辽宁省金矿成矿作用研究

辽宁省是我国重要的金矿产地之一。省内金矿可划分为岩浆热液型、陆相火山岩型、同韧性剪切变质热液型、变质—岩浆热液叠生型、砂砾岩型及河相冲积型（砂金矿）六种类型。金矿的形成与特定的地层、构造、岩浆岩密切相关。稳定同位素资料表明，金矿的成矿物质主要来源于古老的结晶基底——太古宙变质杂岩（第一矿源层）及早元古宙中浅变质岩（衍生矿源层）；含矿热液主要为岩浆水，变质水和大气水，且多为两种水的混合物；大气水在成矿作用中占有重要地位。金矿的成矿演化经历了太古代－早元古代矿源层及同韧性剪切变质热液金矿床、晚三叠纪－燕山早期岩浆热液及叠生型矿床及燕山晚期陆相火山岩型矿床三个形成阶段。     

准噶尔盆地中部1区块侏罗系三工河组油气输导特征分析

分析准噶尔盆地中部1区块侏罗系三工河组油藏输导格架构成及输导特征对油气分布的控制机制.研究区内砂岩输导层包括J1s12输导层及J1b1输导层,对2套输导层的分布及成因类型进行综合评价,认为J1s12砂体为区内主要输导层;将区内断裂体系划分为深层油源断裂与浅层层间断裂,前者是油气垂向输导的最主要通道,后者是油气向圈闭聚集的重要通道.结果表明:现今构造格局不是准中1区块岩性油气藏成藏控制因素,成藏期主要输导层J1s12古构造脊控制油气运移方向,油源断裂沟通的圈闭及输导层古构造脊上与层间断层沟通的圈闭是油气聚集的主要场所.     

Morphological observation of Epithemia ocellata (Ehr.) Kütz. (Bacillariophyceae) from China

The species of Epithemia ocellata (Ehr.) Kütz. from Northeastern China were observed by scanning electron microscopy (SEM). The studies on silica valve formation in different stages were made. At the early stage, a Y-shaped raphe sternum was found. Areolae were made from virgae and vimines. In immature valves, the canal formation before the raphe fissure is visible. The raphe system, virgae and vimines (areolae) might be the early siliceous elements of the valve during morphogenesis. The formations of virgae and vimines are similar to that of Gephyria media W. Arnott. Rows of silica papillae formed gradually on the face of the valve. After the areolae were covered with silica and form rows of papillae, the outer valve surface could become mature. Details of the internal costae were observed in mature valves.     

潍北凹陷孔店组二段页岩气资源潜力分析

潍北凹陷是昌潍坳陷的次一级凹陷盆地,也是胜利油田外围常规油气开采区。潍北凹陷孔店组二段发育了较厚的暗色泥页岩,是页岩气形成最有利层段,也是常规油气的生烃母岩。利用昌页参1井数据,结合以往资料,对潍北凹陷孔店组二段岩性特征,有机地球化学特征、矿物组成、泥页岩含气性特征等进行分析研究,认为孔店组二段上亚段下部和中亚段下部具备页岩气资源勘查开发潜力。     

Research on formation density MWD instrument in engineering geological exploration

A high efficiency method is very important in geological survey for a new city in China. Geophysical parameters are Measured While Drilling(MWD), and these parameters are processed and explained on the ground, so the method can replace conventional engineering geological exploration for drilling rock sample. According petroleum engineering MWD, using the different characters of different rock absorbs γ radial, with the method of storing data in hole and explaining data on the ground, engineering geological exploration formation density MWD is researched. The MWD works stabilized, and the performance is good with precise data.     

山东临清地热田地热地质特征

山东省临清地热田主体位于冠县凹陷内,面积约1550km2。地热类型属层状孔隙型,热源是地球内部的传导热,盖层是第四系和新近纪明化镇组。可被利用的热储层有4个,最有开发利用价值的是馆陶组下段热储,该热储层顶板埋深约1100m,底板埋深约1700m,热储层厚度530~580m,含水层累积厚度158~175m,单井涌水量1500~2000m3/d,出口水温62~67℃,矿化度5000mg/L左右,具腐蚀性,结垢性弱,具较好的开发利用价值。经计算馆陶组热储层单井1a的可采量为5.431×105m3,100a可采量所释放的总热量为1.156×1013kJ,合理井距为1500m。     

Relative velocities among accreting planetesimals in binary systems: The circumprimary case

We investigate classical planetesimal accretion in a binary star system of separation ab?50 AU by numerical simulations, with particular focus on the region at a distance of 1 AU from the primary. The planetesimals orbit the primary, are perturbed by the companion and are in addition subjected to a gas drag force. We concentrate on the problem of relative velocities Δv among planetesimals of different sizes. For various stellar mass ratios and binary orbital parameters we determine regions where Δv exceed planetesimal escape velocities vesc (thus preventing runaway accretion) or even the threshold velocity vero for which erosion dominates accretion. Gaseous friction has two crucial effects on the velocity distribution: it damps secular perturbations by forcing periastron alignment of orbits, but at the same time the size-dependence of this orbital alignment induces a significant Δv increase between bodies of different sizes. This differential phasing effect proves very efficient and almost always increases Δv to values preventing runaway accretion, except in a narrow eb?0 domain. The erosion threshold Δv>vero is reached in a wide (ab,eb) space for small <10-km planetesimals, but in a much more limited region for bigger ?50-km objects. In the intermediate vesc<Δv<vero domain, a possible growth mode would be the type II runaway growth identified by Kortenkamp et al. [Kortenkamp, S., Wetherill, G., Inaba, S., 2001. Science 293, 1127-1129].     

Fluid dynamics of local martian magma oceans

The evolution of a melt region produced by a large impact during Mars formation is addressed. While some impact induced melt is redistributed during crater excavation, sufficiently large impacts (much larger than basin forming impacts) generate an intact melt region which is retained beneath the excavation zone, i.e., a local magma ocean. Local magma ocean evolution depends on the effective rheology controlling large scale deformation of the solid part of the planet, mechanism of crystallization, and melt region size. Within the uncertainties of various parameters, two scenarios are possible. For sufficiently weak rheology or large melt region size, evolution is characterized by rapid extrusion and formation of a global magma ocean. For sufficiently strong rheology or small melt region size, in situ crystallization to a partially molten solid state occurs prior to isostatic adjustment. Subsequent to in situ crystallization, local magma ocean evolution depends on melt region size and efficiency of lateral redistribution compared to bulk conductive cooling. For large melt regions, lateral spreading occurs via plastic deformation and results in an asymmetric, global, partial melt layer. For small melt region size, viscous spreading viscous can result in bulk cooling below the solidus prior to formation of a global layer. A hypothesis for the origin of the hemispherical crustal dichotomy and Tharsis rise is suggested. The dichotomy is associated with a global partial melt layer produced by evolution of a large, local magma ocean. After dichotomy formation, evolution of a second, smaller, local magma ocean is related to Tharsis development.     

Anisotropy and rotation in homeoidally striated Jacobi ellipsoids

In this paper a unified theory of systematically rotating and peculiar motions is developed for homeoidally striated Jacobi ellipsoids, where both real and imaginary rotations are considered. The effect of positive or negative residual motion excess along the equatorial plane is considered to be equivalent either to an additional real or an imaginary rotation, respectively. The principle results consist of (i) the discovery that homeoidally striated Jacobi ellipsoids always admit an adjoint configuration i.e. a classical Jacobi ellipsoid of equal mass and axes; (ii) the establishment of further constraints on the amount of residual velocity anisotropy along the principal axes for triaxial configurations; (iii) the finding that bifurcation points from axisymmetric to triaxial configurations occur as in classical Jacobi ellipsoids, contrary to earlier findings. An interpretation of recent results from numerical simulations on stability is provided in the light of the model. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)