西藏西南部拉昂错地幔橄榄岩的地球化学特征及其构造意义

拉昂错蛇绿岩位于西藏西南部雅鲁藏布缝合带(YZSZ)的西段,由地幔橄榄岩和侵入其中的基性岩墙组成.拉昂错地幔橄榄岩普遍发育碎斑结构及熔体注入和交代结构,尖晶石的Cr#值具有较广泛的变化(0.32～0.70),大多数样品富集LREE并伴随HFSE的明显增加,少数亏损LREE,前者部分熔融程度为15%～23%,后者为10%左右,这表明它们并不是地幔单阶段部分熔融的残余物,而是MORB型亏损橄榄岩在俯冲过程中再度部分熔融后熔体与残余地幔相互作用的产物,由于熔体不同程度的混合与交代,形成了各种再饱满程度不同的橄榄岩.对拉昂错地幔橄榄岩岩石学和地球化学特征的研究,为探讨YZSZ蛇绿岩带所代表的特提斯洋盆的形成和演化提供了新的证据.     

阿尔金南缘构造带西段辉绿岩墙群的地球化学特征及构造环境

对阿尔金南缘构造带西段辉绿岩墙群的岩石学和地球化学的详细研究表明,该区辉绿岩墙群为拉斑系列岩石,其主量元素以中等TiO2(1.19%～1.59%)、高MgO(5.51%～7.88%)、贫K2O(0.04%～0.84%)和P2O5(0.10%～0.20%)、Na2OK2O为特征;高场强元素(HFSE)丰度特征显示其为E-MORB型或过渡型玄武岩质岩石;稀土元素总量相对较高,轻重稀土元素分馏不显著[(La/Yb)N=1.93～3.61,LREE/HREE=3.01～4.10],在球粒陨石标准化配分模式图上呈略富集型.结合玄武岩构造环境判别图解综合分析推测,它们可能形成于一种裂谷向MORB环境过渡的构造环境,即初始小洋盆构造环境.     

滇西南澜沧江结合带北段云县花岗岩的地质特征及形成环境

滇西南澜沧江结合带云县花岗岩体的岩石类型主要为黑云二长花岗岩,SiO2含量平均为68.57%,K2O/Na2O值平均为1.67,相对富钾,岩石属高钾钙碱性系列,岩石酸、碱度低于同类岩石平均值,而镁铁组分高于平均 值,显示岩石偏中性,与同碰撞构造环境形成的花岗岩特征类似.Al2O3含量较高,平均为13.66%,A/CNK平均为1.1,呈铝过饱和,CIPw计算结果均出现标准矿物刚玉分子(105).岩石总体上相对富集大离子亲石元素,亏损高场强元素.稀土元素总量较高,平均为240.75×10-6,轻稀土元素富集,重稀土元素亏损,(La/Yb)N为8.88～9.41,分异不是很大,Eu为中等负异常,銭u为0.52～0.57.经多种相关图解判别,岩石属S型花岗岩,其构造环境相当于大陆碰撞花岗岩类(CCG).锆石颗粒U-Pb测年结果显示,源岩的形成年龄最晚是晋宁期(778 Ma),岩体主体形成于华力西晚期一印支期.其中岩浆成因锆石样品的206Pb.238U和207Pb/235U年龄分别为49 Ma和61 Ma,反映在云县岩体中可能存在喜马拉雅期岩浆活动.     

岩石破坏前后曲线分类及脆-延转换围压研究——蚀变岩常规三轴压缩试验Ⅰ

蚀变岩是工程中少见的软弱岩类,在西南某重大水电工程中,蚀变岩处于工程的重要部位,为保证工程的长期稳定性,对蚀变岩力学特性进行了深入全面的试验研究.通过对孔隙度不同的饱水蚀变岩进行系统的常规三轴压缩试验和总结分析,提出了蚀变岩三轴压缩下破坏前应力.应变曲线可分为3大类,破坏后应力-应变曲线亦可分为3大类的形态模式.并得出结论:蚀变岩的破坏类型受围压与孔隙度的共同影响,在给定的12 MPa围压下蚀变岩以脆性破坏为主,只有孔隙度大于16%且围压大于4 MPa时才有可能进入脆-延转换状态,且脆-延转换围压随孔隙度增加而降低,临界状态应力比随孔隙度增大而增加.     

Cyclotron amplification of geomagnetic micropulsations Pc1 in the magnetosphere

A numerical analysis of cyclotron instabilities is carried out by computing the dispersion relation for a three component cold plasma-beam system. Rates of growth and damping for various values of the stream density are calculated from the dispersion relation. The rates of growth and damping increase monotonically as the number density of the proton stream increases. It is found that the frequencies at the rates of maximum growth and the damping decrease slightly to lower frequencies and a sharp peak at these frequencies becomes blunt. The minimum e-folding times of an ion cyclotron wave for (a) σ_s = 10⁻⁴, σ_i = 10⁻² and (b) σ_s = 10⁻¹, σ_i = 10⁻² are about 3·84 and 0·16 sec respectively in the vicinity of the equatorial plane at 6 Re, where σ_s and σ_i are the ratios of the beam density N_s and the helium ion (H₆⁺) density N_i to the total positive ions in the plasma-beam system.     

Variations in exospheric density at heights near 1100km, derived from satellite orbits

In an earlier paper, values of exospheric density were obtained from the orbit of Echo 2 for the years 1964–1965. The results indicated a semi-annual variation in density by a factor of between 2 and 3, considerably larger than predicted by existing atmospheric models.

These studies have now been extended to the beginning of 1967, using both Echo 2 and Calsphere 1, to show how the density is responding to increasing solar activity. Variations in density during 1964 have been analysed in more detail. The long-term variation associated with the solar cycle and the short-term variations associated with magnetic and solar disturbances agree with the variations expected on the basis of current models. The semi-annual variation is persisting to higher levels of solar activity, and although its amplitude is diminishing the factor of variation was still 1.6 in 1966.     

Measurements of radio noise at 0.700 mc and 2.200 mc from a high-altitude rocket probe

Radio noise observations at frequencies of 0·700 Mc and 2·200 Mc were made at altitudes between 3000 and 11,000 km from a Blue Scout Jr. high-altitude rocket probe on 30 July 1963. A steady background flux of (7·5₋₃⁺⁶) × 10⁻¹⁹ W m⁻²)(c/s)⁻¹ at 0·700 Mc and (1·8^+1.0_−0.5 × 10⁻¹⁹ W m⁻² (c/s)⁻¹ at 2·200 Mc was observed. Assuming a galactic origin of the observed fluxes at both frequencies, the averaged sky brightnesses are b(0·700 Mc) = (6₋₃⁺⁵) × 10⁻²⁰ W m⁻² (c/s)⁻¹ sr⁻¹b(2·200 Mc) = (1.4^+1.0_−0.5 × 10⁻²⁰ W m⁻² (c/s)⁻¹ sr⁻¹ The observed brightness at 2·200 Mc is in reasonable agreement with the results of other observers. The apparent brightness at 0·700 Mc is, however, greater than was expected from previous observations. An alternative source of the 0·700 Mc flux in the terrestrial exosphere, as well as characteristics of several noise bursts observed during the flight, is briefly discussed.