强震作用下陡倾顺层岩质边坡失稳机制研究

安县茶坪乡冷浸沟陡倾顺层岩质边坡在\     

佳木斯地块西缘金矿带构造效应与壳幔作用--以鹤岗隆起为例

佳木斯地块西缘金矿带的形成受左行走滑断裂带和深部流体控制，壳-幔作用和地球动力体制转换是成矿物质活化→运移→聚集→成矿的基本动力学保障，构造应力场转换是其重要表现形式。深切地幔牡丹江岩石圈断裂的活动发生了深熔作用，使成矿物质得以活化、运移的重要驱动力，是成岩成矿作用发生的根本原因之一。地幔流体通过壳-幔相互作用形成了含矿流体，为流体成矿作用提供了矿源，并沿深断裂运移到更高的层位，在物理化学条件发生改变时沉积成矿。佳木斯地块西缘金矿带是受深断裂控制的，矿床之间是相互联系的，是在一个构造应力体制下完成它们的成矿作用的。北北东向和伴生的北西西向断裂，并有中生代浅成-超浅成岩体或脉岩侵位是今后找矿的方向。     

模糊综合评判法在新宾县地质灾害易发程度分区评价中的应用

结合辽宁省新宾县地质灾害发育情况,在充分分析影响该地区地质灾害发生发展的自然因素和人为因素基础上,应用模糊综合评判方法,通过网格单元剖分,对泥石流、崩塌、滑坡、地面塌陷、地裂缝5种地质灾害进行易发程度划分与评价.结合Visual BASIC软件编程对各单元区评定等级,对其数字化结果进行叠加分析,最后应用Sufer 7.0软件生成等值线进行了新宾县地质灾害易发区的划分并作出评价.     

川东地区碳酸盐岩超压与天然气富集关系研究

地层流体超压的形成、演化及分布与油气成藏的主要石油地质过程有着千丝万缕地联系。由于碳酸盐岩本身的复杂性，其超压的成因及研究方法不能简单地借用“欠压实”的原理。本文从对比砂泥岩和碳酸盐岩在成压机理上的差异性入手，详细探讨了川东地区碳酸盐岩成压的各种机理，指出成烃作用是造成区域性超压的最主要因素；并结合该区超压平面上的分区性及纵向上的分带性，论述了各区、带超压与气藏分布的内在联系，总结出该区超压与天然气富集的关系。     

建立地震发射台的建议

目前地球上有成千上万个地震台，但它们都是接收地震波的地震台。建议建立一种新型的地震台，这种地震台用人工的方法不断地向外发射地震波，照亮需要研究地区的地下结构，研究特定的科学问题。建立地震发射台的核心问题是选择合适的人工震源，近年来出现的绿色环保震源，以及现代信息处理技术的发展，使得建立照亮10万km2(深至Moho面)地区地下结构的地震发射台已经完全是可能的。     

北上热带气旋发展与不发展的对比分析

重点分析了一个北上热带气旋（８５０９号台风）变性发展过程中扰动能和扰动有效有效位能的收支平衡关系及其与中纬地区高空环境场、Ｑ矢量散度、旋度特征和锋生锋消现象的联系，并和与此台风前期路径及强度相似、但进入西风带后很快消失了的８４０６号台风的诊断结是要 进行了对比。结果表明：有利的大尺度环境是台风变性发展的主要因子和先决条件，斜压过程是否能有效和大量地制造扰动动能以抵消台风北上过程中的能量耗散是其能否     

利用地基土应力分布原理确定砂垫层厚度

软弱土层场地若采用天然地基不能满足建筑物所需强度与沉降要求,采用换土撼砂法就可以提高地基的承载力。运用应力分布原理合理确定撼砂层厚度不仅可保证工程稳固性,并可节约投资和缩短工期。     

ASP.NET服务器组件技术在网络地图中的应用

在分析当前现有的网络地图发布技术优缺点的基础上,采用了目前大多数GIS厂商都使用的网络地图发布技术——栅格图像,为了克服该技术存在的交互能力弱的问题,引入ASP.NET服务器组件技术来实现地理空间数据的可视化和Web发布。重点介绍了ASP.NET服务器端组件的设计与实现,提出了基于ASP.NET服务器端组件的网络地图发布技术的体系结构,并提供了其原型系统来验证该技术的可行性与实用性。     

The activities of comets related to their aging and origin

Two indices have been developed for the purpose of comparing the natures of various classes of comets. The first is the Activity Index (AI), measuring the inherent magnitude increase in brightness from great solar distances to maximum near perihelion. The second, or Volatility Index (VI), measures the variation in magnitude near perihelion. Tentative determinations of these two indices are derived from observations by Max Beyer over more than 30 years for long-period (L-P) and short-period (S-P) comets near perihelion and from other homogeneous sources. AI determinations are made for 32 long-period (L-P) comets and for 14 short-period (S-P). The range of values of AI is of the order of 3 to 10 magnitudes with a median about 6. An expected strong correlation with perihelion distance q, is found to vary as q ^–2.3. Residuals from a least-square solution (AI) are used for comparing comets of different orbital classes, the standard deviation of a single value of AI is only ±1^m.1 for L-P comets and ±1^m.2 for S-P comets.Among the L-P comets, 19 of period P larger than 10⁴ years yield AI = 0^m.27 ± 0^m.25 compared to 0^m.39 ± 0^m.26 for 13 of period between 10² years and 10⁴ years. This denies any fading with aging among the L-P comets. Also no systematic change with period occurs for the VI index, leading to the same conclusions. Weak correlations are found with the Gas/Dust ratio of comets. No correlations are found between the two indices, nor of either index with near-perihelion magnitudes or orbital inclination.The various data are consistent with a uniform origin for all types of comets, the nuclei being homogeneous on the large scale but quite diverse on a small scale (the order of a fraction of kilometer in extent). Small comets thus may sublimate away entirely, leaving no solid core, while huge comets may develop a less volatile core by radioactive heating and possibly become inactive like asteroids after many S-P revolutions about the Sun. When relatively new, huge comets may be quite active at great solar distances because of volatiles from the core that have refrozen in the outer layers.     

Candidates for families in Apollo-Amor type asteroids

The asteroids whose perihelion distances (q) are smaller than 0.983 AU and aphelion distances (% MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXafv3ySLgzGmvETj2BSbqefm0B1jxALjhiov2D% aebbfv3ySLgzGueE0jxyaibaiGc9yrFr0xXdbba91rFfpec8Eeeu0x% Xdbba9frFj0-OqFfea0dXdd9vqaq-JfrVkFHe9pgea0dXdar-Jb9hs% 0dXdbPYxe9vr0-vr0-vqpWqaaeaabiGaciaacaqabeaadaqaaqGaaO% qaaiqadgfagaqeaaaa!3D1C!\[\bar Q\]) are larger than 1.017 AU are called Apollo type objects. Similarly Amor type objects are defined by the conditions: 0.987 AU < % MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXafv3ySLgzGmvETj2BSbqefm0B1jxALjhiov2D% aebbfv3ySLgzGueE0jxyaibaiGc9yrFr0xXdbba91rFfpec8Eeeu0x% Xdbba9frFj0-OqFfea0dXdd9vqaq-JfrVkFHe9pgea0dXdar-Jb9hs% 0dXdbPYxe9vr0-vr0-vqpWqaaeaabiGaciaacaqabeaadaqaaqGaaO% qaaiqadghagaqeaaaa!3D3C!\[\bar q\] < 1.382 AU and % MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXafv3ySLgzGmvETj2BSbqefm0B1jxALjhiov2D% aebbfv3ySLgzGueE0jxyaibaiGc9yrFr0xXdbba91rFfpec8Eeeu0x% Xdbba9frFj0-OqFfea0dXdd9vqaq-JfrVkFHe9pgea0dXdar-Jb9hs% 0dXdbPYxe9vr0-vr0-vqpWqaaeaabiGaciaacaqabeaadaqaaqGaaO% qaaiqadgfagaqeaaaa!3D1C!\[\bar Q\] > 1.666 AU. Both types are peculiar asteroids and have common dynamical behaviors. So, we regard these two type asteroids as one group and try to search for families among them.