The fraction of galaxies that contain active nuclei and their accretion rates

We investigate the relationship between the present-day optical luminosity function of galaxies and the X-ray luminosity function of Seyfert 1s to determine the fraction of galaxies that host Seyfert 1 nuclei and their Eddington ratios. The local type 1 active galactic nuclei (AGN) X-ray luminosity function is well reproduced if ∼1 per cent of all galaxies are type 1 Seyferts which have Eddington ratios of ∼10⁻³. However, in such a model the X-ray luminosity function is completely dominated by AGN in E and S0 galaxies, contrary to the observed mix of Seyfert host galaxies. To obtain a plausible mix of AGN host galaxy morphologies requires that the most massive black holes in E and S0 galaxies accrete with lower Eddington ratios, or have a lower incidence of Seyfert activity, than the central black holes of later-type galaxies.     

青藏高原物质东流的岩石层力学背景探讨

利用地表大地热流观测资料、岩石生热率及热导率数据研究了三江和四川盆地 6个地区的岩石层平均温度结构及强度分布。结果表明 ,整个三江地区岩石层温度较高 ,而四川盆地温度较低 ;在岩石层强度分布上 ,四川盆地为高强度区 ,而三江地区则为低强度区 ;整个三江地区构成了一条青藏高原物质东流的低强度通道 ;由于四川盆地高强度块体的阻挡 ,青藏高原向东的物质流在此转向近南向 ,沿三江地区流逸 ;不同岩石层块体的强度差异可能是控制高原物质流动态势的重要力学背景之一。     

The Time-Varying Gravitational Potential Field of a Massive,Deformable Body

The internal as well as the external gravitational field of the Earth is computed under the assumption that (i) the mass distribution of the deformable body as well as (ii) the heights of the topographic surface and the depths of the interfaces (dynamic isostasy) vary in time. In order to represent those shape variations properly, the topographic masses as well as the interface masses are regarded as condensed following a proposal by F.R. Helmert (1884, p. 149-163). Accordingly time-varying simple layer mass densities are generated. Basic results are collected in 4 boxes.     

岩石矿物组份质量转移的模糊聚类定量计算

本文根据岩石矿物组份质量分数值的定和特性 ,提出定量计算组份质量转移的新方法。该方法运用模糊动态聚类分析技术 ,通过计算复原定和差并判定差值类型 ,辅以相应的判别参数 ,逐步从中筛选出真恒量组份 ,再利用真恒量组份定值系数 ,计算出变组岩石矿物各组份的真实质量分数值和转移量值。笔者将该方法称为真恒量组份定值法 (TCF法 )。     

GasBench-IRMS在碳酸盐岩δ^13C和δ^18O在线连续分析中的应用

采用GasBench-IRMS气体质谱分析技术，实现了碳酸盐岩中碳氧同位素的在线连续分析。优化了色谱柱温、离子源参数等工作条件，排除了空气中N2O的干扰。结果表明，色谱柱柱温为40℃、65℃时，方法线性范围较宽，结果准确可靠。方法用于碳酸盐岩国家一级标准物质中δ^13C和δ^18O的测定，结果与标准值一致。     

阿中地块北缘库木达坂岩体群特征及锆石U-Pb测年

分布于阿中地块北缘中浅变质岩隆起带之上的库木达坂岩体(群),为一规模较大的复式岩体,不同岩石类型之间接触关系清楚,由早到晚其侵位顺序为细粒黑云二长花岗岩→中粒含斑黑云二长花岗岩。岩石地球化学资料研究证明,该岩体群与大陆岛弧型花岗岩(CAG)相似,显示壳源花岗岩特点,岩体群中获得(449.7±5.8)Ma的单颗粒锆石U-Pb年龄值,确定该岩体群侵位时代为晚奥陶世,岩体形成可能与红柳构—拉配泉早古生代洋壳向南俯冲相关。     

Homogeneity of the Geochemical Reference Material BRP-1 (Paraná Basin Basalt) and Assessment of Minimum Mass

Reference materials (RM) are required for quantitative analyses and their successful use is associated with the degree of homogeneity, and the traceability and confidence limits of the values established by characterisation. During the production of a RM, the chemical characterisation can only commence after it has been demonstrated that the material has the required level of homogeneity. Here we describe the preparation of BRP-1, a proposed geochemical reference material, and the results of the tests to evaluate its degree of homogeneity between and within bottles. BRP-1 is the first of two geochemical RM being produced by Brazilian institutions in collaboration with the United States Geological Survey (USGS) and the International Association of Geoanalysts (IAG). Two test portions of twenty bottles of BRP-1 were analysed by wavelength dispersive-XRF spectrometry and major, minor and eighteen trace elements were determined. The results show that for most of the investigated elements, the units of BRP-1 were homogeneous at conditions approximately three times more rigorous than those strived for by the test of "sufficient homogeneity". Furthermore, the within bottle homogeneity of BRP-1 was evaluated using small beam (1 mm²) synchrotron radiation XRF spectrometry and, for comparison, the USGS reference materials BCR-2 and GSP-2 were also evaluated. From our data, it has been possible to assign representative minimum masses for some major constituents (1 mg) and for some trace elements (1-13 mg), except Zr in GSP-2, for which test portions of 74 mg are recommended.     

Early star formation and the evolution of the stellar initial mass function in galaxies

It has frequently been suggested in the literature that the stellar IMF in galaxies was top-heavy at early times. This would be plausible physically if the IMF depended on a mass-scale such as the Jeans mass that was higher at earlier times because of the generally higher temperatures that were present then. In this paper it is suggested, on the basis of current evidence and theory, that the IMF has a universal Salpeter-like form at the upper end, but flattens below a characteristic stellar mass that may vary with time. Much of the evidence that has been attributed to a top-heavy early IMF, including the ubiquitous G-dwarf problem, the high abundance of heavy elements in clusters of galaxies, and the high rate of formation of massive stars in high-redshift galaxies, can be accounted for with such an IMF if the characteristic stellar mass was several times higher during the early stages of galaxy evolution. However, significant variations in the mass-to-light ratios of galaxies and large amounts of dark matter in stellar remnants are not as easily explained in this way, because they require more extreme and less plausible assumptions about the form and variability of the IMF. Metal-free 'population III' stars are predicted to have an IMF that consists exclusively of massive stars, and they could help to account for some of the evidence that has been attributed to a top-heavy early IMF, as well as contributing importantly to the energetics and chemical enrichment of the early Universe.