编辑等高线图的机助几何设计法

导言来自地形测量,地质测量及其它测量或其它实验观测的三维数据常常是以等高线图表示的。展示等高线图并不能提供直接可见的三维图象。但在实践中等高线图却很有用,如设计公路时研究道路位置,机场定址,环境评估等。从等高线图中获取的数据对建立三维数字地形模型也很有用。从等高线图用手工获取或提取数据是很麻烦的。因而存储等高线图以便计算机进行处理的     

贵金属的堆浸：一种成本低适用于高海拔寒冷地区的方法

金、银的回收条件是多变的,所以对于那些不经济的矿床采用常规工艺流程是不行的,而应用堆浸的方法是有利的。本文介绍了在寒冷的气候高海拨条件下堆浸的实际作业,及其在经济上的应用,而对环境又是无害的,但是必须在任何情况下都要精心设计和工作。堆浸是回收贵金属最经济的几种方法之一。对于适宜于堆浸的矿石来说,其优点是:①投资少;②生产成本低;③氰化物浸液用量比较少。另—个比较明显的特征是堆浸比较慢,从矿石中提取贵金属回收率比其它方法低,这     

低层大气的声雷达探测

随着国民经济和国防建设的迅速发展,对低层大气的风、温度和湿度等气象要素的了解,也就日益迫切。例如:做空气污染预报时,首先要给出污染物浓度分布与气象背景关系,除了系统地知道地面和高空风外,还需要知道低层大气的温度层结和湍流等实况;机场上飞机的起飞与着陆,导弹、火箭和人造地球卫星的发射,除了要定时系统地了解地面风、高空风和气温外,还需要     

Ion-molecule calculation of the abundance ratio of CCD to CCH in dense interstellar clouds

Laboratory measurements and calculations have been performed to determine the abundance ratio of the deuterated ethynyl radical (CCD) to the normal radical (CCH) which can be achieved in dense interstellar clouds via isotopic fractionation in the C2H2+ (HD) = C2HD+ (H2) system of reactions. According to this limited treatment, the CCD/CCH abundance ratio which can be attained is in the range 0.02-0.03 for the Orion molecular cloud and 0.01-0.02 for TMC-1. These ranges of numbers are in reasonable agreement with the observed values in Orion and TMC-1. However, the analysis of the CCD/CCH abundance ratio is complicated via the presence of competing fractionation mechanisms, especially in the low-temperature source TMC-1.     

Stable isotopic compositions of carbonates from the Mesoproterozoic Bangemall Group, northwestern Australia

Marine carbonate rocks from the Mesoproterozoic Bangemall Group of northwestern Australia show little deviation (+/-1.3%) in whole-rock delta 13C(carb)-values about a mean of -0.5%. This narrow range persists despite close sampling (every 10-20 m) through long sections (up to 2500 m) that are geographically widespread (up to 250 km apart), over many depositional environments (supralittoral to outer shelf), sediment sources (stromatolitic bioherms to detrital calcilutites) and rock types (pure limestones to dolomitic shales). The only major excursions from the norm seem related to unusual environmental or post-depositional processes, as they are correlated with large enrichments (to -3%) or depletions (to -16%) in 18O. Relatively heavy delta 13C-values, up to +2.5%, occur in a single bed of brecciated ferruginous dolostone at a single locality; these abnormal values may result from local evaporitic conditions. Limey and shaley nodular dolostones have delta 13C-values as low as -4.3%, probably caused by remineralization of organic matter during late and patchy dolomitization. Most notably, sharp negative excursions in delta 13C, up to -8.4%, occur in bleached kerogen-free rocks with mineral assemblages of dolomite + quartz + calcite +/- tremolite + talc, reflecting isotopic re-equilibration in thick metamorphic aureoles around dolerite intrusions. General environmental variations are minor, with delta 13C-values of peritidal facies tending to be slightly positive whereas those of subtidal facies are slightly negative. There are no strong secular trends, but subtle fluctuations within the range -2 to +l% can be correlated along the northwestern margin of the basin. This resembles the pattern seen in other Mesoproterozoic successions, but is markedly unlike the heavy background (> +5%) and extreme variations (up to l0%) in delta 13C evident in Neoproterozoic successions of similar thickness and environmental setting. Hence, in contrast to the Neoproterozoic, the global rate of organic carbon burial was probably fairly constant during deposition of the Bangemall Group, and perhaps generally during the Mesoproterozoic, as was the redox state of the atmosphere and hydrosphere.     

关于瞬变电磁法波形最优化设计问题

电磁成像分辨率的最优化要考虑发射机波形,可这个问题变成关于发射机电流强度一般特性特性问题的数字化求解,例如,发射机波形设计好了可以使各项异性层产生最大的响应。最优化的激励源为正弦波电流,它比常规时间域瞬变电磁波形在各向异性产生的场具有更高的分辨率。     

Calculations concerning the HCO+/HOC+ abundance ratio in dense interstellar clouds

Calculations have been performed to determine the rate coefficients of several reactions involved in both the formation and depletion of interstellar HCO+ and HOC+. The abundance of HOC+ deduced from these calculations is consistent with the tentative identification of HOC+ in Sgr B2 by Woods et al. The large HCO+/HOC+ abundance ratio observed by Woods et al. is due at least in part to a more rapid formation rate for HCO+ and probably due as well as to a more rapid depletion rate for HOC+.