不同物探方法在青海省共和盆地塔拉滩找水效果的分析

本文通过对不同物探方法在塔拉滩找水效果的详细分析、总结,着重指出可控源音频大地电磁测深法（CSAMT）在该区找水效果良好、成果可信度高。     

A numerical study of swash flows generated by bores

The dynamic processes of bore propagation over a uniform slope are studied numerically using a 2-D Reynolds Averaged Navier–Stokes (RANS) solver, coupled to a non-linear k − ε turbulence closure and a volume of fluid (VOF) method. The dam-break mechanism is used to generate bores in a constant depth region. Present numerical results for the ensemble-averaged flow field are compared with existing experimental data as well as theoretical and numerical results based on non-linear shallow water (NSW) equations. Reasonable agreement between the present numerical solutions and experimental data is observed. Using the numerical results, small-scale bore behaviors and flow features, such as the bore collapse process near the still-water shoreline, the ‘mini-collapse’ during the runup phase and the ‘back-wash bore’ in the down-rush phase, are described. In the case of a strong bore, the evolution of the averaged turbulence kinetic energy (TKE) over the swash zone consists of two phases: in the region near the still-water shoreline, the production and the dissipation of TKE are roughly in balance; in the region farther landwards of the still-water shoreline, the TKE decay rate is very close to that of homogeneous grid turbulence. On the other hand, in the case of a weak bore, the bore collapse generated turbulence is confined near the bottom boundary layer and the TKE decays at a much slower rate.     

基于GPRS的嵌入式TCP/IP协议转换器设计

介绍了一种基于GPRS的TCP/IP嵌入式协议转换器的设计。利用西门子MC55射频模块和嵌入式系统,设计具有标准的RS232串口到GPRS无线网络TCP/IP协议的双向转换传输设备。变传统的串口通讯为GPRS无线网络通讯,实现串口设备的快速无线联网。转换器采用透明传输的方式,用户不用知道复杂的GPRS通讯原理和TCP/IP协议,不用更改程序即可实现原有串口设备的无线网络连接。     

大板金矿物探解译分析及成矿远景预测

大板金矿位于医巫闾造山带中段,为韧性剪切带型金矿,经 1999年度普查资料证实其有一定资源潜力,成矿远景较好,尤其是电法及高精度磁测工作为掩盖区地质填图及地下深部矿体分布提供了透视性信息,为 2000年大板金矿勘查工作奠定了良好的工作基础。经本次对物探资料解译分析,提出大板金矿东部及南部以及白土沟一带为主要成矿远景区。     

综合物探方法在寻找斑岩型钨钼矿中的应用——以青海某钨钼矿区为例

青海某钨钼矿是近年新发现的一处斑岩型钨钼矿,在预查阶段采用了地面高精度磁测结合激电中梯测量等传统物探方法组合,在圈定隐伏斑岩体范围、解析含矿斑岩体空间赋存状态的工作中取得较好的勘查效果.说明在充分认识成矿环境的基础上,综合选择物探方法,可以从不同角度对比、分析物探异常是否为矿致异常,提高地质解释的准确性,较好地解决具体...     

黄海西部2005—2007年海雾演变的气候特征研究

海雾对沿海地区的交通运输、工农业生产等影响很大,需要开展深入研究,以探索其生消演变规律。本文选择黄海西部的成山头、青岛、海阳、日照等4个测站为代表性测站,分析了2005—2007年海雾发生期间的位势高度、海温、海表面风场、相对湿度、稳定度及散度等要素场特征,着重探讨了海雾演变的气候特征。研究结果表明:500 hPa高空槽前位于黄海上空时有利于成雾;海温异常低的年份雾日较多;风向、散度和低层的层结稳定度是影响黄海海雾的主要因素;地理位置也是影响黄海海雾变化的重要因子;黄海海雾的水平分布具有南北空间不一致的特点。     

井中激电在西霞矿区的应用

以西霞矿区ZK001孔的井中激电为实例,介绍了井中激电在该矿区的应用效果及推断解释方法。说明井中激电在对地面激电异常验证中可以判断、验证钻孔是否已揭露异常体及异常体的空间展布状况。     

桩古25井映震效能分析

介绍了桩古２５井的基本情况,分析了地震前该井产油量变化特征和映震效能。震前该井产油量突升,有时还伴有自喷现象,地震强度越大,异常幅度越大或持续时间越长,该井对绝大部分发生在其周围２００ｋｍ以内的４级以上地震和５００ｋｍ以内的５级以上地硅有不同程度的异常反映,最后对该井的映震机理进行了讨论。     

A TiO study of the dwarf nova IP Pegasi

We present red spectra in the region ∼ λ 7000–8300 Å of the eclipsing dwarf nova IP Peg, with simultaneous narrow-band photometry centred at 7322 Å. We show that by placing a second star on the slit we can correct for the telluric absorption bands which have hitherto made the TiO features from the secondary star unusable. We use these TiO features to carry out a radial velocity study of the secondary star, and find this gives an improvement in the signal-to-noise ratio of a factor of 2 compared with using the Na  i doublet. In contrast with previous results, we find no apparent ellipticity in the radial velocity curve. As a result we revise the semi-amplitude to K ₂=331.3±5.8 km s⁻¹, and thus the primary and secondary star masses to 1.05^-0.07_+0.14 M⊙ and 0.33^-0.05_+0.14 M⊙ respectively. Although this is the lowest mass yet derived for the secondary star, it is still overmassive for its observed spectral type. However, the revised mass and radius bring IP Peg into line with other cataclysmic variables in the mass–radius–period relationships.
By fitting the phase-resolved spectra around the TiO bands to a mean spectrum, we attempt to isolate the light curve of the secondary star. The resulting light curve has marked deviations from the expected ellipsoidal shape. The largest difference is at phase 0.5, and can be explained as an eclipse of the secondary star by the disc, indicating that the disc is optically thick when viewed at high inclination angles.