苏浙皖边界地区苏皖运动的有关问题

苏皖运动的存在于否,对研究苏浙皖边界地区的地质发展史和正确认识长兴阶地层有重要意义。笔者论证了长兴组的厚度变化、界线粘土层的性质与成因、底砾岩的确认和地层接触关系、古生物群的突变等问题,认为:1)区内苏皖运动是存在的;2)砺山-江阴海堤不可否定;将安徽广德牛头山经江苏宜兴至江阴条带内的龙潭组上部地层作为长兴组的相变产物是不妥的。     

内蒙古东乌珠穆沁旗舒哈迪铅锌多金属矿成矿特征

舒哈迪铅锌多金属矿床赋存在发育于奥陶系中统多宝山组细碧岩、石英角斑岩岩系中的断裂构造蚀变带内,矿体呈脉状、透镜状,受舒哈迪背斜构造及其伴生的断裂构造控制,铅锌矿石成分简单,伴生有银和铜.围岩蚀变主要为黄铁矿化、硅化、绿泥石化、绿帘石化、绢云母化和碳酸盐化,具有不明显的分带性.成矿物质来源于奥陶系中统多宝山组变质岩系,成矿热液来源于隐伏的岩浆侵入体,矿床成因属于岩浆热液充填（脉）型铅锌多金属矿床,矿床形成时代为燕山早-中期.     

胶东金矿金成色及其指示意义

影响金成色的因素较多,包括矿床成因类型、形成深度、变质程度、成矿时代、成矿温度和矿化阶段等,其中金矿床形成深度是最关键的因素。矿床形成深度大,成矿的物化参数变化慢,形成的金成色高;形成深度小,成矿的物化参数变化快,形成的金成色低。以胶东金矿为例,统计并定性分析了这种关系,证明胶东金矿区存在类似的规律,据此可以推广,以矿床金的成色来判断矿床的形成深度和矿体的延深情况。胶东金矿金成色较低,以５５０～７５０居多,反映了金矿成矿以中浅成为主。南张家金矿金成色最低,暗示其形成深度最浅（小于１．５ｋｍ）。     

东营凹陷下第三系深部碎屑岩储层次生孔隙垂向分布及成因分析

东营凹陷下第三系埋深大于 30 0 0 m的深部碎屑岩储层普遍发育 2～ 4个次生孔隙带 ,Φ=10 %～ 30 % ,K=0 .1× 10 - 3μm2～ 30× 10 - 3μm2 ,为中孔低渗低孔低渗油气储层。综合有机质热演化过程、成岩作用和构造断裂等分析 ,认为东营凹陷埋深大于 30 0 0m碎屑岩地层中 ,第一、二个次生孔隙带埋深在 30 0 0 m～ 390 0 m之间 ,其形成主要与有机质成熟过程释放有机酸对长石等颗粒的溶解有密切关系 ,在深大断裂附近储层同时受到大气淡水的影响 ,而深陷带包裹于暗色泥岩中的浊积砂岩的次生孔隙发育情况还与泥质岩异常压力带有关 ;第三个次生孔隙带埋深一般为 390 0 m～ 430 0 m,主要成因于粘土矿物转化造成的还原环境 ,同时受到硫酸盐热化学氧化还原反应的影响。这三个次生孔隙发育带对储集油气有效。第四个孔隙发育带埋深在 470 0 m以下 ,主要是构造成因的微裂缝 ,较难成为有效的油气储层。     

太平洋水下海山磷酸盐的成因及形成环境

笔者首次对太平洋与大洋富钴结壳密切相关的海山磷酸盐的成因及形成环境进行了比较深入的研究.研究发现,各种产出形态的磷酸盐都不同程度地交代碳酸盐等含钙物质,而呈现出交代生物结构、交代凝灰结构、交代角砾状结构及交代填间结构等各种交代结构,反映了磷酸盐的交代成因. 此外,其δ13C值(变化于0.7‰~2.0‰之间)也证实其属于交代成因.磷酸盐中Na、Mg、Sr、F、P2O5含量以及Na/P2O5、Mg/P2O5、Sr/P2O5、F/P2O5的比值,特别是晶格中结构CO2的含量(变化于5.7%~6.2%之间),与形成于氧化环境下的Blake plateau、Chatham Rise、Agulhas Bank等处的磷酸盐相近,表明调查区磷酸盐亦形成于氧化环境.氧同位素测定结果表明,磷酸盐的形成温度为5.8~14.8 ℃,平均为11.5 ℃,显示其形成于正常的海水温度环境.西、中太平洋海山磷酸盐形成环境十分接近的事实暗示,西、中太平洋广大区域内的成磷事件存在着时间上和成因上的统一性和相似性.     

Spatial mapping of earthquake hazard parameters in the Hindukush–Pamir Himalaya and adjacent regions: Implication for future seismic hazard

The study deals spatial mapping of earthquake hazard parameters like annual and 100-years mode along with their 90% probability of not being exceeded (NBE) in the Hindukush–Pamir Himalaya and adjoining regions. For this purpose, we applied a straightforward and most robust method known as Gumbel’s third asymptotic distribution of extreme values (GIII). A homogeneous and complete earthquake catalogue during the period 1900–2010 with magnitude M_W ⩾ 4.0 is utilized to estimate these earthquake hazard parameters. An equal grid point mesh, of 1° longitude X 1° latitude, is chosen to produce detailed earthquake hazard maps. This performance allows analysis of the localized seismicity parameters and representation of their regional variations as contour maps. The estimated result of annual mode with 90% probability of NBE is expected to exceed the values of M_W 6.0 in the Sulaiman–Kirthar ranges of Pakistan and northwestern part of the Nepal and surroundings in the examined region. The 100-years mode with 90% probability of NBE is expected to exceed the value of M_W 8.0 in the Hindukush–Pamir Himalaya with Caucasus mountain belt, the Sulaiman–Kirthar ranges of Pakistan, northwestern part of the Nepal and surroundings, the Kangra–Himanchal Pradesh and Kashmir of India. The estimated high values of earthquake hazard parameters are mostly correlated with the main tectonic regimes of the examined region. The spatial variations of earthquake hazard parameters reveal that the examined region exhibits more complexity and has high crustal heterogeneity. The spatial maps provide a brief atlas of the earthquake hazard in the region.     

Dynamical response to supernova-induced gas removal in spiral galaxies with dark matter halo

We investigate the dynamical response, in terms of disc size and rotation velocity, to mass loss by supernovae in the evolution of spiral galaxies. A thin baryonic disc having the Kuzmin density profile embedded in a spherical dark matter halo having a density profile proposed by Navarro, Frenk & White is considered. For the purpose of comparison, we also consider the homogeneous and   r ⁻¹  profiles for dark matter in a truncated spherical halo. Assuming for simplicity that the dark matter distribution is not affected by mass-loss from discs and the change of baryonic disc matter distribution is homologous, we evaluate the effects of dynamical response in the resulting discs. We found that the dynamical response only for an adiabatic approximation of mass-loss can simultaneously account for the rotation velocity and disc size as observed particularly in dwarf spiral galaxies, thus reproducing the Tully–Fisher relation and the size versus magnitude relation over the full range of magnitude. Furthermore, we found that the mean specific angular momentum in discs after the mass-loss becomes larger than that before the mass-loss, suggesting that the mass-loss would most likely occur from the central disc region where the specific angular momentum is low.