排序方式: 共有89条查询结果,搜索用时 15 毫秒
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新疆额尔齐斯金矿带构造控矿规律研究 总被引:16,自引:3,他引:13
额尔齐斯金矿带位于新疆阿尔泰南缘。地质研究表明,发生于晚石炭世—早二叠世的金成矿作用在整个额尔齐斯金矿带中广泛发育,明显受额尔齐斯韧性剪切带及其次级断裂的控制。通过对额尔齐斯构造带及其中发育的21个金矿床(点)尤其是多拉纳萨依、托库孜巴依、萨尔布拉克、科克萨依和马热勒铁等金矿床控矿构造的研究,作者提出如下新认识:额尔齐斯韧性剪切带总体上具有向东收敛、向西散开的基本形式,控矿构造具有向东单一(仅为韧性剪切构造)、向西复杂(脆韧性构造叠加于韧性构造和中酸性岩体上)的特点,由此控制的金成矿作用具有“东浅西深、东弱西强”等6条基本规律。在此基础上,结合EH4深部地球物理测量结果,指出额尔齐斯金矿带西部哈巴河地区和中部富蕴地区是形成大型金矿床的有利地区。 相似文献
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EH4电导率成像系统在金属矿找矿中的应用研究 总被引:1,自引:0,他引:1
EH4电导率成像系统是音频大地电磁探测系统之一,该方法多应用于大地构造、石油、水文、地热和工程等领域,在金属矿找矿领域中应用尚不成熟。本文概述了EH4电导率成像系统的方法原理、数据采集和后期数据处理方法。用该测量系统对西藏山南和新疆阿勒泰两个铜矿区的岩性、构造、含矿地质体位置进行了解释,其结果与钻探结果基本吻合。尤其是对于新疆铜矿区规模较小的矿体赋存位置-断裂破碎带,EH4系统能够对此有很好的解释,说明EH4测量系统是金属矿找矿的一种有效的方法。 相似文献
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非洲已成为我国企业海外铜矿资源开发的投资主要目的地之一,针对非洲赞比亚铜矿山的深边部地质找矿技术问题开展的EH4物探找矿技术试验性应用研究,具有重要的示范效应.使用EH4连续电导率剖面测量仪完成的物探剖面测量所获取的某铜矿西矿区14线和东南矿区59线物探电性断面图,较好地反映了加丹加沉积盆地基底构造层与盆地沉积构造层之间的角度不整合沉积接触界面的空间形态展布,而且在含铜页岩层底板与基底构造层顶板之间的石英岩层与高阻异常具有较好的对应关系.这些地球物理信息可为赞比亚沉积岩型铜矿床的深部找矿提供十分重要的间接找矿线索. 相似文献
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在龙首山成矿带小白芨芨沟-小青羊地段采用EH-4连续电导率仪与V8多功能电法仪进行不同点距AMT试验结果表明,两套仪器对马路沟及其次级断裂的探测结果均反映明显,其电性特征表现为反演电阻率等值线密集带、舌状低阻带。从不同点距试验结果来看,10、20 m点距探测精度高,反映效果明显好于50m点距;从不同仪器试验结果来看,EH-4连续电导率仪与V8多功能电法仪的测量结果均能客观地反映地下地质体的电阻率分布规律,与地质剖面具有较好的对应关系,均可投入该地区的生产应用。但EH-4连续电导率仪轻便、单点生产效率高,测量结果对断裂构造的分辨能力更好,特别是中浅层的分辨效果。 相似文献
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EH4电磁成像系统在中西部岩溶区地下水勘查中的应用 总被引:19,自引:0,他引:19
简要介绍了EH4电磁成像系统,特点,工作方法。通过在中国西部岩溶区陕西,宁南,内蒙阿拉善的应用实例和效果。说明在中国西部干旱缺水地区,该系统是一种有效的找水方法。 相似文献
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EH4电导率连续成像系统在银厂坡地质勘查中的应用 总被引:1,自引:0,他引:1
通过EH4电磁方法在贵州威宁银厂坡地质勘查中的应用实例,并经过勘查、成矿靶位的确定、工程验证三个阶段工作后,认为EH4电磁方法在地质勘查中具有较好的应用效果。特别是在深部地球物理信息上优于其它常规物探方法,而它相对其它常规物探方法又更具有设备轻、速度快、费用低、精度较高等优点。 相似文献
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EH4电磁成像系统在杭州湾地区晚第四纪地层中的应用 总被引:3,自引:0,他引:3
超音频电磁-大地电磁测深法(EH4)具有不受高阻层屏蔽影响、性能稳定、轻巧便携、操作方便、施工简单和成本低廉等优点,非常适合浅层地质勘探。本文以杭州湾南岸新湾地区的EH4电磁勘探测量结果为例,论述了它在晚第四纪地层基底识别、岩性和沉积相划分、储层和天然气层判别等方面的应用结果。研究表明,EH4电磁成像系统获得的新湾地区晚第四纪地层电阻率-深度剖面,能够详细地反映晚第四纪地层基底连续变化情况,新湾地区晚第四纪沉积层基底为一凹凸不平的不整合面,变化极其复杂。不同沉积环境下形成的沉积物类型和粒度均不同,随着沉积物粒度的减小电阻率亦减小,因而借助电阻率的变化,可以大致划分沉积物及沉积相类型。通过单点电阻率曲线和电阻率-深度剖面图,可以清楚地反映地下介质电阻率变化情况,气层厚度、气层与水层电阻率差值越大,气层在电阻率曲线上的显示越强,反之则越弱。电阻率曲线可以确定砂质透镜体的位置和分布范围,并判断出气层深度和厚度。 相似文献
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The Quadrantids, one of the more active of the annual meteor showers, is unusual for its strong but brief maximum within a broader background of activity. It is also notable for its recent onset, the first observation having been likely made in 1835. Until recently, no parent with a similar orbit had been observed and previous investigators concluded that the stream was quite old, with the stream's recent appearance and sharp peak attributed to a fortuitous convergence of meteoroid orbits. The discovery of the near-Earth Asteroid 2003 EH1 on an orbit very similar to that of the Quadrantids has probably unveiled the parent body of this stream [Jenniskens and Marsden, 2003. 2003 EH1 and the Quadrantids. IAU Circ. 8252]. From simulations of the orbit of this body and of meteoroids released from it at different intervals in the past, we find that both the sharp peak and recent appearance of the Quadrantids can most easily be explained by a release of meteoroids from 2003 EH1 near 1800 AD. This is supported by three lines of evidence. First, the evolution of the observed solar longitude of the Quadrantids over time is consistent with release from 2003 EH1 approximately 200 years ago. Second, numerical simulations of meteoroids released from this parent body at this time match the basic orbital characteristics of the Quadrantid stream well. Finally, these simulations also reveal that the Quadrantid core is well reproduced by a single outburst at perihelion circa 1800, whereas earlier releases result in the shower's appearance in our skies significantly prior to 1835. These results apply to the concentrated central core of the stream: the extended background was likely produced at earlier times. In fact, we find that 2003 EH1 is in a state of Kozai circulation along with a number of other comets and NEAs which may form a larger Quadrantid complex. Using the current total duration of the broader background Quadrantid activity compared to our simulations, we suggest a minimum age of ∼3500 years for the stream as a whole. This also represents the approximate lower limit for the age of the complex. We have further identified five comets as well as nine additional NEAs which may be part of the aforementioned complex, the latter all having Tisserand parameters less than three, further suggesting that the are extinct comet nuclei. 相似文献
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