四川省康定县三碉金矿床岩矿石化学成分特征及构造环境          下载免费PDF全文

何阳阳  蒋双宇  邓成雪 《地质找矿论丛》2020,35(2):129-137

康定县境内的三碉金矿床是大渡河金矿成矿集中区内的典型矿床。本文基于野外实地调查取样、实验室分析测试工作,通过对岩矿石地球化学特征及构造环境进行研究,结果表明:1)从无矿石英→含矿石英,SiO_2、Al_2O_3、CaO等含量均有所减少,TiO_2、MnO、K_2O、Na_2O等变化范围不大,Fe_2O_3和FeO等则有明显的增高。2)斜长角闪岩的原岩为基性火山岩,δEu主要表现为正异常特征;黑云母花岗岩具有中钾钙碱性特征,形成于造山晚期,δEu表现为明显的负异常特征。即三碉金矿的形成过程中,硅铝质矿物在减少,载金金属矿物在增多;含矿流体混染和交代长英质岩浆减弱抵消负铕异常导致斜长角闪岩δEu值逐渐过渡为正异常;黑云母花岗岩δEu为负异常,是早期斜长石的晶出带走Eu作用的结果。3)矿区断裂与矿床的形成密切相关,为成矿流体的上升运移提供了有利的通道,并提供含矿石英脉的沉聚空间。  相似文献   

Cosmological perturbation theory and the spherical collapse model — III. The velocity divergence field and the Ω dependence     

Pablo Fosalba  & Enrique Gaztañaga 《Monthly notices of the Royal Astronomical Society》1998,301(2):535-546

Cosmological perturbation theory (PT) is a useful tool to study the cumulants of the density and velocity fields in the large-scale structure of the Universe. In Papers I and II of this series we saw that the spherical collapse (SC) model provides the exact solution to PT at tree-level and gives a good approximation to the loop corrections (next-to-leading orders), indicating negligible tidal effects. Here, we derive predictions for the (smoothed) cumulants of the velocity divergence field θ ≡ ▽ ⊙  v for an irrotational fluid in the SC model. By comparing these with the exact analytic results of Scoccimarro &38; Frieman, it is shown that, at least for the unsmoothed case, the loop corrections to the cumulants of θ are dominated by tidal effects. However, most of the tidal contribution seems to cancel out when computing the hierarchical ratios, T _J  = 〈θ ^J 〉 / 〈θ²〉  ^{J −1}. We also extend the work presented in Papers I and II to give predictions for the cumulants of the density and velocity divergence fields in non-flat spaces. In particular, we show the equivalence between the spherically symmetric solution to the equations of motion in the SC model (given in terms of the density) and that of the Lagrangian PT approach (given in terms of the displacement field). It is shown that the Ω dependence is very weak for both cosmic fields even at one loop (a 10 per cent effect at most), except for the overall factor f (Ω) that couples to the velocity divergence.  相似文献   

DO WE NEED TO MODEL PLATES AT ALL?   总被引：2，自引：0，他引：2  

Morrison  Smart  & Taff 《Monthly notices of the Royal Astronomical Society》1998,296(1):66-76

The historical method of obtaining equatorial coordinates for stars observed via astronomical photography has been to convert the measured coordinates to equatorial coordinates with the aid of a plate model which corrects for a variety of effects. However, we now have at our disposal novel smoothing techniques, of considerable generality, which in conjunction with modern star catalogues can reproduce the essence of the plate model while dramatically minimizing both the fortuitous and systematic errors of observation. In this paper we demonstrate that, with this technique and extant catalogues, one can obtain, with at least the same precision and better accuracy, the information necessary to transform the measured coordinates successfully into standard coordinates by a process that involves no sophisticated model for the plate. Using external checks we estimate the increase in accuracy to be of the order of 25 per cent.  相似文献   

An optimal extraction algorithm for imaging photometry     

Tim Naylor 《Monthly notices of the Royal Astronomical Society》1998,296(2):339-346

This paper is primarily an investigation of whether the 'optimal extraction' techniques used in CCD spectroscopy can be applied to imaging photometry. It is found that using such techniques provides a gain of around 10 per cent in signal-to-noise ratio over normal aperture photometry. Formally, it is shown to be equivalent to profile fitting, but offers advantages of robust error estimation, freedom from bias introduced by mis-estimating the point spread function, and convenience. In addition some other techniques are presented, which can be applied to profile fitting, aperture photometry and the 'optimal' photometry. Code implementing these algorithms is available at http://www.astro.keele.ac.uk/~timn/.  相似文献   

An excursion set model for the distribution of dark matter and dark matter haloes     

Ravi K. Sheth 《Monthly notices of the Royal Astronomical Society》1998,300(4):1057-1070

A model of the gravitationally evolved dark matter distribution, in the Eulerian space, is developed. It is a simple extension of the excursion set model that is commonly used to estimate the mass function of collapsed dark matter haloes. In addition to describing the evolution of the Eulerian space distribution of the haloes, the model allows one to describe the evolution of the dark matter itself. It can also be used to describe density profiles, on scales larger than the virial radius of these haloes, and to quantify the way in which matter flows in and out of Eulerian cells. When the initial Lagrangian space distribution is white noise Gaussian, the model suggests that the Inverse Gaussian distribution should provide a reasonably good approximation to the evolved Eulerian density field, in agreement with numerical simulations. Application of this model to clustering from more general Gaussian initial conditions is discussed at the end.  相似文献   

Numerical simulations of protostellar encounters — II. Coplanar disc–disc encounters     

S. J. Watkins  A. S. Bhattal  H. M. J. Boffin  N. Francis  & A. P. Whitworth 《Monthly notices of the Royal Astronomical Society》1998,300(4):1205-1213

It is expected that an average protostar will undergo at least one impulsive interaction with a neighbouring protostar whilst a large fraction of its mass is still in a massive, extended disc. Such interactions must have a significant impact upon the evolution of the protostars and their discs.   We have carried out a series of simulations of coplanar encounters between two stars, each possessing a massive circumstellar disc, using an SPH code that models gravitational, hydrodynamic and viscous forces. We find that during a coplanar encounter, disc material is swept up into a shock layer between the two interacting stars, and the layer then fragments to produce new protostellar condensations. The truncated remains of the discs may subsequently fragment; and the outer regions of the discs may be thrown off to form circumbinary disc-like structures around the stars. Thus coplanar disc–disc encounters lead efficiently to the formation of multiple star systems and small- N clusters, including substellar objects.  相似文献   

Non-parametric reconstruction of distribution functions from observed galactic discs     

C. Pichon  & E. Thiébaut 《Monthly notices of the Royal Astronomical Society》1998,301(2):419-434

A general inversion technique for the recovery of the underlying distribution function for observed galactic discs is presented and illustrated. Under the assumption that these discs are axisymmetric and thin, the proposed method yields a unique distribution compatible with all the observables available. The derivation may be carried out from the measurement of the azimuthal velocity distribution arising from positioning the slit of a spectrograph along the major axis of the galaxy. More generally, it may account for the simultaneous measurements of velocity distributions corresponding to slits presenting arbitrary orientations with respect to the major axis. The approach is non-parametric, i.e. it does not rely on a particular algebraic model for the distribution function. Special care is taken to account for the fraction of counter-rotating stars, which strongly affects the stability of the disc. An optimization algorithm is devised — generalizing the work of Skilling &38; Bryan — to carry this truly two-dimensional ill-conditioned inversion efficiently. The performance of the overall inversion technique with respect to the noise level and truncation in the data set is investigated with simulated data. Reliable results are obtained up to a mean signal-to-noise ratio of 5, and when measurements are available up to 4  R _e. A discussion of the residual biases involved in non-parametric inversions is presented. The prospects of application of the algorithm to observed galaxies and other inversion problems are discussed.  相似文献   

Automated classification of stellar spectra — II. Two-dimensional classification with neural networks and principal components analysis     

Coryn A. L. Bailer-Jones  Mike Irwin  & Ted von Hippel 《Monthly notices of the Royal Astronomical Society》1998,298(2):361-377

We investigate the application of neural networks to the automation of MK spectral classification. The data set for this project consists of a set of over 5000 optical (3800–5200 Å) spectra obtained from objective prism plates from the Michigan Spectral Survey. These spectra, along with their two-dimensional MK classifications listed in the Michigan Henry Draper Catalogue, were used to develop supervised neural network classifiers. We show that neural networks can give accurate spectral type classifications (σ₆₈= 0.82 subtypes, σ_rms= 1.09 subtypes) across the full range of spectral types present in the data set (B2–M7). We show also that the networks yield correct luminosity classes for over 95 per cent of both dwarfs and giants with a high degree of confidence.   Stellar spectra generally contain a large amount of redundant information. We investigate the application of principal components analysis (PCA) to the optimal compression of spectra. We show that PCA can compress the spectra by a factor of over 30 while retaining essentially all of the useful information in the data set. Furthermore, it is shown that this compression optimally removes noise and can be used to identify unusual spectra.   This paper is a continuation of the work carried out by von Hippel et al. (Paper I).  相似文献   

编制地壳垂直运动速率等值线图的有限元法   总被引：2，自引：0，他引：2  

李家权  张勤 《大地测量与地球动力学》1998,(3)

根据地壳垂直运动研究中的均衡理论,建立描述地壳垂直运动速率空间分布的数学模型,并提出应用有限元法拟合地壳垂直运动速率面的理论和方法。通过计算验证,说明有限元法可实现对地壳垂直运动速率面的精确逼近,是编制地壳垂直运动速率等值图的有效方法。  相似文献   

华北克拉通基性火山岩高场强元素对Ar-Pt界限及新生代地幔源区特征的示踪   总被引：5，自引：0，他引：5       下载免费PDF全文

刘勇胜  高山  骆庭川 《地球科学》1998,23(5):91

华北克拉通不同时代基性火山岩存在向富集方向演化的趋势,并出现明显的Ａｒ－Ｐｔ界限和新生代异常．元古宙基性火山岩比太古宙富集大部分高场强元素（ＨＦＳＥ）和轻稀土元素（ＬＲＥＥ）,ＲＥＥ分异程度显著增加,而且相容性接近的不相容元素（如Ｎｂ,Ｔａ）的相对不相容性发生了改变．新生代玄武岩ＨＦＳＥ及Ｎｉ高度富集,ＲＥＥ强烈分异,δ（Ｅｕ）值最高．Ａｒ－Ｐｔ界限可能与地幔熔融时物理条件（如氧逸度）的改变和地幔富集作用有关．新生代玄武岩独特的地球化学特征可能主要反映了地幔源区的特殊性———“似ＯＩＢ型”富集地幔,其形成既可能有携带远洋沉积物的俯冲古老玄武岩洋壳部分熔融残余的贡献,也可能有直接循环（如通过拆沉作用）的陆壳物质的贡献,同时还可能涉及了地幔柱活动的影响．  相似文献