常规次生晕法在广西资源县云头界钨钼矿找矿中的成果及意义   总被引：3，自引：0，他引：3  

伍静  梁华英  娄峰  张献河  胡光黔 《矿床地质》2010,29(2):301-307

广西资源县云头界钨矿异常区多被表土覆盖,局部出露钨矿化。据钨重砂矿物化学性质较稳定,风化剥蚀后迁移距离较近,而异常区表土覆盖不厚的特点,采用次生晕化探方法对云头界钨矿异常区1.4km2开展化探扫面找矿。根据8条化探剖面线共575个样品分析结果,圈出了6个钨异常区,在其中4个钨异常区施工槽探工程,都发现对应的石英脉型钨矿体。这揭示了该区矿体与次生晕异常的分布具有非常一致的对应关系。次生晕化探异常表明,该矿主矿脉沿走向长度超过1km,矿床规模可望达到中型。常规次生晕法在云头界钨矿异常区找矿效果明显,这对华南风化土层覆盖区钨矿找矿工作有重要的启示。  相似文献   

山东三甲金矿床控矿构造特征及深部预测     

李旭芬 《地质与勘探》2010,46(3):392-399

三甲金矿床位于胶东半岛东部的牟乳金矿带内岔河—三甲断裂的南端,其围岩主要为古老变质岩和昆嵛山花岗岩,为含金石英脉型金矿。本文通过对矿床控矿构造空间形态、活动期次、力学性质以及围岩蚀变等方面的研究,认为三甲金矿主要受控于主断裂,其内不同期次的次级断裂控制了矿体的空间产出位置;控矿断裂至少经历了三期应力改造,早期为压扭兼张扭性的右行剪切变形,中、晚期以张性裂隙为主-形成多金属硫化物石英脉,后期为压扭性裂隙内部充填形成石英+碳酸盐+多金属硫化物。进而总结了矿体在断裂带中分布的规律性。深部地球化学研究表明,三甲金矿的矿石类型、矿石矿物组合具有垂向分带的特征,矿物组合逆向分带与地球化学原生晕所指示的深部成矿叠加相一致。结合矿体在断裂中分布的规律以及原生晕特点,推断三甲金矿在-506m标高以下尚有成矿富集段的存在,此次研究为深部找矿提供了重要的依据。  相似文献   

南黄海盆地中部隆起的形成与演化     

杨长清  董贺平  李刚 《海洋地质前沿》2014,30(7):17-21

南黄海盆地是在前震旦系克拉通基础上发育的中、古生界海相与中、新生界陆相多旋回叠合盆地。通过地震资料解释,结合邻区钻井与区域地质资料,对南黄海盆地中部隆起中、古生代地层及其形成演化进行了研究,结果表明,南黄海盆地中部隆起沉积了较全的中、古生界海相地层,发育第四系—新近系、中—下三叠统青龙组、上二叠统、下二叠统—上泥盆统、中—下志留统,奥陶系—震旦系和前震旦系变质岩系等7套地震地质层序;主要经历了前震旦纪基底形成、震旦纪—早古生代克拉通发育、晚古生代—中三叠世稳定台地—陆内裂陷、晚三叠世—古近纪形成与抬升剥蚀及新近纪-第四纪坳陷沉降5个阶段。  相似文献   

“岩浆热场”说及其成矿意义(下)   总被引：2，自引：0，他引：2  

张旗  金惟浚  李承东  焦守涛 《甘肃地质》2014,23(2):1-20

上篇(张旗等[1])初步讨论了岩浆热场说的概念,本文为下篇,主要谈应用,探讨它与成矿作用的关系。研究表明,岩浆热场说对热液成矿作用有重要的意义,可能解决了岩浆热液成矿作用中许多很难解释和争议很大的问题:如钨锡与金铜为什么相伴的问题,矿床为什么大多是多金属成矿的问题,远离侵入体的夕卡岩成因问题,成矿为什么滞后于花岗岩的问题,为什么有些岩体成矿,有些岩体不成矿的问题,为什么大规模岩浆活动与大规模成矿作用息息相关的问题等。岩浆热场与煤和油气成藏有关是一个重要的发现。岩浆热场对煤和油气生成、运移、聚集的影响主要表现在加速烃源岩的热演化,使生油门限变浅,使烃源岩进入高成熟或过成熟,使烃源岩中残余有机质丰度降低。令人感兴趣的是,岩浆热场说还导出了一个"成矿组合"的概念,所谓成矿组合是指在一个或大或小的区域内,在岩浆活动集中的时间段范围内,在热场的统一作用下所形成和影响的所有矿床,不论成因和矿种,均属于一个成矿组合。它包括下述4种类型的矿床:岩浆热液矿床、热泉型矿床、层状热液矿床及生物有机质矿床等。岩浆热场说对于找矿也有启示:首先,我们可以从3个不同的级别上(大规模岩浆活动级别;成矿带、成矿区、矿集区级别;单个矿床级别)规划找矿布局;其次,在岩浆热场的统一影响下将金属矿床和非金属矿床、热液矿床和沉积矿床、无机质矿床和有机质矿床联系起来;第三,推进不同类型矿床研究的互补和交流。看来,岩浆热场对于成矿的作用是最值得学术界关注的,它也许可以改变我们目前对成矿作用的某些根深蒂固的认识,开拓出一个新的领域,推进矿床学研究进入新的时代。  相似文献   

东川-易门式铜矿床成矿作用研究的几个问题     

冉崇英  吴鹏 《大地构造与成矿学》2014,(4)

从宏观基础地质入手,按矿床学的一些基本概念,针对东川-易门铜矿床地质地球化学特征,探讨了一些存在争议的重要问题。研究认为:狮山段是绿汁江组下部独立存在的地层层位;东川-易门式铜矿床属沉积-改造成因,其中的层状铜矿属沉积成岩成因,不是"热液成矿";所谓东川-易门式矿床(稀矿山除外)为"喷流沉积成矿"或"岩浆叠加",尚依据不足;刺穿体是构造作用产物,对成矿有利,是良好的找矿标志,其中的角砾岩主要是沉积角砾岩与构造角砾岩,或沉积-构造角砾岩,不足以冠名"隐爆角砾岩(筒)"。  相似文献   

Transfers between libration-point orbits in the elliptic restricted problem     

L. A. Hiday-Johnston  K. C. Howell 《Celestial Mechanics and Dynamical Astronomy》1994,58(4):317-337

A strategy is formulated to design optimal time-fixed impulsive transfers between three-dimensional libration-point orbits in the vicinity of the interiorL ₁ libration point of the Sun-Earth/Moon barycenter system. The adjoint equation in terms of rotating coordinates in the elliptic restricted three-body problem is shown to be of a distinctly different form from that obtained in the analysis of trajectories in the two-body problem. Also, the necessary conditions for a time-fixed two-impulse transfer to be optimal are stated in terms of the primer vector. Primer vector theory is then extended to non-optimal impulsive trajectories in order to establish a criterion whereby the addition of an interior impulse reduces total fuel expenditure. The necessary conditions for the local optimality of a transfer containing additional impulses are satisfied by requiring continuity of the Hamiltonian and the derivative of the primer vector at all interior impulses. Determination of the location, orientation, and magnitude of each additional impulse is accomplished by the unconstrained minimization of the cost function using a multivariable search method. Results indicate that substantial savings in fuel can be achieved by the addition of interior impulsive maneuvers on transfers between libration-point orbits.An earlier version was presented as Paper AAS 92–126 at the AAS/AIAA Spaceflight Mechanics Meeting, Colorado Springs, Colorado, February 24–26, 1992.  相似文献   

Anisotropic Inhomogeneous Riemann S-Ellipsoids in Spheroidal Halos. I.     

M. G. Abrahamyan 《Astrophysics》2005,48(4):514-531

The classical Riemann S-ellipsoids are generalized to account for a Ferrers inhomogeneity in the mass distribution, a three-dimensional anisotropy of the velocity dispersions, and the gravitation of a spheroidal halo. The Ferrers inhomogeneity does not affect the equilibrium and stability conditions for the ellipsoids, but only changes the numerical coefficients in the equilibrium parameters. The anisotropy of the velocity dispersions changes both the equilibrium conditions and the criterion for stability of the ellipsoids, either extending or limiting the region in which the ellipsoids exist. A halo extends this region in all cases and stabilizes the ellipsoids. The observed of the velocity dispersions of stars in the neighborhood of the sun are obtained using the inhomgeneous model. __________ Translated from Astrofizika, Vol. 48, No. 4, pp. 613–632 (November 2005).  相似文献   

Cuspy dark matter haloes and the Galaxy     

J.J. Binney  N.W. Evans 《Monthly notices of the Royal Astronomical Society》2001,327(2):L27-L31

The microlensing optical depth to Baade's Window constrains the minimum total mass in baryonic matter within the Solar circle to be greater than ∼     , assuming the inner Galaxy is barred with viewing angle ∼20°. From the kinematics of solar neighbourhood stars, the local surface density of dark matter is ∼     . We construct cuspy haloes normalized to the local dark matter density and calculate the circular-speed curve of the halo in the inner Galaxy. This is added in quadrature to the rotation curve provided by the stellar and ISM discs, together with a bar sufficiently massive so that the baryonic matter in the inner Galaxy reproduces the microlensing optical depth. Such models violate the observational constraint provided by the tangent-velocity data in the inner Galaxy (typically at radii     . The high baryonic contribution required by the microlensing is consistent with implications from hydrodynamical modelling and the pattern speed of the Galactic bar. We conclude that the cuspy haloes favoured by the cold dark matter cosmology (and its variants) are inconsistent with the observational data on the Galaxy.  相似文献   

A search for previously unrecognized metal-poor subdwarfs in the Hipparcos astrometric catalogue     

I. Neill Reid  F. van Wyk  F. Marang  G. Roberts  D. Kilkenny  S. Mahoney 《Monthly notices of the Royal Astronomical Society》2001,325(3):931-962

We have identified 317 stars included in the Hipparcos astrometric catalogue that have parallaxes measured to a precision of better than 15 per cent, and the location of which in the ( M _V ,( B − V ) _T ) diagram implies a metallicity comparable to or less than that of the intermediate-abundance globular cluster M5. We have undertaken an extensive literature search to locate Strömgren, Johnson/Cousins and Walraven photometry for over 120 stars. In addition, we present new UBV ( RI )_C photometry of 201 of these candidate halo stars, together with similar data for a further 14 known metal-poor subdwarfs. These observations provide the first extensive data set of R _C I _C photometry of metal-poor, main-sequence stars with well-determined trigonometric parallaxes. Finally, we have obtained intermediate-resolution optical spectroscopy of 175 stars.
47 stars still lack sufficient supplementary observations for population classification; however, we are able to estimate abundances for 270 stars, or over 80 per cent of the sample. The overwhelming majority have near-solar abundance, with their inclusion in the present sample stemming from errors in the colours listed in the Hipparcos catalogue. Only 44 stars show consistent evidence of abundances below [Fe/H]=−1.0 . Nine are additions to the small sample of metal-poor subdwarfs with accurate photometry. We consider briefly the implication of these results for cluster main-sequence fitting.  相似文献   

HST/STIS observations of the high-velocity interstellar cloud HVC 291.2−41.2+80: a warm, mainly ionized high-velocity cloud     

N. Lehner  F. P. Keenan  K. R. Sembach 《Monthly notices of the Royal Astronomical Society》2001,323(4):904-910

We present intermediate-resolution HST /STIS spectra of a high-velocity interstellar cloud ( v _LSR=+80 km s⁻¹) towards DI 1388, a young star in the Magellanic Bridge located between the Small and Large Magellanic Clouds. The STIS data have a signal-to-noise ratio (S/N) of 20–45 and a spectral resolution of about 6.5 km s⁻¹ (FWHM). The high-velocity cloud absorption is observed in the lines of C  ii , O  i , Si  ii , Si  iii , Si  iv and S  iii . Limits can be placed on the amount of S  ii and Fe  ii absorption that is present. An analysis of the relative abundances derived from the observed species, particularly C  ii and O  i , suggests that this high-velocity gas is warm ( T _k∼10³–10⁴ K) and predominantly ionized. This hypothesis is supported by the presence of absorption produced by highly ionized species, such as Si  iv . This sightline also intercepts two other high-velocity clouds that produce weak absorption features at v _LSR=+113 and +130 km s⁻¹ in the STIS spectra.  相似文献