我国草原下垫面低层大气湍流结构

利用超声风速仪资料分析了科尔沁草原下垫面低层大气的湍流谱结构，无量纲化湍流速度分量及温度脉动的标准偏差，和湍流通量与稳定度参数的关系。结果表明，草原下垫面低层大气湍流速度谱，在较宽的稳定度范围内， 符合Kolmogorov 相似理论，在惯性副区接近局地各向同性，无量纲化湍流速度分量及温度脉动的标准偏差服从A(1-Bζ)1/3和A(-ζ)-1/3规律， 湍流热通量与稳定度参数ζ存在较好的相关性。     

近40年东亚夏季风及我国夏季大尺度天气气候异常

定义了一个反映东亚夏季大尺度季风强度的指数，计算了夏季逐月及季的东亚季风指数（1873～1989年）。用近40年资料研究了东亚夏季风与我国夏季大尺度天气的关系。指出，强夏季风时，我国夏季大范围高温。东亚夏季风与我国夏季降水的关系则表现在夏季雨带的南北位置上。强夏季风时，雨带偏北。夏季雨带位置偏南均与弱季风有关。长江中下游夏季的涝年与弱季风有关，而强夏季风时，长江中下游经常是旱年。最后，研究了强、弱夏季风年时的北半球500 hPa环流异常特征，结果表明，东亚夏季风强度是造成我国夏季气温、降水异常的主要原因。     

有限区域卫星云图资料变分分析的试验研究

资料分析在数值预报中的重要性受到越来越多的关注，星目前常规探测网的时空局限性，利用分辨率较高的非常规资料势在必行。该文利用一个有限区域中尺度模式ＭＭ４，采用变分分析技术对有限区域的常规探空资料和非常规云图资料进行变分分析和数值模拟。     

1993年3月20日拉孜、昂仁间6．6级地震与西藏南北向地震构造带

本文在野外实地考察资料的基础上，结合前人工作成果，对１９９３年３月２０日拉孜、昂仁间６．６级地震等震线重新进行了校定并探讨其发震构造．通过对笔者近十年在青藏高原地震地质工作的总结，对西藏最新南北向地震构造带的成生、活动性及其最大地震潜在能力进行了讨论。     

铜街子电站水库诱发地震的判定及最大可能诱发地震震级的估计

对于水库围堰后猛然增加的地震活动，人们普遍关心两个问题，第一是这些地震的成因，第二是这些地震能对大坝安全性带来多大的影响。位于四川省乐山地区的铜街子电站在蓄水后地震活动骤然增高。本文通过对地震活动的分布范围、震源深度、震源机制解以及地震活动与库水水位变化之间的关系判定这些地震系铜街子电站蓄水后所诱发的地震。为了估计该水库所诱发地震的震级上限，本文通过定性预测方法和定量预测方法试图对诱震震级上限给出一个估计，但各手段所给出的结果却不完全一致，这说明目前的预测手段的不完善。在对各手段给出的结果进行综合分析之后，认为铜街子电站最大可能诱发地震震级上限在５．０级左右。当然，也可能以较小震级的震群型形式出现。     

潮汐韵律层的研究进展及其天文地质意义

潮汐沉积物记录着一系列的潮汐周期。本文简要介绍了几种主要的现代潮汐周期，在此基础上回顾了最近十余年来国外对周期性潮汐沉积物，特别是潮汐韵律层的研究进展，系统介绍了几种从古代沉积物中识别出来的潮汐周期，包括基本潮汐（半日潮、全日潮和混合潮），大－小潮周期以及一些长期周波动等。最后对潮汐韵律层在推测地史时期地－月系的演化历史中的意义作了评述。     

地震空间分维Dq及b值的临震变化特征及其非线性机制分析

对云南省几个不同地区的强震孕震阶段及临震时的地震空间分维Ｄｑ（ｑ＝０，１，２，）及ｂ值进行了计算和研究，发现虽然在孕震阶段各地区的Ｄｑ及ｂ值均有着共同的下降主趋势，但临震时不同区域的Ｄｑ及ｂ的变化形态却存在着差异，大地震可能发生在Ｄｑ及ｂ值均降至最低时，也可能发生在Ｄｑ及ｂ值下降后又回升之时，还可能发生在Ｄｑ回升而ｂ值仍保持最低时。本着重对Ｄｑ及ｂ值的临震变化特征及其个体差异从非线性的角度作了物     

The Geothermal Study of the Mid-Segment of the Tancheng-Lujiang Fault Zone and Its Neighboring Region

In this paper,25 new terrestrial heat flow values newly observed along the mid-segment of the Tancheng-Lujiang fault zone are listed.With these geothermal data and 37 other terrestrial heat flow values(previously published),we describe the distribution features of terrestrial heat flows in the area.In this research,the two-dimensional temperature structure from the surface to lithospheric bottom of the Huaibei-Sixian-Jinhu profile is inferred by using the finite-element method and the temperature and heat flow of sedimentary,granitic,and basaltic layers is calculated.     

Three-dimensional MHD simulation of interplanetary magnetic field changes at 1 AU as a consequence of simulated solar flares

A fully three-dimensional (3D), time-dependent, MHD interplanetary global model (3D IGM) has been used, for the first time, to study the relationship between different forms of solar activity and transient variations of the north-south component, B_z, of the interplanetary magnetic field (IMF) at 1 AU. One form of solar activity, the flare, is simulated by using a pressure pulse at different locations near the solar surface and observing the simulated IMF evolution of B (=-B_z) at 1 AU. Results show that, for a given pressure pulse, the orientation of the corresponding transient variation of B_z has a strong relationship to the location of the pressure pulse and the initial conditions of the IMF. Two initial IMF conditions are considered: a unipolar Archimedean spiral with outward polarity and a flat heliospheric current sheet (HCS) with outward polarity in the northern hemisphere and which gradually reverses polarity in the solar equatorial plane to inward polarity in the southern heliospheric hemisphere. The wave guide effect of the HCS is also demonstrated.     

Generation and evolution of interplanetary slow shocks

It is well known that most MHD shocks observed within 1 AU are MHD fast shocks. Only a very limited number of MHD slow shocks are observed within 1 AU. In order to understand why there are only a few MHD slow shocks observed within 1 AU, we use a one-dimensional, time-dependent MHD code with an adaptive grid to study the generation and evolution of interplanetary slow shocks (ISS) in the solar wind. Results show that a negative, nearly square-wave perturbation will generate a pair of slow shocks (a forward and a reverse slow shock). In addition, the forward and the reverse slow shocks can pass through each other without destroying their characteristics, but the propagating speeds for both shocks are decreased. A positive, square-wave perturbation will generate both slow and fast shocks. When a forward slow shock (FSS) propagates behind a forward fast shock (FFS), the former experiences a decreasing Mach number. In addition, the FSS always disappears within a distance of 150R_⊙ (where R_⊙ is one solar radius) from the Sun when there is a forward fast shock (with Mach number \geq1.7) propagating in front of the FSS. In all tests that we have performed, we have not discovered that the FSS (or reverse slow shock) evolves into a FFS (or reverse fast shock). Thus, we do not confirm the FSS-FFS evolution as suggested by Whang (1987).