准噶尔盆地车排子北部地区沙湾组碳酸盐胶结物差异性分布控制因素

通过铸体薄片、AxioVision图像分析、岩芯常规分析、地层水测试等方法,在明确了碳酸盐胶结物类型的基础上,采用多方法进行了碳酸盐胶结物含量的测定,探讨了准噶尔盆地车排子地区北部沙湾组碳酸盐胶结物差异性分布控制因素,并揭示了其对储层物性、油水分布的影响.研究表明,车北地区沙湾组储层中发育大量的早期碳酸盐胶结物,不均匀...     

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。     

Rhuddanian to Aeronian (Llandovery,early Silurian) carbon isotope stratigraphy throughout carbonate sequences in the upper Yangtze region,South China block

The Xiangshuyuan Formation (middle Rhuddanian to middle Aeronian stages of the Llandovery Series, lower Silurian) records a shelly fauna representing recovery after the end-Ordovician mass extinction in a well-oxygenated shallow carbonate platform of the Upper Yangtze region, South China Block. Carbon isotope stratigraphy is documented from limestone sequences of the formation at the Qiankou section, northeast Guizhou. The early Aeronian carbon isotope excursion (EACIE, with an amplitude of about 2 ‰ and peak value of 2.44 ‰) is identified in the middle and upper parts of the formation (Ozarkodina obesa conodont Biozone). The EACIE recorded herein correlates well with those in Baltica, Canada, and the United States; together with its records from organic material (δ¹³C_org) the data verify that the EACIE is a global event. The beginning of the EACIE can be used as a chemostratigraphic marker defining the Rhuddanian/Aeronian boundary in strata that lack high-resolution biostratigraphic constraints.     

辽宁义县—北票地区义县组地层层序——义县阶标准地层剖面建立和研究之一

义县地区广义的义县组可解体为王家屯组 (暂命名 )和义县组 ;分属王家屯和义县火山旋回 ,前者为偏酸、偏碱性 ,后者主体为中基性、末期为中酸性火山岩系 ,并广泛发育潜火山岩相的玄武玢岩、安山玢岩和火山集块角砾熔岩筒。该区有七个主要沉积层 ,自下而上分别为王家屯组马神庙层、义县组老公沟层、业南沟层、砖城子层、大康堡层、朱家沟层和金刚山层 ;产有较丰富的无脊椎动物、脊椎动物和植物化石。以砖城子层、大康堡层和金刚山层为界 ,义县火山旋回可划分为 4个亚旋回 ,分别代表火山活动的初始期、主期、晚期和末期。北票四合屯地区的义县组相当义县地区义县组的第一和第二亚旋回 ,含鸟类化石的主沉积层 (尖山沟层和上园层 )可与砖城子层对比     

燕山地区中元古代常州沟组潜穴化石

在燕山地区中元古代常州沟组中发育有大量的潜穴化石，潜穴产于常州沟组中部的泥质粉砂岩中。潜穴呈个体较大的直管状，垂直层面保存。这是我国迄今为止发现的最古老的遗迹化石，表明在距今近1800Ma前就已出现古老的后生动物，这对于研究后生动物的起源及演化具有重要意义。     

长城系团山子组火山岩颗粒锆石U－Pb年龄及其地质意义

蓟县中－上元古界典型剖面之邻区平谷县境内，长城系团山子组连续发育两层厚度各为１ｍ左右的富钾粗面安山岩，发育气孔构造和绳状构造。其中存在三种不同成因类型锆石，应用颗粒锆石Ｕ－Ｐｂ测定年龄技术，得到：（１）自生锆石，其Ｕ－Ｐｂ不一致上交点年龄为１６８３±６７Ｍａ，代表该火山岩形成年龄；（２）捕获锆石，多为原碎屑锆石，较年轻的一种捕获锆石的２０７Ｐｂ／２０６Ｐｂ表面年龄为１８２３±６８Ｍａ，这限定了长城系底界年龄应新于１８２３Ｍａ；（３）后生热液锆石，其Ｕ－Ｐｂ年龄为４６０Ｍａ左右，反映后期热液事件发生的时代。     

东濮凹陷古近系沙三段、沙四段介形类生物地层及界线

根据十余口探井微体古生物分析结果和对多年来积累的大量微体古生物分析资料的复查 ,将东濮凹陷古近系沙河街三段 (ES3)和四段 (ES4 )的介形类化石群自下而上分为 3个组合和 3个亚组合 :Cyprinotus igneus组合 ,分布于沙四段下亚段 ;Cyprinotus altilis- Cyprinotus jiyangensis组合 ,分布于沙四段上亚段 ;H uabeinia sinensis组合 ,分布于沙三段 ,其中 H uabeinia obscura- H uabeinia costatispinata亚组合分布于沙三段下亚段 ,H uabeiniasinensis- Candona binxianensis亚组合分布于沙三段中亚段 ,H uabeinia huidongensis- Cyprinotus dongmingensis亚组合分布于沙三段上亚段。各化石组合特征比较清楚 ,为东濮凹陷沙三段、沙四段的划分以及与渤海沿岸盆地的对比提供了依据。虽然东濮凹陷缺少渤海沿岸盆地沙四段顶界的标志性化石 Austrocypris,但该区沙三段、沙四段介形类化石组合整体面貌与整个渤海沿岸盆地相比仍然具有可对比性 ,从介形类化石组合方面来确定本区沙三段、沙四段的界线仍然是可行的     

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.