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Search Results: 1 - 10 of 73920 matches for " 邹永廖 "
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月面克里普岩成分特征及REE等资源开发利用前景
,欧阳自远
空间科学学报 , 2003,
Abstract: 克里普岩(KREEP)最早发现于Apollo-12样品,后来在所有返月样品中都发现3克里普岩碎片,尤其以Apollo-12和Apollo-14着陆点样品中最多,因其富含元素K,REE和P而被称之为KREEP.克里普岩在月面上的分布极为重要,不但因其对月壳形成期间及形成以后的月球的演化具有重要的意义,而且由于克里普岩中富含REE等重要资源性元素,被认为可能是除钛铁矿外最重要的月球矿产资源储存库.本文在综合已有探测资料和研究成果的基础上,通过克里普岩的化学成分与矿物组成特征,Th在风暴洋区丰度的异常特征,以及克里普岩中Th与REE相关关系的分析,探讨了KREEP岩石在月面上的分布区域,进而对月球REE资源的开发利用前景进行了初步评估.
辣根过氧化物酶处理五氯酚过程的毒性特征
张国平,J.,A.,Nicell,
科学通报 , 2000,
Abstract: 用酶的催化聚合作用来处理酚类及芳香胺类化合物的污染是近年来受到重视的新方法,但人们很少研究废水在这一处理过程中的毒性变化.采用辣根过氧化物酶和过氧化氢在pH值为4时处理含五氯酚的模拟废水,集中研究了该过程的发光菌毒性特征.结果表明,五氯酚溶液的毒性在处理后大为降低,总毒性可降低至起始毒性的15%左右.处理过程的产物有少量溶解在水中,也构成一部分毒性.
月球表面水冰的探测和意义
徐琳,刘建忠,,李春来
空间科学学报 , 2003,
Abstract: 综述了月表水冰的发现,探测技术,水资源的存在形式、分布、资源量,月表水的运移和利用前景.已有的探测表明,月球上的水资源主要分布在两极的永久阴影区内,储量约为66亿吨.月表水冰主要分布于两极永久阴影区中的原因,是月球上的水可以通过弹道式跳跃逐步迁移到温度低的地区所致.本文认为月球上是否存在水对于人类进行月球基地的建设没有根本性的影响,而利用月球玄武岩中钛铁矿的反应来获取水,是更为简便和经济的方法.
地外撞击球粒的成因探讨──以K/T界面事件为例
,欧阳自远,王世杰,李春来
空间科学学报 , 1998,
Abstract: 本文对KTB地层中富含尖晶石的地外撞击球粒的成份、矿物组成、构造特点等进行了系统研究,通过陨石消熔模拟实验的分析,以及陨石消融成因模式和撞击汽云凝聚成因模式的对比研究,认为该类球粒在成因上既有消融成因的球粒,又有撞击汽云凝聚成因的球粒,并且可能同时存在另外一种成因机制的球粒.
基于稀疏分解和聚类的自适应图像去噪新方法
魏雅丽,温显斌,,郑永春
计算机应用 , 2013,
Abstract: ?随着信号稀疏表示原理的深入研究,稀疏分解越来越广泛地应用于图像处理领域。针对过完备字典构造和稀疏分解运算量巨大的问题,提出一种基于稀疏分解和聚类相结合的自适应图像去噪新方法。该方法首先通过改进的k均值(k-means)聚类算法训练样本,构造过完备字典;其次,通过训练过程中每一次迭代,自适应地更新字典的原子,使字典更适应样本的稀疏表示;然后利用正交匹配追踪(omp)算法实现图像的稀疏表示,从而达到图像去噪的目的。实验结果表明:与传统的字典训练方法相比,新算法有效地降低了运算复杂度,并取得更好的图像去噪效果。
IMPACT EVENTS AND ITS EFFECTS ON PALAEOENVIRONMENT: EVIDENCE FROM ODP SITE 1144 CORE A
撞击事件对古环境的影响——来自ODP1144站A孔样品的证据

刘建忠,张蕾,李春来,王世杰,,徐琳,欧阳自远
第四纪研究 , 2002,
Abstract: The study on microtektites of Ocean Drilling Project(ODP) site 1144 core A around Brunhes/Matuyama boundary indicated the impact event had happened in mid Pleistocene. In this paper we use shell of foraminifera G.sacculifer to determine their C and O isotope compositions. The results indicate that C and O isotope components had changed( δ13 C reduced and δ18 O ascend) in the late stage of microtektite event. The main reason of changes of C and O isotope components is because a part of target rock can be melted and boil away by huge energy when exterrestrial object shocked the Earth so the oxygen( δ18 O) and carbon( δ13 C) isotope composition of atmosphere can be transferred and in the mean time a large of clastic debris and shocking dust can be displaced into stratosphere and diffused to the seven seas. These clastic debris and shocking dust can reduce radialization of the sun and result in the temperature and photosynthesis reduced, so biologic acts weakened and amount of CO2 decreased. In relative to carbon( δ13 C) isotope composition,the oxygen( δ18 O) isotope composition is ascend.
LUNAR SURFACE ENVIRONMENTAL CHARACTERISTICS
月球表面的环境特征

,欧阳自远,徐琳,刘建军,胥涛
第四纪研究 , 2002,
Abstract: Based on the exploration data and previous studies, the authors suggest that small volume and mass of the moon, the short distance from the sun ( i e . high surface temperature) result in the very tenuous and thin lunar atmosphere, demonstrate that there exits ice water on shadow area of the lunar polar region and calculate out 6.6 Ga tons of ice. By comparing the composition of rare gas elements in the lunar regolith and in the solar wind, the authors analyze the physical, chemical and isotopic effects of the solar radiation on the lunar surface materials, the distributions and contents of the 3He in the lunar regolith, point out that the content of 3He relates with grain size, the mineral components, structures and elemental compositions of the lunar soil, and evaluate the exploration values of 3He. The lunar surface materials govern the lunar reflectance. Based on the spectrum characteristics of the mare basalts, highland plagioclases and their mineral components which both of them are the main rocks of the lunar surface materials, the authors analyze the different reflectance of the lunar near side and far side. Not only is the lunar magnetic field the important part of the lunar environment but also great significance for studying on the lunar interior structures. The moon has regional scale distribution magnetic field which may result from great impact processes.$$$$
THE MAIN ELEMENTS OF CONSTRAINT ON THE ATMOSPHERE AND HYDROSPHERE ORIGIN AND EVOLUTION OF THE TERRESTRIAL PLANETS
制约类地行星大气层和水体发育的主要因素

欧阳自远,,李春来,刘建忠,徐琳
第四纪研究 , 2002,
Abstract: In this paper, the authors analyze the original and evolutional characteristics of the atmosphere and hydrosphere of the Mercury, Venus, Earth (including the Moon), Mars, discuss the differences of the atmosphere and hydrosphere among the Venus, Mars and the Earth. Compared with the outer planets of the solar system, the terrestrial planets have small mass and volume, high density, slow rotation, less or no satellite, low volatile element abundances,near the Sun, lost all of their original atmosphere driven by the strong solar wind during Taurus Period,combined with the frequent and heavy impacts, the present atmosphere is secondary and come from the leaving of gases in interiors. The formation and evolution of the atmosphere and hydrosphere of the terrestrial planets were controlled by their mass (representing their energy as well as the duration and intensity of tectonic activities), the distance from the sun, and other elements. Generally, among the terrestrial planets the Earth and Venus characterized by the haviest mass, highest escape velocity, tied up much more gases which are more complicated in components and higher in density. The Mars with light mass and a velocity of no more than the half of the Earth′s, the gases on its surface gradually escaped into the deep space and the atmosphere became rare. The Mercury is the lightest planet in the terrestrial planets and nearest to the sun on which not only the solar wind but also thermal motions of molecules of gases (high temperature) is strong, and the gases easily escape into the space leaving rather rare atmosphere and have the solar wind properties. The Moon has the minimum mass with almost no atmosphere and hydrosphere. Overall, the thermal history of planets,the distance from the sun and their mass puts important effects on their atmosphere and hydrosphere formation and evolution.
山西吕梁山界河口群变质基性火山岩的地球化学及年代学研究*
刘建忠,张福勤,欧阳,自远,李春来,,徐琳
中国科学 地球科学 中国科学 地球科学 , 2001,
Abstract: ?通过对山西吕梁山东西两侧的界河口和西榆皮地区变基性火山岩的系统采样和测试分析,其常量、微量、稀土元素地球化学的特征表明该区的变基性火山岩形成于类似现代大陆裂谷的构造环境中.Sm-Nd,Rb-Sr同位素年代学的研究表明,界河口群变基性火山岩形成于2600Ma的壳幔分异事件中,在新太古晚期(2500Ma±)遭受了麻粒岩相变质作用的改造,使岩石的Sm-Nd体系发生了重设.而在古元古代晚期(1800Ma±)由于吕梁运动的影响,使岩石的Rb-Sr体系又一次发生变化,因其强度较小而未涉及Sm-Nd体系.该区所获得的1600Ma±的年龄值,可能与克拉通内局部的岩浆活动有关.研究结果不支持吕梁群生成于太古代的观点,而应该是古元古代时期的产物.
模拟月壤研制的初步设想
郑永春,王世杰,刘建忠,李泳泉,
空间科学学报 , 2005,
Abstract: 模拟月壤是月球样品的地球化学复制品.作者总结世界上已有的5种模拟月壤JSC-1,MLS-1,MLS-2,MKS-1和FJS-1的研制过程、方法与基本理化性质.认为系列化模拟月壤研制对中国首次月球探测有重要意义.在此基础上,作者提出系列化模拟月壤研制的基本思路.
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