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.     

Fragmentation of the Current Sheet,Anomalous Resistivity,and Acceleration of Particles

The evolution of the current sheet in the electric current direction (in the guiding magnetic field direction) is studied numerically in the 3-D particle-in-cell model with two current sheets and periodic boundary conditions. In the regime with (where v _D and are the electric current drift and electron thermal velocities, respectively) the current sheets are unstable owing to the Buneman and kink instabilities and become strongly fragmented. During their evolution, in addition to an increase of the energy of the electric field component in the guiding magnetic field direction, the energies of the electric field components in the perpendicular direction are even more enhanced. In the current sheet the anomalous resistivity (η _anom/η _C∼7×10⁵, where η _C is the classical resistivity) is generated and thus the magnetic field dissipates. Most of the dissipated magnetic energy is transformed into the electron kinetic energy in the direction of the electric current. The associated electric field accelerates the electrons from the tail of the distribution function.     

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.     

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。     

台湾东部海域沉积物波特征及其成因探讨

利用地震剖面对沉积物波的分布、形态和内部结构进行了分析,结合区域地质背景对沉积物来源和成因进行了探讨。识别出的沉积物波域主要位于台东峡谷与陆坡其他峡谷的交汇区,单个波形的波长为0.8～7.2 km,波高为18～75 m左右,呈NE—SW向展布。台东峡谷弯曲段内侧向上坡迁移的沉积物波,其底界发育块体流沉积,内部可细分为下部过渡单元和上部波形单元。弯曲段外侧的沉积物波呈垂向加积的特征,底部无块体流沉积。基于沉积物波的几何形态,估算整个波域的流体厚度在196～356 m之间,流体速度在15～21 cm/s之间。沉积物波的形态特征、内部结构、分布规律以及数值计算表明这些沉积物波为浊流成因。台湾东部海域沉积物波域的发育与台湾西南部的沉积物波域一样,是台湾造山运动的沉积响应。距今3.5 Ma以来花东海脊的形成以及广燠火山岛—绿岛—兰屿火山岛间闸口的抬升和封闭使得沉积物经由卑南溪及海下水道向南输送到绿岛西侧的台东海槽残留弧前盆地时受阻,转而沿台东峡谷及陆坡冲沟体系向东输送入花东海盆。浊流沉积物沿着峡谷/沟谷体系向下坡方向输送的过程中,在峡谷/冲沟的嘴部等地形限制性降低的位置卸载,或在台东峡谷的高弯曲段漫溢出来,从而形成沉积物波域。     

Prediction Model of Coal Reservoir Pressure and its Implication for the Law of Coal Reservoir Depressurization

The main methods of coalbed methane(CBM) development are drainage and depressurization, and a precise prediction of coal reservoir pressure is thus crucial for the evaluation of reservoir potentials and the formulation of reasonable development plans. This work established a new reservoir pressure prediction model based on the material balance equation(MBE) of coal reservoir, which considers the self-regulating effects of coal reservoirs and the dynamic change of equivalent drainage area(EDA). According to the proposed model, the reservoir pressure can be predicted based on reservoir condition data and the actual production data of a single well. Compared with traditional reservoir pressure prediction models which regard EDA as a fixed value, the proposed model can better predict the average pressure of reservoirs. Moreover, orthogonal experiments were designed to evaluate the sensitivity of reservoir parameters on the reservoir pressure prediction results of this proposed model. The results show that the saturation of irreducible water is the most sensitive parameter, followed by Langmuir volume and reservoir porosity, and Langmuir pressure is the least sensitive parameter. In addition, the pressure drop of reservoirs is negatively correlated with the saturation of irreducible water and the Langmuir volume, while it is positively correlated with porosity. This work analyzed the reservoir pressure drop characteristics of the CBM wells in the Shizhuangnan Block of the Qinshui Basin, and the results show that the CBM reservoir depressurization can be divided into three types, i.e., rapidly drop type, medium-term stability type, and slowly drop type. The drainage features of wells were reasonably interpreted based on the comprehensive analysis of the reservoir depressurization type; the latter was coupled to the corresponding permeability dynamic change characteristics, eventually proving the applicability of the proposed model.