深圳市景亿山庄滑坡特征及成因分析

根据现场工程地质调查和勘察,论文深入分析了景亿山庄滑坡的变形特征、性质、变形机制,并探讨了滑坡的成因。指出在具有剥蚀残丘地貌特征的场地开挖以砂岩残积物为主要组成物质的边坡时,边坡高陡是造成边坡变形破坏的主要因素。长时间的持续降雨是诱发因素。对于陡倾原生节理裂隙发育的土质和类土质边坡,滑坡周界受边坡体内原生节理裂隙控制,滑坡后缘常沿该陡倾的节理裂隙发育。在深圳等降雨量大的亚热带气候区,若坡体内没有不利于边坡稳定的各种结构面,当边坡开挖高度不超过20m,总体坡率不陡于1∶1时,边坡能够保持短期稳定。但长期稳定性受当地降雨量和降雨强度的控制,开挖后若不采取适当的加固措施,易发生滑坡等浅层病害。其病害从孕育到发生可持续长达10a之久。通过论文的研究,可供在类似地区开挖边坡、整治边坡病害借鉴。     

西藏直孔水电站大坝混凝土防渗墙超前支护成槽试验研究及施工

在西藏直孔水电站松散砂卵石地层混凝土防渗墙成槽施工中，结合坝基水文地质及工程地质特点，创造性地提出了超前支护成槽方案，通过三维应力模拟和渗透试验，结合现场生产试验，对原方案更进一步完善，在施工中加以应用获得了成功。     

The brown dwarf desert as a consequence of orbital migration

We show that the dearth of brown dwarfs in short-period orbits around Solar-mass stars – the brown dwarf desert – can be understood as a consequence of inward migration within an evolving protoplanetary disc. Brown dwarf secondaries forming at the same time as the primary star have masses which are comparable to the initial mass of the protoplanetary disc. Subsequent disc evolution leads to inward migration, and destruction of the brown dwarf, via merger with the star. This is in contrast with massive planets, which avoid this fate by forming at a later epoch when the disc is close to being dispersed. Within this model, a brown dwarf desert arises because the mass at the hydrogen-burning limit is coincidentally comparable to the initial disc mass for a Solar mass star. Brown dwarfs should be found in close binaries around very low mass stars, around other brown dwarfs, and around Solar-type stars during the earliest phases of star formation.     

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.     

新疆柯坪新生代推覆岩席的走向连接与成因分析

柯坪断隆新生代推覆构造是南天山南缘冲断系统的一部分,断隆上多排逆冲岩席被数条横向断裂复杂化,致使不同地段岩席排数不等,各排岩席在走向上的对应关系不明,形成了十分奇特的山弯构造.逆冲岩席的变形特点是南天山新生代造山运动的重要表征.笔者通过卫星影像分析和野外路线地质调查,对横向断裂切割各排逆冲岩席之切点部位的构造特征及岩席内部中小型构造所显示的成因信息进行了详细分析,据此,对复杂岩席在走向上进行了连接,对其数量进行了识别.在此基础上,提出了复杂岩席成因的斜冲褶皱模式,即在北西向应力场持续作用下,岩席向南东斜冲,并在其水平位移分量作用下,沿走向发生褶皱和斜冲错断:横向断裂是多排岩席褶皱翼部扭性断层的发展和连通.     

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。