High resolution TEM of chondritic carbonaceous matter: Metamorphic evolution and heterogeneity

Abstract– The insoluble carbonaceous matter from 12 chondrites (CI, CM, CO, CV, EH, and UOC), was characterized by high resolution transmission electron microscopy (HRTEM). Besides ubiquitous nanoglobules, the insoluble organic matter from petrologic type 1 and 2 chondrites and Semarkona (LL 3.0) is composed of a highly disordered polyaromatic component. No structural differences were observed between these IOMs, in agreement with the limited thermal metamorphism they all experienced. In chondrites of petrologic type >3.0, the evolution of the IOM is controlled by the extent of thermal metamorphism. The polyaromatic layers, shorter than 1 nm in petrologic type ≤3.0 chondrites, grow up to sizes between 5 and 10 nm in petrologic type >3.6 chondrites, contributing to the increase of the degree of structural order. In addition, we find rare, but ubiquitous onion‐like carbons, which may be the product of nanodiamond graphitization. The insoluble carbonaceous matter of the enstatite chondrite Sahara 97096 (EH 3) is different from the other meteorites studied here. It is more heterogeneous and displays a high abundance of graphitized particles. This may be the result of a mixture between (1) the disordered carbon located in the matrix, and (2) catalytic graphitized phases associated with metal, potentially originating from partial melting events. The structural and nanostructural evolution are similar in all IOMs. This suggests that the structure of the accreted precursors and the parent body conditions of their secondary thermal modifications (temperature, duration, and pressure) were similar. The limited degree of organization of the most metamorphosed IOMs compared with terrestrial rocks submitted to similar temperature suggests that the conditions are not favorable to graphitization processes, due to the chemical nature of the precursor or the lack of confinement pressure.     

宁夏固原硝口重碳酸根离子高值变化分析

对宁夏固原硝口重碳酸根离子的高值变化进行了详细研究。对观测条件和观测环境进行了细致的调查分析,得出该台重碳酸根离子的高值变化主要是观测条件不符合规范要求所致,不是地震前兆异常。     

南海北部初级生产力的物理-生物海洋学耦合特征及其对固碳量的影响

通过修订的VGPM模型,利用南海北部7年平均SeaWiFS和AVHRR遥感资料,分析了该海域河口上升流及反气旋涡等生境表层叶绿素浓度和初级生产力的周年变化,结果表明,季风驱动下的物理一生物海洋学耦合过程是控制研究海域浮游植物生物量和初级生产力时空变化的主导因素.浮游植物生物量和初级生产力随着季风、环流以及中尺度涡等物理...     

1958-2012年来河北汛期暴雨气候变化特征分析

应用1958-2012年河北21个基准站和基本站逐日降水观测资料,分析了河北汛期暴雨的气候分布特征、年际、年代际变化以及趋势变化特征。结果表明,汛期暴雨分布呈现东部、南部多,向西北部递减的特征。最大暴雨量中心在河北东部、燕山南麓的唐山、秦皇岛地区。从年际和年代际尺度分析,暴雨量、频次、强度都存在2-3 a的年际变化周期信号,暴雨量和频次在20世纪80年代以后存在15-20 a的年代际周期信号。汛期暴雨量、暴雨频次时间序列整体呈现下降趋势,特别是21世纪以来,河北暴雨量和暴雨频次下降趋势更为明显,暴雨强度在近50 a变化幅度不大。在空间分布上,暴雨量、暴雨频次和暴雨强度三个特征量在年代际变化中整体都呈现东退南缩的特征。从趋势分析看来,大部分站点汛期暴雨量、频次、强度都呈现下降趋势。     

Analysis of the Properties of Super Solar Proton Events and Associated Phenomena

The solar flares, the speeds of shocks propagated in the solar-terrestrial space and driven by coronal mass ejections (CMEs), the heliographic longitudes and Carrington longitudes of source regions, and the geomagnetic storms, which are accompanied by the super solar proton events with a peak ?ux equal to or exceeding 10 000 pfu, have been studied by using the data of ground-based and space observations. The results show that the heliographic longitudes of source regions of super solar proton events distributed in the range from E30? to W75°. The Carrington longitudes of source regions of super solar proton events distributed in the two longitudinal belts, 130°∼220° and 260°∼320°, respectively. All super solar proton events were accompanied by major solar flares and fast CMEs. The averaged speeds of shocks propagated from the sun to the Earth were greater than 1 200 km/s. Eight super solar proton events were followed by major geomagnetic storms (Dst≤−100 nT), except that one super solar proton event was followed by a geomagnetic storm with the geomagnetic activity index Dst=−96 nT, a little smaller than that of major geomagnetic storms.     

A Statistical Study of the Relation between the Amplitude of Solar Cycle and the Area of Active Regions

Based on the observational data of sunspots, the relation between the amplitude of solar cycle and the total area of all active regions occurred in a solar cycle has been investigated. The result shows that the amplitude of solar cycle has a good correlation with the total area of all active regions occurred in the solar cycle. The relation between the amplitude of solar cycle and the area of the largest active region during a solar cycle has also been investigated. The result shows that the amplitude of solar cycle has a poor correlation with the area of the largest active region during a solar cycle, and there is no fixed relation between the peak time of a solar cycle and the time when the largest active region occurred in the solar cycle.