The vertical structure of planet-induced gaps in protoplanetary discs

Giant planets embedded in circumstellar discs are expected to open gaps in these discs. We examine the vertical structure of the gap edges. We find that the planet excites spiral arms with significant (Mach number of a half) vertical motion of the gas, and discuss the implications of these motions. In particular, the spiral arms will make the edge appear 'puffed up' relative to the bulk of the disc. Infrared observations (sensitive to dust) would be dominated by the light from the thick inner edge of the disc. Submillimetre observations (sensitive to gas velocities) would appear to be hot in 'turbulent' motions (actually the ordered motion caused by the passage of the spiral arms), but cold in chemistry. Resolved submillimetre maps of circumstellar discs might even be able to detect the spiral arms directly.     

Periastron precession measurements in transiting extrasolar planetary systems at the level of general relativity

Transiting exoplanetary systems are surpassingly important among the planetary systems since they provide the widest spectrum of information for both the planet and the host star. If a transiting planet is on an eccentric orbit, the duration of transits T _D is sensitive to the orientation of the orbital ellipse relative to the line of sight. The precession of the orbit results in a systematic variation in both the duration of individual transit events and the observed period between successive transits,   P _obs  . The periastron of the ellipse slowly precesses due to general relativity and possibly the presence of other planets in the system. This secular precession can be detected through the long-term change in   P _obs  (transit timing variations, TTV) or in T _D (transit duration variations, TDV). We estimate the corresponding precession measurement precision for repeated future observations of the known eccentric transiting exoplanetary systems (XO-3b, HD 147506b, GJ 436b and HD 17156b) using existing or planned space-borne instruments. The TDV measurement improves the precession detection sensitivity by orders of magnitude over the TTV measurement. We find that TDV measurements over a approximately 4 yr period can typically detect the precession rate to a precision well exceeding the level predicted by general relativity.     

An analytical method to compute comet cloud formation efficiency and its application

A quick analytical method is presented for calculating comet cloud formation efficiency in the case of a single planet or multiple-planet system for planets that are not too eccentric (e _p ≲ 0.3). A method to calculate the fraction of comets that stay under the control of each planet is also presented, as well as a way to determine the efficiency in different star cluster environments. The location of the planet(s) in mass-semi-major axis space to form a comet cloud is constrained based on the conditions developed by Tremaine (1993) together with estimates of the likelyhood of passing comets between planets; and, in the case of a single, eccentric planet, the additional constraint that it is, by itself, able to accelerate material to relative encounter velocity U ~ 0.4 within the age of the stellar system without sweeping up the majority of the material beforehand. For a single planet, it turns out the efficiency is mainly a function of planetary mass and semi-major axis of the planet and density of the stellar environment. The theory has been applied to some extrasolar systems and compared to numerical simulations for both these systems and the Solar System, as well as a diffusion scheme based on the energy kick distribution of Everhart (Astron J 73:1039–1052, 1968). The analytic results are in good agreement with the simulations.     

塔里木盆地肖尔布拉克剖面下寒武统底部硅质岩微量元素和稀土元素地球化学及其沉积背景

对塔里木盆地北部肖尔布拉克寒武系露头剖面中 8.8m厚的黑色页岩夹硅质岩组合中的硅质岩的系统采样分析表明,该硅质岩具有深源成因特征。其低的Th/U和Rb/Sr比也证明了其沉积时所具有的深部物源和热水注入迹象。硅质岩的稀土元素经北美页岩标准化后的Ce/Ce 从 0.4 2到 0.79,平均 0.5 7。Ce的负异常明显。这些稀土元素的参数特征与加利福尼亚弗朗希斯科杂岩 (FranciscanComplex)中沉积在大洋海底硅质岩的稀土元素特征十分相似。北美页岩标准化后的Eu/Eu 值从 8.0 5下降到 1.0 3。其相对较高的Eu/Eu 值很有可能反映了热水的注入。Eu/Eu 值从剖面底部到顶部的系统降低反映了剖面底部的热水作用最强烈,向上热水作用逐渐减弱。上述一系列的地球化学标志指示该硅质岩应沉积在离洋中脊不远的、具有深源物质/热水注入的远洋盆地背景中。结合区域地质和伴生黑色页岩地球化学的综合分析认为,该套硅质岩的形成与上升洋流的影响有关。上升洋流将形成于大洋盆地背景中的物质带到大陆边缘陆棚环境中发生沉积,造成了沉积在陆棚环境中的硅质岩,在地球化学组成上保留了其大洋盆地背景的特征     

54与80坐标系转换数学模型研究

54北京坐标系与80西安坐标系转换计算,属54系与80系不同参考椭球下高斯—克吕格投影数据转换计算,因全国不同区域重力场的变化而无法用一个固定的参数或公式推算,能否另辟途径实现其精确算法。应用多元统计分析基础理论,研究二者互换随机数学模型,以福建省区域为例,成功实现大批数据坐标转换。     

强制海退体系域识别特征及其油气意义

利用地震沉积学、层序地层学的相关理论和方法,结合钻测井数据、地震反射结构特征、均方根振幅属性和滨线迁移轨迹特征等资料,对珠江口盆地白云凹陷北坡21 Ma强制海退体系域的识别特征、演化模式和油气意义进行了探讨,指出该体系域在平行物源方向具有高角度斜交型前积反射,其前端靠近盆地中心发育具丘状反射的盆底扇,滨线迁移轨迹呈向盆地方向逐级下降的趋势。结果表明:强制海退体系域在垂直物源方向发育"U"型的下切谷,内部为平行的地震反射充填结构;测井曲线为漏斗形和箱型的组合特征,表现为多个四级相对海平面变化控制的准层序组,且每个准层序组都具有向上水体变浅和顶部突然变深的特征;强制海退体系域之下为前期层序高位体系域的前三角洲或陆架泥岩,其上沉积了海侵体系域和高位体系域的半深海暗色泥岩,同时受陆架坡折带地层尖灭和断裂沟通深部油源的控制,可形成有利的生、储、盖组合,是寻找岩性油气藏的有利场所。     

川西汉旺地区雷口坡组四段风暴岩特征及地质意义

通过野外实测剖面和镜下薄片观察,川西汉旺地区雷口坡组四段发育典型的风暴岩,具有底冲刷—充填构造、风暴砾屑层、菊花构造和丘状交错层理等典型风暴沉积标志。根据该风暴岩岩性、沉积位置、沉积标志组合特征,共识别出三种风暴沉积序列类型:1)序列Ⅰ由侵蚀底面及砾屑段、粒序段组成,代表靠近风暴浪基面附近的台前缓斜坡下部环境; 2)序列Ⅱ由侵蚀底面及砾屑段、粒序段、平行纹层段、丘状纹层段组成,代表靠近正常浪基面附近的台前缓斜坡上部环境; 3)序列Ⅲ由粒序段、平行纹层段组成,代表台地边缘环境。风暴层序自下而上的沉积演化为:台前缓斜坡下部—台前缓斜坡上部—台地边缘,整体为一个向上变浅的沉积序列。     

福建黄塘晚侏罗世长林组硅质岩地球化学特征及其沉积环境意义

福建黄塘地区晚侏罗世长林组发育一套层状硅质岩,夹薄层凝灰岩,产硅质海绵骨针和硅质钙藻,其硅质岩沉积环境复杂,成因一直存在不同认识。本文通过野外地质调查和岩相学研究,以及主量元素、稀土元素和微量元素分析认为,该区硅质岩为非纯硅质岩,在FeMnAl三角图中样品位于生物成因区及附近,Mo和V含量富集、轻稀土富集、Eu弱负异常及U/Th值也都具有典型的生物成因特征,且微观特征显示其受到火山活动的影响。黄塘硅质岩在Fe2O3/TiO2Al2O3/(Al2O3+Fe2O3)、TFe2O3/(100-SiO2)Al2O3/(100-SiO2)和(La/Ce)NAl2O3/(Al2O3+Fe2O3)图解中都投在了大陆边缘及附近。ΣREE值较高、Ceanom值、MnO/TiO2值及(La/Yb)N值等这些地球化学指标一致表明黄塘硅质岩处于受陆源物质影响的大陆边缘浅海沉积环境。在前人研究基础上,认为研究区在晚侏罗世早期开始发生海侵并伴有小规模的火山活动,整体为还原环境,局部可能水体较深,为进一步开展福建、浙江地区的石油地质评价工作提供了依据。