秦巴山区煌斑岩特征与金成矿的关系

秦巴山区煌斑岩脉广泛分布,岩脉时代主要有加里东期、印支期、燕山-喜山期。大部分含金煌斑岩产于古生代地层中,主要是志留系和泥盆系的细碎屑岩类。本文主要讨论了秦巴山区煌斑岩与金成矿关系,并指出构造破碎作用在成岩成矿中的重要地位。脉体与围岩的同化混染作用、蚀变作用与氧化作用促使金的活化、迁移、富集成矿。     

初议中亚成矿域

给出了中亚成矿域的地质含义与地理范围。此巨型成矿域以发育中、晚元古代及晚古生代成矿作用为其特点。以超大型矿床为重点,并主要围绕金、铜讨论了中亚成矿域6种类型矿床的时空展布。近年取得的进展说明,中亚成矿域在矿产资源优势与潜力方面并不亚于环太平洋成矿域及特提斯成矿域。     

地震活动时序谱的涨落统计特征与地震活跃期

为寻求地震活动演化的统计判据，本文采用多项式拟合法展示地震时序谱之涨落谱，以分维函数法判断最小邻间距（NNS）分布的Poisson性，然后采用MKS无参量法判别涨落谱之统计稳定性，确定NNS分布的转变区，具体研讨了四川、云南若干震区地震活动时序谱的涨落统计分布，发现地震活跃期到来时NNS分布表现出非Poisson化的特征。进一步通过改变和调节时序数据样本集之震级下限，并逐段前推进行统计计算的方式进一步验证结果的可靠性，客观地确定了这些震区地震活动时序涨落谱统计特征的转变期，使根据该统计法判断地震活跃期的方法论渐趋完善。     

辽东地区连山关岩体锆石U-Pb一致线年龄特征及其意义

本文以连山关花岗岩体为例，指出该区古老花岗岩体2种锆石可以作出3组U-Pb一致线交点年龄，分析了这3组年龄间的相互关系及其所代表的意义，并提出一种可能求出岩体上限年龄的方法。     

青海湟水盆地活动断裂构造格架激光散斑模拟试验研究

将最新研究的湟水盆地断裂构造格架设置于合理的试验材料之上，进行激光散斑模型模拟试验，取得了断裂活动特征的量化显示结果，并用于评价区域地壳稳定性．     

太湖流域典型滨湖河网水动力与水质时空异质性

基于中国太湖梅梁湾东部的无锡市滨湖区河网29个监测点在丰水期、平水期和枯水期的流速和水质监测数据,将河网分为梁溪河、曹王泾、骂蠡港、城市河网南区以及城市河网北区5个区域,对流速和典型水质指标的时空异质性进行分析,结合主成分分析和相关性分析,得到各区域水动力与水质现状及其成因.结果显示:梁溪河和曹王泾的水质条件和水动力条件较好,多数水质因子与流速表现出了强相关性;骂蠡港的水质和流速区域变化明显,表现弱相关性;城市河网北区和南区的流速较缓,河道污染负荷较大,流速与水质因子之间的相关性较低.通过在滨湖河网开展流速和水质的野外监测,分析流速对于河网水环境的实际效果,验证不同水质指标与流速之间的响应关系,为滨湖河网区水质保护和科学的水污染治理技术提供基础支撑.     

广西霜日的气候变化特征及其与500 hPa位势高度的关系

在统计广西各站历年霜日总数、初霜、终霜日的基础上 ,分析了广西霜日的气候概况、气候变化特征及与 5 0 0 h Pa位势高度的关系。     

The proton temperature and the total hourly variance of the magnetic field components in different solar wind speed regions

A comparison has been made between the predictions of the theory for radial variations of both Alfvénic fluctuations and solar wind proton temperatures proposed by Tu (1987, 1988) and the statistical results of hourly averaged plasma and magnetic field data observed by Helios 1 and 2 from launch through 1980 for different solar wind speed regimes. The comparison shows that for speed ranges between 500–800 km s^-1, the radial variation of the proton temperature between 0.3 and 1 AU can be explained by heating from the cascade energy determined by the radial variation of the total variance of magnetic field vector. The explanation of the radial variations of both temperature and the total variance of magnetic fields for speed ranges less than 400 km s ^-1 is less clear.This project was supported by National Natural Science Foundation of China for Tu's part of the work.     

Modeling of Solar Wind in the Coronal Funnel with Mass and Energy Supplied at 5 Mm

The origin of the solar wind is a long-standing issue in both observational and theoretical studies. To understand how and where in the solar atmosphere the mass and energy of the solar wind are supplied is very important. Previous observation suggests a scenario in which the fast solar wind originates at heights above 5 Mm in the magnetically open funnel, a process that is accompanied by downward flow below 5 Mm, whereby the mass and energy are supplied through reconnection between the open funnel and adjacent closed loops. Based on this scenario, we develop a fluid model to study the solar wind generation under the assumption that mass and energy are deposited in the open funnel at 5 Mm. The mass supply rate is estimated from the mass loss rate as given by the emptying of the side loops as a result of their assumed reconnection with the open funnel. Similarly, the energy input rate is consistent with the energy release rate as estimated from the energy flux associated with the reconnection between the open magnetic funnel and the closed magnetic loops. Following the observations, we not only simulate the plasma flowing upward to form the solar wind but also calculate the downward flow back to the lower atmosphere. This model is a first attempt to study physically the proposed scenario of solar wind origin and gives a new physical illustration of the possible initial deposition and consequent transportation of mass and energy in the coronal funnel.