内蒙古阿拉善北部雅干构造带白山组火山岩年龄、地球化学特征及其对区域构造演化的约束

阿拉善北部雅干地区古生代火山岩发育,研究其形成时代和地质特征,对探讨中亚造山带中段南缘北山弧盆系的演化具有重要的意义。对雅干地区原划奥陶系火山岩进行了同位素年代学与地球化学研究,获得流纹岩LA-ICP-MS锆石U-Pb年龄为298.4±1.5Ma,时代为早二叠世初期,结合岩石组合特征和区域对比,将其重新厘定为上石炭统—下二叠统白山组。该套火山岩富SiO2、高K2O、低TiO2,属于钙碱性系列; 相对富集Rb、Pb、K等大离子亲石元素,明显亏损Ta、Nb、P、Ti等高场强元素; 呈现为轻稀土元素相对富集、重稀土元素相对亏损的的右倾特征,具有较明显的负Eu异常,显示出陆缘弧火山岩的地球化学特征。上述证据表明,雅干地区白山组火山岩形成于古亚洲洋向明水-旱山地块北缘俯冲的陆缘弧构造环境。     

Eutrephoceras subplicatum (Steinmann, 1895) is a junior synonym of Eutrephoceras dorbignyanum (Forbes in Darwin, 1846) (Cephalopoda, Nautiloidea) from the Maastrichtian Quiriquina Formation of Chile

Nautilus subplicatusSteinmann, 1895 is a latest Cretaceous species of nautiloid which is common in southern South America (Chile, Argentina) and the Antarctic Peninsula and which is best assigned to the genus EutrephocerasHyatt, 1894. Nautilus dorbignyanusForbes in Darwin, 1846 and Nautilus valenciennii Hupé in Gay, 1854 are here considered to be senior synonyms which later authors have apparently overlooked. The type material of these two taxa is reillustrated. On the basis of this and additional material it is demonstrated that only a single nautiloid species occurs in the Quiriquina Formation of late Maastrichtian age. For this we propose to use N. dorbignyanus as the oldest available name.     

Ginkgo from Lower Cretaceous Changcai Formation in Helong of Jilin, NE China

Based on gross morphological and cuticular study, two species of Ginkgo From the Lower Cretaceous Changcai Formation in Helong of Jilin. were identified from this area for the first time, including Ginkgo coriacea Florin and G. sibirica Heer. The study is significant for better understanding the paleophytogeographic, paleoecologic and stratigraphic characters of the Early Cretaceous Changcai flora.     

内蒙古突泉盆地突D1井中侏罗统万宝组烃源岩地球化学特征

突泉盆地南部的牤牛海凹陷实施的突D1井见到良好的油气发现.钻井烃源岩的地化指标表明：有机质丰度低;有机质类型主要为Ⅲ型,少部分为Ⅱ型;有机质演化进入高成熟阶段,处于生气阶段.指示突D1井中侏罗统万宝组烃源岩具有一定的生烃条件.突泉盆地油气勘探方向应以找气为主.     

Effect of Shale Reservoir Characteristics on Shale Oil Movability in the Lower Third Member of the Shahejie Formation,Zhanhua Sag

To reveal the effect of shale reservoir characteristics on the movability of shale oil and its action mechanism in the lower third member of the Shahejie Formation(Es3l), samples with different features were selected and analyzed using N2 adsorption, high-pressure mercury injection capillary pressure(MICP), nuclear magnetic resonance(NMR), high-speed centrifugation, and displacement image techniques. The results show that shale pore structure characteristics control shale oil movability directly. Movable oil saturation has a positive relationship with pore volume for radius > 2 μm, as larger pores often have higher movable oil saturation, indicating that movable oil is present in relatively larger pores. The main reasons for this are as follows. The relatively smaller pores often have oil-wetting properties because of organic matter, which has an unfavorable effect on the flow of oil, while the relatively larger pores are often wetted by water, which is helpful to shale oil movability. The rich surface provided by the relatively smaller pores is beneficial to the adsorption of immovable oil. Meanwhile, the relatively larger pores create significant pore volume for movable oil. Moreover, the larger pores often have good pore connectivity. Pores and fractures are interconnected to form a complex fracture network, which provides a good permeability channel for shale oil flow. The smaller pores are mostly distributed separately;thus, they are not conducive to the flow of shale oil. The mineral composition and fabric macroscopically affect the movability of shale oil. Calcite plays an active role in shale oil movability by increasing the brittleness of shale and is more likely to form micro-cracks under the same stress background. Clay does not utilize shale oil flow because of its large specific surface area and its block effect. The bedding structure increases the large-scale storage space and improves the connectivity of pores at different scales, which is conducive to the movability of shale oil.     

基于解释量版的渤海油田巨厚砂砾岩定量表征

渤海油田古近系三角洲沉积发育巨厚（大于100 m）的砂岩和砾岩储层,储层横向变化快,内部非均质性强,地震预测难题大。文章针对此类问题,提出一种基于厚度解释量版的砂砾岩定量表征方法。根据已有钻井资料建立井点处地质模型,结合已有地质资料分析储层可能的变化形式,形成地质模型库,对地质模型库进行正演获得相应的正演地震资料库,然后提取正演地震资料的反射振幅属性,建立不同砂砾岩变化形式下的厚度解释量版,最后提取实际地震资料的反射振幅属性,将其投射到厚度解释量版上,实现对巨厚砂砾岩储层的定量表征。该方法克服了常规地震反演、地震属性等方法难以有效刻画巨厚砂砾岩储层的难题,实现了对具有干涉效应的巨厚砂砾岩储层的厚度及其内部变化的精确定量表征。     

Formation of the regular satellites of giant planets in an extended gaseous nebula I: subnebula model and accretion of satellites

We model the subnebulae of Jupiter and Saturn wherein satellite accretion took place. We expect each giant planet subnebula to be composed of an optically thick (given gaseous opacity) inner region inside of the planet’s centrifugal radius (where the specific angular momentum of the collapsing giant planet gaseous envelope achieves centrifugal balance, located at rCJ ∼ 15R_J for Jupiter and rCS ∼ 22R_S for Saturn) and an optically thin, extended outer disk out to a fraction of the planet’s Roche-lobe (R_H), which we choose to be ∼R_H/5 (located at ∼150 R_J near the inner irregular satellites for Jupiter, and ∼200R_S near Phoebe for Saturn). This places Titan and Ganymede in the inner disk, Callisto and Iapetus in the outer disk, and Hyperion in the transition region. The inner disk is the leftover of the gas accreted by the protoplanet. The outer disk may result from the nebula gas flowing into the protoplanet during the time of giant planet gap-opening (or cessation of gas accretion). For the sake of specificity, we use a solar composition “minimum mass” model to constrain the gas densities of the inner and outer disks of Jupiter and Saturn (and also Uranus). Our model has Ganymede at a subnebula temperature of ∼250 K and Titan at ∼100 K. The outer disks of Jupiter and Saturn have constant temperatures of 130 and 90 K, respectively.Our model has Callisto forming in a time scale ∼10⁶ years, Iapetus in 10⁶-10⁷ years, Ganymede in 10³-10⁴ years, and Titan in 10⁴-10⁵ years. Callisto takes much longer to form than Ganymede because it draws materials from the extended, low density portion of the disk; its accretion time scale is set by the inward drift times of satellitesimals with sizes 300-500 km from distances ∼100R_J. This accretion history may be consistent with a partially differentiated Callisto with a ∼300-km clean ice outer shell overlying a mixed ice and rock-metal interior as suggested by Anderson et al. (2001), which may explain the Ganymede-Callisto dichotomy without resorting to fine-tuning poorly known model parameters. It is also possible that particulate matter coupled to the high specific angular momentum gas flowing through the gap after giant planet gap-opening, capture of heliocentric planetesimals by the extended gas disk, or ablation of planetesimals passing through the disk contributes to the solid content of the disk and lengthens the time scale for Callisto’s formation. Furthermore, this model has Hyperion forming just outside Saturn’s centrifugal radius, captured into resonance by proto-Titan in the presence of a strong gas density gradient as proposed by Lee and Peale (2000). While Titan may have taken significantly longer to form than Ganymede, it still formed fast enough that we would expect it to be fully differentiated. In this sense, it is more like Ganymede than like Callisto (Saturn’s analog of Callisto, we expect, is Iapetus). An alternative starved disk model whose satellite accretion time scale for all the regular satellites is set by the feeding of planetesimals or gas from the planet’s Roche-lobe after gap-opening is likely to imply a long accretion time scale for Titan with small quantities of NH₃ present, leading to a partially differentiated (Callisto-like) Titan. The Cassini mission may resolve this issue conclusively. We briefly discuss the retention of elements more volatile than H₂O as well as other issues that may help to test our model.     

西藏尼玛北部新生代盆地沉积记录及控盆机理

通过野外地质调查和地层对比,将尼玛北部盆地新生代陆相地层定为牛堡组。根据岩石组合和沉积特征分析,尼玛北部盆地牛堡组可划分为扇三角洲相、湖泊相和冲积扇相。扇三角洲相可进一步划分为扇三角洲前缘和前扇三角洲2种亚相;湖泊相可划分为半深湖—深湖和滨湖—浅湖2种亚相。盆地的演化特征可分为盆地形成初始期、盆地扩张期和盆地萎缩期,3期的演化可分别对应牛堡组的一段、二段和三段。尼玛北盆地发育的各个阶段都跟古气候变化和构造活动有很大的联系,两者共同影响着盆地发育的各个阶段。结合前人的研究资料,认为尼玛盆地的发育时代为早白垩世末期—晚白垩世初。根据盆地边缘相与半深湖—深湖沉积相伴生、牛堡组底部发现火山岩夹层等沉积特征,可以推断尼玛盆地是一个具有走滑拉张性质的盆地。     

Characteristics and evolution of lacustrine turbidite of Chang-7 Member of Yanchang Formation in northern Shaanxi

Lacustrine turbidite of Chang-7 Member in the studied area consists of sihstone and fine sandstone with respect to grain size, which is feldspathic lithie sandstone, syrosem arkose and arkose with respect to mineral constitution affected by provenance. There are such apparent signatures as lithology, sedimentary structure, sedimentary sequence and well logs, to recognize turbidite. During the paleogeographic evolution of Chang-7 Member, lake basin and deep lake are both at their maximum extent during Chang-73 stage, resulting in the deposition of Zhangjiatan shale with widespread extent and of turbidite with fragmental-like. Deep lake line is gradually moving toward lake center and turbidite sand bodies are gradually turning better with better lateral continuity, connectivity and more thickness, from stages of Chang-73, Chang-72 and Chang-7t, which can be favorable reservoir in deep-water.     

河北宽城地区中元古界高于庄组微古植物群

通过对河北宽城地区高于庄组微古植物进行系统采样,利用化学浸解法,获得了大量微古植物信息,在80件样品中发现微古植物个体5000余粒,共鉴定出41属108种（含1个新属,9个新种,38个未定种）,其中包括丰富的多细胞植物化石及其碎片。根据微古植物化石的分布和特征,划分出4个化石组合。与下伏长城系微古植物相比,高于庄组微古植物具有明显的差异。这些微古植物的发现为地球早期生物演化、区域地层划分和对比,以及生物成矿和成油研究提供了重要信息。