吸收衰减属性在准噶尔盆地西北缘二叠系储层预测中的应用探讨

地震波的吸收衰减与储层的含油气性直接相关。通过对地震波衰减属性的提取和分析,可以使我们更好地对储层的性质(含油气性)做出识别和判断,使地震资料的储层预测工作取得更好的效果。这里主要叙述了利用分频瞬时Q值属性识别和预测研究区夏子街组优质储层的方法流程及应用效果。通过与已钻井的资料对比分析得到,吸收衰减属性的应用效果较好,所得结果正确可靠,从而为该地区的油气储层预测提供了重要依据。     

“蓝绿”合作,对抗气候变化

全球气候变化给人类生存和发展带来的影响早已不言而喻,如何有效控制气候变化成为一个重要而紧迫的话题。目前,多数专家认可的有效途径莫过于从“末端”增加碳吸收以及从源头上减少碳排放两种。减少碳排放,主要从调整能源结构、减少化石燃料使用量、增加可再生能源的使用等方面入手。至于增加碳吸收,则更多要借助自然的力量。     

稀疏存储的显式有限元三角网格地震波数值模拟及其PML吸收边界条件

有限元法是复杂介质地震模拟的有力工具,它能比较客观地反映地震波的传播,比较细致地再现地震图像.但是,为了获得较精确的结果,有限元法模拟地震波的传播需要的网格点数多,具有计算量大和消耗内存多的缺点.针对上述缺点,本文对刚度矩阵采用压缩存储行(CSR)格式,以减少计算量并节省内存;采用集中质量矩阵得到对角的质量矩阵以提高有限元法(显式有限元)的计算效率;时间离散采用保能量的Newmark算法以提高有限元法的计算精度;采用变分形式(弱形式)的PML吸收边界条件对人工截断边界进行处理.通过与高精度的数值方法--谱元法的数值试验的对比表明,上述方法的引入可使有限元法在计算精度和计算效率方面均可取得比较显著的改进.为了获得相当的计算精度,相比于7阶谱元法,显式有限元法需要更精细的网格.然而,显式有限元法的计算速度比前者快近2倍,而内存需求仅为谱元法的1/4~1/6.     

翡翠的A货B货C货的区别

翡翠A货 是指仅仅经过雕刻打磨加工的纯天然翡翠.翡翠A货有以下特征: 1.翠性.这是由于组成翡翠的硬玉或其它辉石矿物的晶体具有两组完全的解理而造成的.在光照下,由于这些解理面的反射作用,可以看到翡翠表面众多的闪闪发光的小面,通常在翡翠锯开的或未抛光的表面上,翠性非常明显. 2.天然翡翠还具有橘皮效应,其抛光表面上常常像橘皮似的起伏不平,产生这一现象的原因是由于翡翠中硬玉颗粒的排列方向不一致所致.     

本期文章导读

571土壤溶解性有机质对植物吸收-输送-贮存重金属的影响研究现状与进展沈亚婷土壤溶解性有机质是陆地生态系统中最活跃的有机质存在形式之一,它影响着土壤重金属元素在土壤中的     

应用石墨炉原子吸收法测定地质样品中痕量银

用磷酸氢二铵作基体改进剂和塞曼效应,应用石墨炉原子吸收法对地质样品中痕量银进行测定和试验研究。该项测定和试验研究简化了样品处理过程,地质标样及实际样品分析均获得了满意的结果,加标回收率为91.2%～99.8%,相对标准偏差为6.5%～7.7%。应用该方法快速、简便、准确。     

PML吸收边界条件影响因素分析

影响完全匹配层方法吸收效果的主要因素有吸收层厚度和衰减系数,笔者通过地震波场数值模拟,讨论了吸收层厚度和衰减系数对吸收效果的影响。研究表明,在衰减系数一定时,吸收层厚度越大,边界反射越弱。吸收层的厚度一般在12～20道较为适当,在吸收层的厚度比较小时,随着衰减系数的增大,边界反射逐渐减弱甚至完全没有边界反射,但是若再进一步增大衰减系数则又会逐步出现边界反射。因此,在实际应用中应该注意衰减系数的选择,衰减系数一般在500～2 000之间,衰减系数较大反而影响其效果。     

Observation and Simulation of Abnormal Transmittance over Yangbajing,Tibet

Defining abnormal transmittance as the case where the magnitude of the shortwave flux transmittance is greater than 1.0, the authors used surface solar irradi- ance and all-sky images obtained at the Yangbajing site in Tibet to analyze the reasons for the occurrence of abnor- mal shortwave flux transmittance. Based on the Interna- tional Intercomparision of Three-Dimensional Radiation Code （I3RC） Monte Carlo community model of three-dimensional radiative transfer, the authors also per- formed simulations at a nonabsorbing wavelength and an absorbing wavelength through a stratocumulus and a cu- mulus field. The results showed the detection of abnormal transmittance on more than half the days, and the maxi- mum transmittance was 1.34. The probability of the oc- currence of abnormal transmittance appeared to be largest in summer, and on a daily basis was mainly at about noon local time. Abnormal transmittance mainly appeared when clear sky and clouds co-existed, especially at the edges of broken clouds and nearby regions with clear-sky conditions. The flux transmittance decreased as the solar zenith angle increased.     

The kilosecond variability of X-ray sources in nearby galaxies

Chandra observations of 17 nearby galaxies were analyzed and 166 bright sources with X-ray counts 〉 100 were chosen for temporal analysis. Fractional root mean square （rms） variability amplitudes were estimated for light curves, binned at 4 kilosecond （ks）, with length 〈 40 ks. While there are nine ultra-luminous X- ray sources （ULXs） with unabsorbed luminosity （in the 0.3-8.0 keV band） L 〉 1039 erg s-1 in the sample for which the fractional rms variability is constrained to be 〈 10%, only two of them show variability. One of the variable ULXs exhibits a secular transition and has an ultra-soft spectrum with temperature - 0.3 keV while the other is a rapidly varying source in NGC 0628, which has previously been com- pared to the Galactic microquasar GRS 1915＋105. These results seem to indicate that ULXs are typically not highly variable on ks timescales, except for some ultra-soft ones. Among the relatively low luminosity sources （L - 10^38 erg s-1）, we find five of them to be variable. Apart from an earlier known source in NGC 1569, we identify a source in NGC 2403 that exhibits persistent high amplitude fluctuations. In general, the variability of the sources does not seem to be correlated with hardness, which indicates that they may not be due to variations in any absorbing material, but instead could reflect instabilities in the inner accretion disk.