X射线荧光光谱法直接测定地质样品中多种痕量元素

采用低压聚乙烯镶边垫底的粉末压饼法制样,Ｘ射线荧光光谱法直接测定了地质样品中痕量元素Ａｓ、Ｇａ、Ｓｃ、Ｌａ、Ｙ、Ｃｅ、Ｗ、Ｍｏ、Ｓｎ、Ｃｏ和Ｐｂ。讨论了背景校正、谱线重叠校正、基体效应校正和仪器漂移校正等问题。利用理论α系数代替经验系数,使方法具有较高的准确度和较低的检出限。所测１１个元素的检出限在（０．３０～２．０２）×１０－６水平,精度（ＲＳＤ,ｎ＝１１）在０．９５％～１３．０％。方法经国家一级标准物质分析验证,结果与标准值相符。     

邢台地区新近沉积粉质粘土的土性分析

以邢台地区新近沉积粉质粘土为例,对其土性进行分析,介绍了其在SEM下观察及X－射线衍射分析结果;并对该土的地基评价与处理方法进行了探讨。     

风浪对水体表层下行光场平均余弦影响的数值研究

针对不同风速造成的粗糙水面、不同入射光场,利用射线跟踪法计算了无云状况下水表下行光场的平均余弦。结果表明:对不同入射光场而言,不同风速对其几何结构的改变程度及趋势有着明显的不同,在较小直射入射的天顶角情况下,天空漫射光的比例越高,水体表层下行光场平均余弦随风速的递增而递减得越小;但当直射天顶角大到一定程度时(如:80°时),其值会随风速而增大,且直射比例越高,这种趋势越明显。太阳直射光比例越高,在风速越小时,不同太阳天顶角情况下的水体表层下行光场平均余弦的差别越大,而风速越大,其差别越小。该研究有利于水体固有光学特性的反演、提高水体初级生产力的计算精度,且该方法的计算量小,精度也较高。     

Vortex Rossby Waves in Asymmetric Basic Flow of Typhoons

Wave ray theory is employed to study features of propagation pathways(rays) of vortex Rossby waves in typhoons with asymmetric basic flow, where the tangential asymmetric basic flow is constructed by superimposing the wavenumber-1 perturbation flow on the symmetric basic flow, and the radial basic flow is derived from the non-divergence equation. Results show that, in a certain distance, the influences of the asymmetry in the basic flow on group velocities and slopes of rays of vortex Rossby waves are mainly concentrated near the radius of maximum wind(RMW), whereas it decreases outside the RMW. The distributions of radial and tangential group velocities of the vortex Rossby waves in the asymmetric basic flow are closely related to the azimuth location of the maximum speed of the asymmetric basic flow, and the importance of radial and tangential basic flow on the group velocities would change with radius. In addition, the stronger asymmetry in the basic flow always corresponds to faster outward energy propagation of vortex Rossby waves. In short, the group velocities, and thereby the wave energy propagation and vortex Rossby wave ray slope in typhoons, would be changed by the asymmetry of the basic flow.     

GRBs on probation: Testing the UHE CR paradigm with IceCube

Gamma ray burst (GRB) fireballs provide one of very few astrophysical environments where one can contemplate the acceleration of cosmic rays to energies that exceed 10²⁰ eV. The assumption that GRBs are the sources of the observed cosmic rays generates a calculable flux of neutrinos produced when the protons interact with fireball photons. With data taken during construction IceCube has already reached a sensitivity to observe neutrinos produced in temporal coincidence with individual GRBs provided that they are the sources of the observed extra-galactic cosmic rays. We here point out that the GRB origin of cosmic rays is also challenged by the IceCube upper limit on a possible diffuse flux of cosmic neutrinos which should not be exceeded by the flux produced by all GRB over Hubble time. Our alternative approach has the advantage of directly relating the diffuse flux produced by all GRBs to measurements of the cosmic ray flux. It also generates both the neutrino flux produced by the sources and the associated cosmogenic neutrino flux in a synergetic way.     

基于成像射线的偏移剖面和速度时深转换评述

深度域地震波速度模型是地震勘探中最重要的参数之一,是获得精确深度域偏移剖面的基础.本文基于成像射线的概念,阐述了时间偏移域和深度域之间的关系,明确了时间偏移后的像点是通过成像射线与深度域的散射点联系起来的.在有横向变速的情况下,时间偏移剖面需要经过时深转换才能真实反映深度域层位,同样,从时间偏移剖面上提取的速度也需要经过时深转换才能得到深度域的速度.与前者不同的是,在速度的时深转换中,不仅速度的位置需要改变,且其数值也需要进行校正.该校正因子有几种等价的描述形式：度规量、速度扩散因子和几何扩散因子.     

Long-term modulation of cosmic ray intensity in relation to sunspot numbers and tilt angle

A detailed correlative analysis between sunspot numbers (SSN) and tilt angle (TA) with cosmic ray intensity (CRI) in the neutron monitor energy range has been performed for the solar cycles 21, 22 and 23. It is found that solar activity parameters (SSN and TA) are highly (positive) correlated with each other and have inverse correlation with cosmic ray intensity (CRI). The ‘running cross correlation coefficient’ between cosmic ray intensity and tilt angle has also been calculated and it is found that the correlation is positive during the maxima of odd cycles 21 and 23. Moreover, the time lag analysis between CRI and SSN, and between CRI and TA has also been performed and is supported by hysteresis curves, which are wide for odd cycles and narrow for even cycles.     

Late Quaternary climate change record from two long sediment cores from Guaymas Basin,Gulf of California

Modern Guaymas Basin (Gulf of California, Mexico) is a region of high diatom productivity where exceptional preservation factors maintain biannually alternating sediment deposition as annual varves. New sediment cores from Guaymas Basin (MD02‐2512 and MD02‐2515) present the opportunity to construct climate records from below the last glacial period. A low‐resolution age model has been constructed from oxygen isotope analysis, correlation with other dated short piston cores from Guaymas Basin and an estimate of sedimentation rate. MD02‐2512 from eastern Guaymas Basin has an age range from the Holocene to late marine isotope stage 6 (MIS 6); MD02‐2515 from western Guaymas Basin has an age range from ～8000 to 40 000 yr. Shipboard analyses of colour reflectance, magnetic susceptibility and sediment density are combined with continuous X‐ray fluorescence scans to reconstruct a picture of glacial climate in the Gulf of California. Eastern Guaymas Basin is affected by glacial sea level fall, which results in a drastic change in productivity rates and sediment type. The laminated record of MIS 5 allows comparison with the Holocene, showing a similarity of sedimentation patterns during deglaciation and a series of very rapid variations just prior to the last glaciation. In western Guaymas Basin there are a series of Younger Dryas‐like events during the glacial, typified by low productivity and high terrigenous input. Long‐term climate and productivity changes appear to be caused by the southward displacement of the Subtropical High pressure zone. Copyright © 2005 John Wiley & Sons, Ltd.     

二阶后牛顿光线方程

近来相继提出一系列的空间天体测量计划，要求考虑在多参考系中二阶后牛顿部分对光线传播的贡献，也就是说，必须讨论在最近完成的扩展的DSX体系下的二阶后牛顿(2PN)光线方程．DSX体系是在20世纪90年代初建立的，用来讨论对N个任意形状和组成、自转可变形物体的一套完整的一阶后牛顿(1PN)天体力学理论．在此建议采用迭代的方法来推导2PN光线方程．从度规和Christoffel记号出发推导太阳系中的2PN光线方程．当忽略掉更高阶的项时，2PN光线方程将回到在很多教科书中广泛出现的1PN光线方程．利用这套方程就可以计算太阳系的光线传播．