ASTER多光谱波段与SPOT全色波段融合方法研究

遥感图像融合可以发挥多源遥感数据的优势。但由于不同传感器的遥感数据有着不同的特征,不同数据所采用的融合方法也应不同。文章探讨了ASTER多光谱波段与SPOT全色波段数据融合的方法,通过对PCA融合、IHS融合和基于小波的IHS融合方法的对比研究,得出基于小波的IHS融合法在提高空间分辨率的同时较好地保持了地物的多光谱信息。     

青海省柴达木盆地西北缘盐类矿产遥感预测研究

利用ETM多光谱遥感图像,在对盐湖区的遥感影像特征和主要地物光谱特征分析的基础上,通过波段组合变换,压抑粘土及砂砾层等地物的影响,将盐类矿产信息增强提取出来。对比前人的钾盐矿田勘查成果,所提取的盐类信息异常与现代新盐带、湿盐滩和现正在开采的钾盐矿区十分吻合。结合区域地质背景与成矿条件的分析研究,圈定了4个预测区、9处有利地段,为进一步盐类矿产勘查提供了科学依据和目标地。     

新疆若羌县维宝铅锌矿床地质特征及成因分析

维宝铅锌矿床位于祁漫塔格成矿带西段,矿床产于元古界蓟县系狼牙山组浅海相碎屑-碳酸盐岩系地层中,矿体具有明显的层控性,以及多阶段矿化特点。文章在深入分析矿床地质特征及成因的基础上,提出了该矿床在成因上属后生层控多金属矿床,并总结了找矿标志,认为在东昆仑-祁漫塔格地区具有较大的找矿前景。     

数字摄影测量相机在航空摄影测量及大比例尺数字化成图中的应用

分析了数字摄影测量相机(DMC)在航空摄影测量及大比例尺数字化成图中遇到的问题,如摄影比例尺的选择;数字解析空中三角测量野外像控点间航向基线数、旁向航线数、区域网总航线数的确定;摄影测量平台软件的选择;对计算机硬件的要求;摄影精度、加密精度、成图精度等.     

下地壳基性麻粒岩流变强度实验研究

镁铁质基性麻粒岩被认为可能是大陆下地壳的主要组成岩石[1,2],涉及当前地球动力学研究中地壳变形和高原隆升,壳幔边界的力学耦合与拆离,底侵和拆沉作用等一系列地球动力学问题阳[3,4],具有重要的地球动力学意义.大陆下地壳的流变学性质是我们深入认识这些地球深部过程的关键点之一.     

藏南硅质岩及富SiO2热水流体成岩成矿作用研究

藏南地区中生代硅质岩广泛发育,呈东西向带状展布,自北向南可分为雅鲁藏布江缝合带北侧早白垩世硅质岩带、雅鲁藏布江缝合带南侧三叠纪至白垩纪硅质岩带和特提斯喜马拉雅沉积区白垩纪硅质岩带.按照野外的沉积建造特征,分为蛇绿岩_硅质岩建造、火山岩-硅质岩建造、改造型硅质岩建造(构造断块型和构造混杂型)和浊积岩-硅质岩建造等多种类型.按照岩石学特征分为块状硅质岩、层状硅质岩、角砾状硅质岩和结核状硅质岩等四大类.     

广东大宝山金属硫化物矿床开发的环境地球化学效应

华南是中国最重要的金属成矿带之一.目前已探明储量的矿种达100多种,特别是有色金属、稀有金属、稀土金属、贵金属、放射性元素等矿产在全国占据着重要的地位.广西大厂锡多金属矿、湖南柿竹园特大型钨-钼-铋多金属矿床、水口山铅-锌多金属矿床、广东大宝山多金属矿、河台金矿、高明富湾银-金矿、廉江庞西洞银-金矿、仁化铀矿等都是全国著名的大型矿山.     

结合濮阳实际 鼓励开发地上地下空间

随着濮阳市城市框架的不断拉大,建设用地需求不断增加,在国家紧缩＂地根＂的形势下,做好节约集约用地工作尤为重要。今后各项建设要优先开发利用空闲、废弃、闲置和低效利用的土地,努力提高建设用地利用效率,严格执行闲置土地处置政策。重点在盘活城镇存量上下工夫,提高土地利用效益。     

Detection of a new interstellar molecular ion, H2COH+ (protonated formaldehyde)

A new interstellar molecular ion, H2COH+ (protonated formaldehyde), has been detected toward Sgr B2, Orion KL, W51, and possibly in NGC 7538 and DR21(OH). Six transitions were detected in Sgr B2(M). The 1(1,0)-1(0,1) transition was detected in all sources listed above. Searches were also made toward the cold, dark clouds TMC-1 and L134N, Orion (3N, 1E), and a red giant, IRC + 10216, without success. The excitation temperatures of H2COH+ are calculated to be 60-110 K, and the column densities are on the order of 10(12)-10(14) cm-2 in Sgr B2, Orion KL, and W51. The fractional abundance of H2COH+ is on the order of 10(-11) to 10-(9), and the ratio of H2COH+ to H2CO is in the range 0.001-0.5 in these objects. The values in Orion KL seem to be consistent with the "early time" values of recent model calculations by Lee, Bettens, & Herbst, but they appear to be higher than the model values in Sgr B2 and W51 even if we take the large uncertainties of column densities of H2CO into account. We suggest production routes starting from CH3OH may play an important role in the formation of H2COH+.     

A photochemical model of the martian atmosphere

The factors governing the amounts of CO, O2, and O3 in the martian atmosphere are investigated using a minimally constrained, one-dimensional photochemical model. We find that the incorporation of temperature-dependent CO2 absorption cross sections leads to an enhancement in the water photolysis rate, increasing the abundance of OH radicals to the point where the model CO abundance is smaller than observed. Good agreement between models and observations of CO, O2, O3, and the escape flux of atomic hydrogen can be achieved, using only gas-phase chemistry, by varying the recommended rate constants for the reactions CO + OH and OH + HO2 within their specified uncertainties. Similar revisions have been suggested to resolve discrepancies between models and observations of the terrestrial mesosphere. The oxygen escape flux plays a key role in the oxygen budget on Mars; as inferred from the observed atomic hydrogen escape, it is much larger than recent calculations of the exospheric escape rate for oxygen. Weathering of the surface may account for the imbalance. Quantification of the escape rates of oxygen and hydrogen from Mars is a worthwhile objective for an upcoming martian upper atmospheric mission. We also consider the possibility that HOx radicals may be catalytically destroyed on dust grains suspended in the atmosphere. Good agreement with the observed CO mixing ratio can be achieved via this mechanism, but the resulting ozone column is much higher than the observed quantity. We feel that there is no need at this time to invoke heterogeneous processes to reconcile models and observations.