藏北商旭造山型金矿床的发现及意义

西藏双湖县商旭金矿床位于班公湖-怒江缝合带中段。矿体赋存于中-下侏罗统木嘎岗日群浅变质复理石中,受北西西向断裂构造控制,呈透镜体状、脉状,或者似层状产出;矿石矿物以自然金为主,矿石类型为石英脉型和蚀变岩型,围岩蚀变特征明显。该矿床主要受地层及构造因素控制,矿区的构造、围岩蚀变、矿物、地球化学异常等可作为找矿标志。野外地质调查和矿床对比研究显示,商旭金矿床在矿物共生组合、蚀变类型、构造类型等方面,与典型的造山型金矿床相似,其成因类型属于造山型金矿床。商旭金矿床的发现为班公湖-怒江成矿带金等贵金属矿产的地质找矿工作开辟了新的方向。     

安徽金寨三仙山地区梅山群碎屑岩成分及其对物源区构造属性和地层时代的意义

安徽金寨三仙山地区位于大别山北缘,该地梅山群主要为一套轻微变质的碎屑岩系。砂岩碎屑组分统计表明,砂岩类型主要为岩屑石英砂岩、岩屑石英杂砂岩,石英、长石、岩屑的平均含量为87.21%、1.67%、9.64%,杂基含量为15%,石英几乎全为单晶石英（95.79%）,长石以斜长石为主,岩屑主要为沉积岩屑（75.49%）,其次为变质岩屑（24.51%）。碎屑岩地球化学元素平均含量为：SiO₂（75.99%）,Al₂O₃（11.96%）,MgO（0.72%）,CaO（0.10%）,Fe₂O₃（4.02%）,K₂O（1.70%）,Na₂O（0.26%）。ΣREE=170.49×10^-6（74.49×10^-6～309.42×10^-6）,LREE/HREE=11.16（7.89～14.26）,轻稀土略有富集,δEu=0.72（0.59～0.90）,La/Yb=22.08（13.01～31.18）,（La/Yb）_N=14.89（8.77～21.02）,δCe=0.84（0.42～0.97）。碎屑岩地球化学特征指示三仙山地区梅山群母岩主要为古老沉积岩、长英质火山岩和古老变质基底,具有多重物源区。梅山群构造背景较复杂,主要为被动大陆边缘和活动大陆边缘,其次为大陆岛弧。三仙山地区梅山群碎屑岩的源岩成分、构造背景与商城-固始地区石炭系有很大差别,故其地层时代有待于进一步研究。     

嵩山地区熊耳群火山岩岩石学、地球化学及成因探讨

近年在河南省嵩山地区发现有熊耳群火山岩地层。通过岩石学、地球化学特征及成因研究,认为嵩山地区熊耳群火山岩主要为弱过铝质流纹岩,属于高钾钙碱性系列-钾玄岩系列,以高硅、高钾、过铝、贫钠、贫钙镁为特征;轻稀土富集,重稀土亏损,轻重稀土分馏较为明显,Eu强烈负异常,Ce微弱负异常;富Ba而贫Sr,Rb,U,富Zr而贫Nb,Th,Hf,Ta;岩石属A型岩浆作用产物,形成于板内拉张环境。     

陕西小秦岭地区熊耳群火山岩型铁(钛)矿及资源潜力

对小秦岭地区熊耳群地层的分布作了概述。在熊耳群地层分布区划出了坝源—洛源(A区)、三岔—石门(B区)和西峪河—梧桐河(C区)三个火山岩型铁矿资源潜力区。阐述了各潜力区的铁矿成矿条件,对潜在资源量作了测算。预测全区300 m以上铁矿潜在资源量为≥9.4亿吨,钛铁矿≥300万吨。     

Tectonic control on third‐order sequences in a siliciclastic ramp‐style basin: An example from the Roper Superbasin (Mesoproterozoic), northern Australia

TThe Roper Group is a cyclic, predominantly marine, siliciclastic succession of Calymmian (Early Mesoproterozoic) age. It has a distribution of at least 145 000 km² and a maximum known thickness of ～5000 m. In the Roper River district the middle part of the Roper Group (～1300 m thick) is characterised by the cyclical alternation of mudstone and sandstone units, and can be divided into six third‐order depositional sequences. A typical sequence is broadly progradational in aspect, and comprises a lower, mudstone‐rich, storm‐dominated shelf succession (up to 330 m thick), and a sequence‐capping unit dominated by tidal‐platform cross‐bedded sandstone (up to 80 m thick); both are interpreted as highstand systems tracts. Transgressive strata are poorly represented but where present are characterised by paralic to fluvial redbed assemblages that include ooidal ironstone. Roper Group sequences lack a distinct condensed section and sequence boundaries are mostly conformable. Erosional contacts separate mud‐rich shelf facies from sequence‐capping sandstones. We infer that these erosion surfaces were generated by episodic flexural tectonism, which also generated the accommodation and sediment supply for Roper sequences.     

Neoproterozoic (Cryogenian) stromatolites from the Wolfe Basin,east Kimberley,Western Australia: Correlation with the Centralian Superbasin

Linella avis, an early to middle Neoproterozoic (Tonian to Cryogenian) stromatolite, occurs in the Eliot Range Dolomite, part of the Ruby Plains Group in the Wolfe Basin, east Kimberley. Previously, this dolomite was assigned to the Mesoproterozoic Bungle Bungle Dolomite in the Osmond Basin, which contains a different suite of stromatolites. Linella avis, which also occurs in the Neoproterozoic Bitter Springs Formation of the Amadeus Basin, central Australia, appears to be restricted to rocks aged around 850 to 800 Ma. The presence of L. avis indicates that the Ruby Plains Group is a probable correlative of the Heavitree Quartzite and Bitter Springs Formation, and is probably much younger than the Bungle Bungle Dolomite. If the correlation suggested here is correct, the Wolfe Basin, together with the Amadeus and Ngalia Basins, formed part of the Centralian Superbasin.     

实验标定的一种地质温压计及其应用

本文简略回顾了堇青石-石榴石-矽线石-石英地质温压计的研究历史,并介绍由Aranovich等人完成的最新实验研究。以内蒙古南部贺兰山群的麻粒岩相矽线石榴堇青片麻岩的温压计算为例,用Aranovich等人实验标定的温压计计算结果与石榴石-堇青石Fe-Mg交换反应温度计和石榴石-斜长石-矽线石-石英压力计的计算结果相当吻合;而应用含有假定的热力学参数的哈奇森的温压计与其它温压计计算结果有较大差别,温度明显偏低,与岩石形成于麻粒岩相变质条件这一地质事实不符。     

Giant HVC’s and the Rotation Curves of the Milky Way and M31

We have modelled, for the cases of Milky Way and M31, the effects on the galactic discs, of the arrival at high velocity (≥150 km s⁻¹) of giant HI clouds, with masses of up to 10⁸M⊙. Predictions are compared with the detailed structure of the observed rotation curves for these two galaxies. The model explains the rises and falls observed at large distances from the centre of each galaxy, distributed with a degree of regularity in radius, in terms of a specific type of perturbations driven by the infall of the high velocity clouds (HVC's) arriving from the intracluster medium of the Local Group. The underlying rotation curve is explained conventionally via the distribution of the baryonic and dark matter components of the galaxy in question. This scenario, though tested here on the two major Local Group objects, is in principle applicable to galaxies undergoing minor mergers with subgalactic mass gas clouds.     

论辽南上前寒武系的划分与对比

辽南上元古界的区域对比的关键是如何与蓟县层型、峡东层型的衔接或对比。作者认为辽南群是介于北方的青白口群与南方的震旦系之间的层位，仅金县群才相当于震旦系，震旦系与寒武系的界线则应置于兴民村组与葛屯组之间。     

Dark matter in dwarf spheroidals – II. Observations and modelling of Draco

We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude   V ≈19.5  with a mean velocity precision of ≈2 km s⁻¹. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.
We find statistically strong evidence of a rising velocity dispersion consistent with a dark matter halo that has a gently rising rotation curve. There is a <2 σ signature of rotation about the long axis, inconsistent with tidal disruption as the source of the rising dispersion. By comparing our data set with earlier velocities, we find that Draco probably has a binary distribution and fraction comparable to those in the solar neighbourhood.
We apply a novel maximum likelihood algorithm and fit the velocity data to a two parameter spherical model with an adjustable dark matter content and velocity anisotropy. Draco is best fit by a weakly tangentially anisotropic distribution of stellar orbits in a dark matter halo with a very slowly rising rotation law  ( v _circ∝ r ^0.17)  . We are able to rule out both a mass-follows-light distribution and an extended halo with a harmonic core at the 2.5 to 3 σ significance level, depending on the details of our assumptions about Draco's stellar binary population. Our modelling lends support to the idea that the dark matter in dwarf spheroidals is distributed in the form of massive, nearly isothermal haloes.