岩石声发射Kaiser点信号频带能量分布和分形特征研究

通过单轴加载岩石破坏全过程声发射试验,根据Kaiser效应原理采用参数法确定了Kaiser点.在此基础上,首先采用小波包频带分解方法,对岩石声发射Kaiser点信号的能量分布特征进行了研究,分析了砂岩声发射信号的不同频带能量分布规律,得到了Kaiser点特征频带能量百分比大于相邻点的重要结论.其次,采用G-P算法计算了声发射过程关联分维数,结果表明声发射过程不仅具有分形特征,而且Kaiser点声发射信号关联分维数小于其相邻点,其结论可作为通过波形分析识别Kaiser点的特征.     

微波消解等离子体发射光谱和石墨炉原子吸收光谱法联合测定土壤中多元素

采用密闭式微波消解系统处理土壤样品,电感耦合等离子体发射光谱法或石墨炉原子吸收光谱法测定土壤样品中铜、砷、铅、锌、钴、铬、锰、镍、钒9个元素。分别从消解液的选择、用酸量及样品消解量等方面进行消解条件的优化,确定了一个最适合土壤消解的前处理体系。各元素的检出限为0.16～2.52μg/g,回收率为95.2%～106.6%,精密度为2.03%～9.79%(n=7)。方法简单快速,效率高,劳动强度低,是进行土壤中多元素测定的高效方法。     

复杂地质构造波动方程数值模拟

利用全声波方程进行地震波场的数值模拟，虽然可以计算全声波波场值，但是也常常会出现层间多次波，给资料解释造成一定的困难。作者在本文中根据无反射声波方程，采用有限差分数值解法，实现了自激自收时间剖面的制作，避免了层间多次波的产生。本方法不但允许速度有纵向变化，而且允许速度有横向变化，这使得模拟复杂地质构造的地震响应成为可能。实际计算结果表明，该方法是一种行之有效的自激自收时间剖面的计算机数值模拟方法。     

电感耦合等离子体原子发射光谱法测定黄铁矿中微量元素

采用电感耦合等离子体原子发射光谱法检测了黄铁矿中Cd,Co,Cu,Mn,Pb,Zn和Ni。用干扰系数校正法消除黄铁矿中铁对上述元素的干扰，采用HCl-HNO3体系溶解矿样，不需化学分离，直接测定。方法已应用于国家标准物质GBW07267的测定。结果与标准值相符，相对标准偏差（n=8)为1.5%-7.3%。     

中高温三轴应力下鲁灰花岗岩热破裂声发射特征的试验研究

在中高温三轴应力作用下岩石内部物理化学性质和结构特性将发生变化,随着岩石内部结构的变化会引发一系列的声发射现象。通过试验研究了大试件花岗岩在三轴压力状态下声发射随温度的变化规律。试验研究表明：①随着温度升高,岩石的声发射现象是间断发生的;②花岗岩存在一个开始发生热破裂的门槛值温度,其值为120 ℃左右;③试验温度范围内花岗岩热破裂的声发射现象可分为5个阶段,即岩石原生裂隙整合阶段、热破裂前声发射静默阶段、热破裂声发射阶段、大规模热破裂后声发射静默阶段、二次热破裂开始阶段。     

Cathodoluminescence of authigenic albite

Authigenic albites in carbonate rocks typically grow in a high-grade diagenetic to low-grade metamorphic environment and often show Roc-Tourné-twinning sensu Füchtbauer. Based on an investigation of four Middle to South European occurrences, they show Mn²⁺- and Fe³⁺-activated cathodoluminescence (CL), as revealed by combined high resolution spectroscopy of cathodoluminescence emission (HRS-CL), electron paramagnetic resonance (EPR), and proton-induced X-ray emission (μPIXE).     

同步辐射软X射线吸收谱与发射谱测定天然针铁矿能带结构

天然半导体矿物由于成分、缺陷复杂,传统测试方法如紫外可见漫反射等难以准确测定其禁带宽度.本文以针铁矿为例,通过第一性原理计算得到纯针铁矿及掺Al针铁矿的电子结构.计算结果显示,纯针铁矿导带底与价带顶均由Fe3d与O2p轨道组成,而当含杂质Al时,Al2p与O2p发生杂化参与了价带组成.在此基础上,利用同步辐射X射线氧的K边吸收谱与发射谱对纯针铁矿及天然针铁矿的能带结构进行了测定.结果表明,天然含Al的针铁矿禁带宽度为2.30eV,小于纯针铁矿(2.57eV).本研究提供了一种测定天然氧化物矿物禁带宽度的新方法,为深入研究天然半导体可见光催化活性产生机制提供了理论依据.     

The shape of the radio wavefront of extensive air showers as measured with LOFAR

Extensive air showers, induced by high energy cosmic rays impinging on the Earth’s atmosphere, produce radio emission that is measured with the LOFAR radio telescope. As the emission comes from a finite distance of a few kilometers, the incident wavefront is non-planar. A spherical, conical or hyperbolic shape of the wavefront has been proposed, but measurements of individual air showers have been inconclusive so far. For a selected high-quality sample of 161 measured extensive air showers, we have reconstructed the wavefront by measuring pulse arrival times to sub-nanosecond precision in 200 to 350 individual antennas. For each measured air shower, we have fitted a conical, spherical, and hyperboloid shape to the arrival times. The fit quality and a likelihood analysis show that a hyperboloid is the best parameterization. Using a non-planar wavefront shape gives an improved angular resolution, when reconstructing the shower arrival direction. Furthermore, a dependence of the wavefront shape on the shower geometry can be seen. This suggests that it will be possible to use a wavefront shape analysis to get an additional handle on the atmospheric depth of the shower maximum, which is sensitive to the mass of the primary particle.     

Detection of solar neutron events and their theoretical approach

Solar neutron events provide important opportunities to explore particle acceleration mechanisms using data from ground-based detectors and spacecrafts. Energetic neutrons carry crucial physics information of the acceleration site, such as energy spectrum, atmospheric elements of solar flare, scale height, convergence of the magnetic field and magnetohydrodynamic turbulence. Here 12 representative solar neutron events observed on the Earth, together with X and γ-ray observations from spacecrafts are presented. Theoretical approaches on solar neutrons that are carried out mainly through the Monte Carlo simulation are compared with the observation data, and the constraints of different theoretical models on the observations are to be summarized.     

活动星系核（AGN）的宽线区（BLR）（Ⅱ）

ＡＧＮ天体的主要特征之一，就是它们的光谱中有宽而强的发射线，因此，这些宽发射线的产生区域ＢＬＲ为人们提供了一个了解ＡＧＮ天体物理本质的独特而重要的场。在文中围绕讨论了ＢＬＲ基本物理特征，评述近年来有关的理论和观测研究进展及其现状在文（Ⅱ）中主要涉及ＢＬＲ的几何结构和尺度及其运动学研究的进展和现状。