that previous approximate treatments are quite efficient at determining the location of the snow line if the energy budget is locally dominated by viscous accretion. Using this result we derive an analytic estimate of the location of the snow line that compares very well with results from this and previous studies. Using solar abundances of the elements we compute the abundance of dust and ice and find that the expected jump in solid surface density at the snow line is smaller than previously assumed. We further show that in the inner few AU the refractory species are also partly evaporated, leading to a significantly smaller solid state surface density in the regions where the rocky planets were formed.