辽宁庄河地区花岗岩侵位机制及岩浆动力学的初步探讨——以光明山花岗岩复式岩体为例

运用岩浆动力学原理探讨庄河地区光明山花岗岩复式岩体岩浆侵位的驱动力、上升通道、通道最小临界宽度和定位过程,指出光明山花岗岩复式岩体是由其岩浆在区域挤压力的作用下,沿由深大断裂所提供的最小临界宽度呈脉状上侵,并在地壳浅部以岩墙扩张的形式定位而成.     

中国道路网络的通达性评价与演化机理

现代交通方式产生之前,传统道路设施及道路运输是主要交通方式,成为各历史时期社会经济联系的主要途径,本文力图探究道路设施网络的长期演化规律。为此,本文以具有国家意义的“国道”为研究对象,以商周以来3500年为时间尺度,设计了道路网发育指标和可达性—最短距离模型;刻画了中国道路网的拓展和演化过程,总结各时期的发展特征、空间格局及模式,揭示演变规律;评价了道路网的结构特征、成熟水平与连通性,分析各时期的可达性格局及演变,识别可达性优势与劣势区域;考察了道路网演变与中国社会—经济系统的关系机制。研究发现,中国道路网遵循了“内陆扩张”模式尤其从内陆向边疆拓展,可达性形成明显的“核心—边缘”中心圈层格局,并同国防建设和国家集权、邮驿系统、贸易运输有紧密关系。     

气候态意义下的南海春季暖池

应用气候态月平均的Levitus和COADS(Comprehensive Ocean-Atmosphere Data Set)温度资料及COADS海面通量资料, 探讨了南海气候态意义下春季暖池(温度大于29.5℃的水体)的演变过程及其生消的动力学机制.研究发现, 在气候态意义下, 南海表层海温在5月份存在显著的增温, 在南海中南部形成了大面积、具有一定厚度(约15 m深)的春季暖池, 暖池面积在6月份迅速减小以至消失.对南海春季暖池的生消机制研究发现, 春季暖池的产生过程是由于在不断增长的海面净热通量的作     

上地幔密度异常驱动小尺度对流及实验模型

建立了由密度异常驱动上地幔小尺度对流的数学 物理模型, 发展了利用地震层析成像数据反演上地幔小尺度对流的基本理论和方法. 该模型建立在三维直角坐标系框架上, 假设地震层析成像所显示的地震波速度异常对应于上地幔物质密度异常, 而该密度异常反映了上地幔小尺度热对流系统的温度异常场. 模型首先将地震层析成像确定的地震波速度异常转换为密度异常, 并视其为对流的驱动力; 进而利用三维傅立叶变换, 在波数域内, 在给定的边界条件下, 求解控制流体行为的运动方程和连续性方程, 最后求得对流的流场. 为检验本研究提出的理论和方法的有效性, 本文使用了两个简单的实验模型: 热体和冷体模型; 俯冲断离( break off)板片模型, 计算了其驱动的地幔流场. 结果表明, 本文提供的理论和方法, 可以直接应用于与区域岩石层构造动力学相关的上地幔小尺度对流的研究.      

层序成因动力学参数类型及意义

层序地层学为沉积盆地分析的一个重要手段和方法。层序地层学在沉积盆地分析中的参数包括宏观参数和微观参数。宏观参数特指沉积盆地中同一成因类型或成因相关的层序构成的层序组合体的总体特征,主要包括物质组成、宏观轮廓及叠置序列等。微观参数系指单个层序本身的识别标志,分为层序内部标志和层序界面标志。前者包括层序的几何形态、规模级别、内部构型、成因格架和充填序列等;后者包括界面的物理标识、剖面特征、成因属性和级别类型等。不同的层序参数类型揭示不同的成因背景,反映不同的动态过程和成因动力学意义。通过这些参数类型及其成因意义的研究,可分析层序形成与沉积盆地及板块构造的关系,进而研究层序的形成背景和成因动力学,最终为盆地动力学研究提供基础。     

Deep Structure and Dynamics of Passive Continental Margin from Shelf to Ocean of the Northern South China Sea

To study the deep dynamic mechanism leading to the difference in rifting pattern and basin structure from shelf to oceanic basin in passive continental margin,we constructed long geological sections across the shelf,slope and oceanic basin using new seismic data.Integrated gravity-magnetic inversion and interpretation of these sections were made with the advanced dissection method.Results show that the basement composition changes from intermediate-acid intrusive rocks in the sheff to intermediate-basic rocks in the slope.The Moho surface shoals gradually from 31 km in the sheff to 22.5 km in the uplift and then 19 km in the slope and finally to 13 km in the oceanic basin.The crust thickness also decreases gradually from 30 km in the northern fault belt to 9 km in the oceanic basin.The crustal stretching factor increases from the shelf toward the oceanic basin,with the strongest extension under the sags and the oceanic basin.The intensity of mantle upwelling controlled the style of basin structures from sheff to oceanic basin.In the Zhu 1 depression on the shelf,the crust is nearly normal,the brittle and cold upper crust mainly controlled the fault development;so the combinative grabens with single symmetric graben are characteristic.In the slope,the crust thinned with a large stretching factor,affected by the mantle upwelling.The ductile deformation controlled the faults,so there developed an asymmetric complex graben in the Baiyun (白云) sag.     

Strike-slip fault patterns on Europa: Obliquity or polar wander?

Variations in diurnal tidal stress due to Europa’s eccentric orbit have been considered as the driver of strike-slip motion along pre-existing faults, but obliquity and physical libration have not been taken into account. The first objective of this work is to examine the effects of obliquity on the predicted global pattern of fault slip directions based on a tidal-tectonic formation model. Our second objective is to test the hypothesis that incorporating obliquity can reconcile theory and observations without requiring polar wander, which was previously invoked to explain the mismatch found between the slip directions of 192 faults on Europa and the global pattern predicted using the eccentricity-only model. We compute predictions for individual, observed faults at their current latitude, longitude, and azimuth with four different tidal models: eccentricity only, eccentricity plus obliquity, eccentricity plus physical libration, and a combination of all three effects. We then determine whether longitude migration, presumably due to non-synchronous rotation, is indicated in observed faults by repeating the comparisons with and without obliquity, this time also allowing longitude translation. We find that a tidal model including an obliquity of 1.2°, along with longitude migration, can predict the slip directions of all observed features in the survey. However, all but four faults can be fit with only 1° of obliquity so the value we find may represent the maximum departure from a lower time-averaged obliquity value. Adding physical libration to the obliquity model improves the accuracy of predictions at the current locations of the faults, but fails to predict the slip directions of six faults and requires additional degrees of freedom. The obliquity model with longitude migration is therefore our preferred model. Although the polar wander interpretation cannot be ruled out from these results alone, the obliquity model accounts for all observations with a value consistent with theoretical expectations and cycloid modeling.     

Could giant impacts cripple core dynamos of small terrestrial planets?

Large impacts not only create giant basins on terrestrial planets but also heat their interior by shock waves. We investigate the impacts that have created the largest basins existing on the planets: Utopia on Mars, Caloris on Mercury, Aitken on Moon, all formed at ∼4 Ga. We determine the impact-induced temperature increases in the interior of a planet using the “foundering” shock heating model of Watters et al. (Watters, W.A., Zuber, M.T., Hager, B.H. [2009]. J. Geophys. Res. 114, E02001. doi:10.1029/2007JE002964). The post-impact thermal evolution of the planet is investigated using 2D axi-symmetric convection in a spherical shell of temperature-dependent viscosity and thermal conductivity, and pressure-dependent thermal expansion. The impact heating creates a superheated giant plume in the upper mantle which ascends rapidly and develops a strong convection in the mantle of the sub-impact hemisphere. The upwelling of the plume rapidly sweeps up the impact-heated base of the mantle away from the core-mantle boundary and replaces it with the colder surrounding material, thus reducing the effects of the impact-heated base of the mantle on the heat flux out of core. However, direct shock heating of the core stratifies the core, suppresses the pre-existing thermal convection, and cripples a pre-existing thermally-driven core dynamo. It takes about 17, 4, and 5 Myr for the stratified cores of Mars, Mercury, and Moon to exhaust impact heat and resume global convection, possibly regenerating core dynamos.     

Analytical description of physical librations of saturnian coorbital satellites Janus and Epimetheus

Janus and Epimetheus are famously known for their distinctive horseshoe-shaped orbits resulting from a 1:1 orbital resonance. Every 4 years these two satellites swap their orbits by a few tens of kilometers as a result of their close encounter. Recently Tiscareno et al. (Tiscareno, M.S., Thomas, P.C., Burns, J.A. [2009]. Icarus 204, 254-261) have proposed a model of rotation based on images from the Cassini orbiter. These authors inferred the amplitude of rotational librational motion in longitude at the orbital period by fitting a shape model to Cassini ISS images. By a quasi-periodic approximation of the orbital motion, we describe how the orbital swap impacts the rotation of the satellites. To that purpose, we have developed a formalism based on quasi-periodic series with long- and short-period librations. In this framework, the amplitude of the libration at the orbital period is found proportional to a term accounting for the orbital swap. We checked the analytical quasi-periodic development by performing a numerical simulation and find both results in good agreement. To complete this study, the results obtained for the short-period librations are studied with the help of an adiabatic-like approach.     

Obliquity tides do not significantly heat Enceladus

Recently, Tyler [Tyler, R.H., 2009. Geophys. Res. Lett. 36, L15205; Tyler, R., 2011. Icarus, 211, 770-779] proposed that the tide due to an obliquity of greater than 0.1° might drive resonant flow in a liquid ocean at Enceladus, and that dissipation of the ocean’s kinetic energy may be an alternate source for the observed global heat flux. While there is currently no measurement of Enceladus’ obliquity, dissipation is expected to drive the spin pole to a Cassini state. Under this assumption, we find that Enceladus should occupy Cassini state 1 and that the obliquity of Enceladus should be less than 0.0015° for values of the degree-2 gravity coefficient C_2,2 between 1.0 × 10⁻³ and 2.5 × 10⁻³. Unless there is a significant free obliquity or the gravity coefficient C_2,2 has been significantly overestimated, it is unlikely that obliquity-driven flow in a subsurface ocean is the source of the extreme heat on Enceladus.