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

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.     

Dark haloes of spiral galaxies: ISO photometry

We exclude hydrogen-burning stars, of any mass above the hydrogen-burning limit and any metallicity, as significant contributors to the massive haloes deduced from rotation curves to dominate the outer parts of spiral galaxies. We present and analyse images of four nearly edge-on bulgeless spiral galaxies (UGC 711, NGC 2915, UGC 12426, UGC 1459) obtained with ISOCAM (The CAMera instrument on board the Infrared Space Observatory ) at 14.5 and 6.75 μm. Our sensitivity limit for detection of any diffuse infrared emission associated with the dark haloes in these galaxies is a few tens of μJy per 6 × 6 arcsec² pixel, with this limit currently set by remaining difficulties in modelling the non-linear behaviour of the detectors. All four galaxies show zero detected signal from extended non-disc emission, consistent with zero halo-like luminosity density distribution. The 95 per cent upper limit on any emission, for NGC 2915 in particular, allows us to exclude very low mass main-sequence stars ( M  > 0.08 M⊙) and young brown dwarfs (≲1 Gyr) as significant contributors to dark matter in galactic haloes. Combining our results with those of the Galactic microlensing surveys, which exclude objects with M  < 0.01 M⊙, excludes almost the entire possible mass range of compact baryonic objects from contributing to Galactic dark matter.     

Constraining the Mass Distribution of Cluster Galaxies by Weak Lensing

Analysing the weak lensing distortions of the images of faint background galaxies provides a means to constrain the average mass distribution of cluster galaxies and potentially to test the extent of their dark matter haloes as a function of the density of their environment. The observable image distortions are a consequence of the interplay between the effects of a global cluster mass distribution and the perturbations resulting from individual cluster galaxies. Starting from a reconstruction of the cluster mass distribution with conventional techniques, we apply a maximum likelihood method to infer the average properties of an ensemble of cluster galaxies. From simulations this approach is found to be reliable as long as the galaxies including their dark matter haloes only contribute a small fraction to the total mass of the system. If their haloes are extended, the galaxies contain a substantial mass fraction. In this case our method is still applicable in the outer regions of clusters, where the surface mass density is low, but yields biased estimates of the parameters describing the mass profiles of the cluster galaxies in the central part of the cluster. In that case it will be necessary to resort to more sophisticated strategies by modelling cluster galaxies and an underlying global mass distribution simultaneously. We conclude that galaxy–galaxy lensing in clusters provides a unique means to probe the presence and extent of dark haloes of cluster galaxies.     

Mass constraints from multiphase cooling flow models

I review the multiphase cooling flow equations that reduce to a relatively simple form for a wide class of self-similar density distributions described by the single parameter, k , first introduced by Nulsen. It is shown that steady-state cooling flows are not consistent with all possible emissivity profiles, which can therefore be used as a test of the theory. In combination, they provide strong constraints on the temperature profile and mass distribution within the cooling radius. The model is applied to ROSAT HRI data for three rich clusters. At one extreme ( K  ∼ 1) these show evidence for cores in the mass distribution of size 110–140 h ⁻¹₅₀ kpc and have temperatures that decline towards the flow centre. At the other ( k ∈ ∞), the mass density and gas temperature both rise sharply towards the flow centre. The former are more consistent with observations which usually show a lower emission-weighted temperature within the cooling flow than from the cluster as a whole. The requirement that the solutions have a temperature gradient that is non-increasing towards the cluster centre limits the matter density gradient to be shallower than ρ_grav ∝∼  r ^−1.2 in the cluster core.     

鲁山棚沟金矿床包裹体特征及找矿意义

棚沟金矿床赋存于华北古陆块南缘前寒武纪花岗岩中，在空间上受区域韧性剪切带中的燕山末期花岗斑岩控制。根据矿床地质特点判断属中低温热液型金矿。通过岩石矿物组合及包裹体组成、性质、同位素等测试，确定成矿物质来源于围岩，成矿流体来源于变质水且有岩浆水与雨水的混入。通过电子探针测定的岩矿组分，计算围岩成岩及变质温度，以及成矿温度、压力和沉淀条件，认为金矿床的成矿作用，主要表现为减压环境中的岩浆热液充填和交代蚀变，以及热液的泡腾作用。从找矿标志角度确定富ＣＯ２的泡腾包裹体群、液相高硫富ＨＣＯ－３、气相高ＣＯ２和高ＣＯ２／Ｈ２Ｏ比值等参数是寻找此类金矿的重要标志     

栖霞市马家窑金矿床成矿流体地球化学特征

马家窑金矿床是胶东地区比较典型的石英脉型金矿床代表,属中低温热液矿床,成矿流体盐度较低,气相成分以H2O,CO2为主,其次是Na^＋,Ca^＋和Cl^-,K^＋和F^-较贫,流体的成分与大气降水热液相类似。成矿流体的H,O同位素值则反映大气降水在不同温度和不同水／岩值条件下与栖霞超单元回龙夼单元交换后的分布特征,认为马家窑金矿床的成矿热液属大气降水成因。     

山东蓬莱地区侯格庄金矿床流体包裹体特征

侯格庄金矿床位于胶东栖(霞)-蓬(莱)金成矿带大柳行金矿田东南部。该文采用包裹体显微测温方法对金矿石中石英矿物内残留的流体包裹体进行研究,总结了金矿石石英矿物中的流体包裹体特征,并对该矿床成矿流体来源、矿床成因进行了研究。研究表明,该矿床石英矿物中流体包裹体以纯液包裹体为主,次为H_2O-CO_2气液两相包裹体及H_2O-CO_2三相包裹体,未见含子矿物包裹体。均一温度在109~396℃,盐度在2.9~22.44wt%NaCl,密度在0.64~1.06g/cm~3之间,估算成矿压力为128~340MPa,成矿深度约4.4~11.6km。该矿床至少经历了2个矿化期次,成矿流体为中低温、低盐度、低密度流体,流体来源于天水与岩浆水的混合产物,属中低温、中浅成热液矿床。     

黄铁矿中不同赋存状态金的测试及意义 —以胶莱盆地金矿中黄铁矿为例

本文论述了黄铁矿中晶格金、自然金、石英包体金的分离技术及测试方法,它可用于研究金矿载金矿物黄铁矿中不同赋存状态金与成矿的关系。运用本方法对胶莱盆地典型金矿中主成矿阶段黄铁矿三种赋存状态的金进行了测试,发现以自然金为主,且自然金含量比例差别不大,说明盆地中的金矿可能具有相同成矿流体和环境。通过对含矿与不含矿黄铁矿中离子晶格金含量研究,进行了靶区预测验证。研究发现黄铁矿中存在石英包体金,且部分金矿中石英包体金含量较高,普通测试方法可能丢失该类金,造成样品分析结果偏低,进而出现丢矿或资源量估算不准确的现象。     

鄂尔多斯盆地南部直罗油田长8油层油气沸腾包裹体群研究

运用激光拉曼光谱、包裹体充填度测定等方法对鄂尔多斯盆地直罗油田富南3井、6井长8油层裂缝岩芯充填物中包裹体群进行分析,发现富南3井、6井与英旺油田英16井长8油层中油气沸腾包裹体群完全相同,密集分布的气泡不停晃动,证实油气沸腾包裹体群不是孤立的、偶然的地质现象。富南3井、6井和英16井长8油层裂缝岩芯的原始裂缝性质为滑动-剪切裂缝和剪切裂缝,在区域构造的作用下,反复发生拉张-挤压交替活动;在拉张发生的瞬间,与裂缝沟通的油层里的原油发生减压沸腾,原油中的轻质馏分和其他流体进入裂缝空间;在随后的挤压发生时,裂缝基本封闭,一部分流体返回原来的油层,一部分被挤到别的裂隙空间形成新的油藏;残留在裂缝里的碳酸钙,在较高的地层压力下逐渐结晶,并把残留的轻质馏分包裹,形成油气包裹体;这些油气包裹体形成压力较高,又包裹着成分类似液化气的轻质馏分,在常温常压下就处于沸腾状态;这样的过程反复进行,在裂缝充填物中形成了沿着晶体生长线以及成片、成带分布的油气沸腾包裹体群。上述油气沸腾包裹体群的形成过程就是油气的地震泵运移机制,丰富了油气运移地震泵地质模型。     

Periodic exposure to ambient solar irradiance benefits the growth of juvenile seedlings of Hizikia fusiformis

In our trials, from 2007 to 2008, of mass production of seedlings of Hizikia fusiformis using synchronization techniques, problems of a dark thalli phenomenon and epiphytes contamination severely threatened the health of juvenile seedlings. In this investigation, we optimized conditions for improving the growth of juvenile seedlings. Seven string collectors were seeded with zygotes and a series of experiments were conducted including direct exposure to solar irradiance, co-culture with Ulva spp. and treatme...