塔中地区奥陶系喜马拉雅山期S干气充注的证据

塔中地区奥陶系天然气成因多样;Ⅰ号坡折带中东部奥陶系天然气以高干燥系数、 甲烷同位素值重为特征;与塔深1井寒武系原油裂解气接近;应主要来自寒武系原油裂解气成因。寒武系贫H2S、 高成熟原油裂解气在喜马拉雅山期时;气侵奥陶系油气藏;得到了以下主要证据的支持: 1）天然气甲烷δ13C值大多比Chung et al.（1988）天然气模式甲烷δ13C值计算值高3‰以上;2）干燥系数与甲烷δ13C值大体上具有正相关关系;3）天然气干燥系数与H2S含量大体上具有负相关关系。这些特征表明;存在贫H2S、 相对富13C甲烷为主的干气与富H2S、 相对贫13C甲烷的湿气混合作用。奥陶系中H2S-δ34S 值为14‰～20‰;远低于中深1井寒武系原地热化学硫酸盐还原作用（TSR）成因的H2S（33‰）;支持了奥陶系中H2S并不是来源于寒武系古油气藏。于是提出;来自寒武系贫H2S的干气在喜马拉雅山期对良里塔格组和鹰山组油气藏发生了气洗;油气藏的气/油比值增大、 导致了原油蜡含量增高、 甲烷δ13C值发生正偏移。     

Sr,Nd and O Isotopic Studies on the Genesis of the Huashan Granite Complex1

Abstract Systematical Sr, Nd and O isotopic studies were made on the Huashan granite complex in Guangxi. In combination with the studies of geological, petrological and geochemical data, it is believed that the complex consists of granites of three stages, with different geneses and different source materials. They are not the products of differentiation and evolution of one single consanguineous magma. Granites of the 1st stage are of the Indosinian syntectic type or I type, also derived from a mixed mantle-crustal source. Those of the 2nd stage are of the early Yanshanian syntectic type or I type, also derived from a mixed mantle-crustal source, and those of the 3rd stage are of the late Yanshanian transformed type or S type, derived from a crustal source.     

新疆博格达山晚古生代地层的形成时代、物源及其演化:碎屑锆石U-Pb年代学证据

新疆博格达山主体由石炭系海相火山—沉积岩系组成, 以发育两期双峰式火山岩, 但不发育花岗岩为特征, 对其晚古生代地层时代的划分和演化争议较大.本文重点对博格达山北部两个晚古生代砂岩进行了碎屑锆石U-Pb年代学分析, 重新标定博格达山地区晚古生代地层的形成时代; 利用物源区的演化, 约束晚古生代构造演化.测年结果显示博格达上亚群砂岩的碎屑锆石表面年龄值分布范围较宽, 主峰年龄为343～284 Ma(80%), 次峰年龄为386～375 Ma(3%)、503～441 Ma(7%)和871～735 Ma(10%); 芦草沟组砂岩的碎屑锆石表面年龄值非常集中, 主峰年龄为358～279 Ma(97%), 次峰年龄为257～251 Ma(约3%).博格达山中部原石炭纪博格达群上亚群与西部和南部下芨芨槽群相当, 应属于早二叠世, 中部—东部的石炭—二叠纪界线应在博格达下亚群—上亚群或居里得能组—沙雷塞尔克组之间的不整合面之中.博格达北部地区晚二叠世以南侧天山物源区供给为主, 反映出晚古生代期间博格达山地区至少存在晚石炭世末和中二叠世两期构造隆升.结合区域火山岩与火山碎屑岩的研究, 认为博格达山地区晚古生代主要经历4个演化阶段: 早石炭世弧后盆地裂解阶段、晚石炭世碰撞拼贴阶段、早二叠世碰撞后伸展阶段、中-晚二叠世再次隆升到稳定阶段.     

First application of the revised Ti-in-zircon geothermometer to Paleoproterozoic ultrahigh-temperature granulites of Tuguiwula, Inner Mongolia, North China Craton

The revised titanium-in-zircon geothermometer was applied to Paleoproterozoic ultrahigh-temperature (UHT) granulites at Tuguiwula, Inner Mongolia, North China Craton. The Tuguiwula granulites contain diagnostic UHT mineral assemblages such as sapphirine + quartz and high alumina orthopyroxene + sillimanite + quartz, suggesting formation under temperatures of ca. 1,000°C and pressures of up to 10 kbar. Here, we report detailed petrographic studies and ICP-MS data on titanium concentration in zircons associated with the UHT assemblages. The zircons associated with sapphirine–spinel–sillimanite–magnetite assemblages have the highest Ti concentration of up to 57 ppm, yielding a temperature of 941°C, and suggesting that the growth of zircons occurred under ultrahigh-temperature conditions. The maximum temperatures obtained by the revised Ti-in-zircon geothermometer is lower than the equilibrium temperature of sapphirine + quartz, indicating an interval of cooling history of the granulites from UHT condition to ca. 940°C. Many of the zircons have Ti concentrations ranging from 10 to 33 ppm, indicating their growth or recrystallization under lower temperatures of ca. 745–870°C. These zircons are interpreted to have recrystallized during the retrograde stage indicated by microstructures such as cordierite rim or corona between spinel and quartz, and orthopyroxene–cordierite symplectite around garnet. Previous geochronological study on the zircons of the Tuguiwula UHT granulites gave a mean U–Pb SHRIMP age of 1.92 Ga. However, based on the Ti-in-zircon geothermometer results reported in this work, and considering the relatively slow thermal relaxation of these rocks, we infer that the timing of peak UHT metamorphism in the Tuguiwula area could be slightly older than 1.92 Ga.     

粒状碎屑溜砂坡运动方程与砂坡土r压力计算（溜砂坡系列研究之三）

在溜砂坡系列研究之二的基础上,对风干砂的运动特征进行了细致观察。将干砂流视为连续介质的流动,对干砂流的运动动力和阻力进行了深入研究,建立了干砂流垂线流速分布方程和干砂流体底面、表面滑动速度方程。结合挡砂工程,将干砂流体视为沿底面（此种砂坡的天然休止角）滑动的三角体,从而导出粒状碎屑溜砂坡水平土压力（或水平推力）计算模型。     

The geobiological formation process of the marine source rocks in the Middle Permian Chihsia Formation of South China

The Chihsia Formation is one of the four sets of regional marine hydrocarbon source rocks from South China.In the past two decades,detailed geochemical and sedimentological studies have been carried out to investigate its origination,which have demonstrated that the high primary productivity plays a primary role in the deposition of sediments enriched in the organic matter.However,the mechanism of this high productivity and the path of the deposition and burial of the organic matter have always been a mystery.Based on the previous studies on the Shangsi Section in Guangyuan City,Sichuan Province,we proposed that the development of the equatorial upwelling due to the sea level rise is responsible for the relatively high productivity in the Chihsia Formation.The sea waters with high nutrient were transported by the sub-surface currents along the equator.High organic carbon flux was deposited on the deeper shelf,and then decomposed by bacteria,leading to the occurrence of anaerobic respiration.The metabolism of the microorganisms consumed the dissolved oxygen in waters,which was in favor of the preservation of the organic matter.This suggested geobiological model integrating with paleoclimatology,paleoceanography and geomicrobiology will help us to understand the causes of this particular sedimentary sequence.     

多普勒天气雷达冰雹探测算法评估及检验改进

利用新一代多普勒天气雷达资料和WSR-88D提供的冰雹指数算法,对2005年1月至2007年8月发生在贵州省黔西南地区的20个冰雹个例进行验证。用此算法对20个风暴日的样本计算了WT（警报阈值）、H（相对雷达的高度）、M（漏报率）、FA（虚警率）、POD／FAR／CSI（探测概率／误报率／临界成功指数）等多个函数,并将这些数据与强冰雹指数（SHI）作对比分析,将SHI作为冰雹尺寸的预报因子进行独立评估,对实际观测到的冰雹尺寸与模式预报尺寸进行比较。在考虑了本地环境、气候特征的前提下对误警率较高的情况进行了算法补尝,并针对误警率较高的现象提出解决办法：①输入当天的正确0℃／-20℃高度,②提高冰雹探测反射率阈值。用改进方法对2007年发生的9次冰雹天气过程进行对比检验。结果表明,误报率有所降低,预报冰雹尺寸更接近实际探测尺寸。     

星载铷原子频率标准的可靠性研究

星载原子频率标准在许多空间系统中担当着重要的角色,其性能和可靠性对这些系统的功能有重要的影响。介绍了广泛使用的星载铷原子频率标准的基本工作原理,分析了影响其可靠性的各种因素,并探讨了提高其可靠性的基本途径。     

M31的观测与研究进展

介绍了本星系群中最大的旋涡星系M31(仙女星系)的基本观测性质。与银河系结构类似，M31的基本成分包括：核、核球、盘和晕。对以上各个成分的观测和研究进展分别作了综述，重点是盘的星族成分和恒星形成历史，以及球状星团的分布和晕的形成历史。同时与银河系的各种观测特征和形成机制作了详细的比较。