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.     

江西省小龙钨矿深部地球化学找矿远景预测

运用岩石地球化学找矿方法预测了小龙钨矿区深部Ｃｕ、Ａｇ、Ｗ矿化富集规律及其找矿远景。认为矿区南涪７、１１勘探线八中段以下存在Ｃｕ、Ａｇ、Ｗ矿体可能;北部０勘探线六中段Ｃｕ、Ａｇ晕已收敛,深部存在Ｃｕ、Ａｇ矿体可能性不大,而Ｗ的强度和规模在八中段以下呈显著增大趋势,深部可能存在Ｗ矿体,为矿区深部部署坑道工程提供了准确的地球化学依据。     

The globular cluster system of the Sagittarius dwarf spheroidal galaxy: the age of Terzan 8

We present deep V - and I -band CCD photometry of the globular cluster Terzan 8, recently found to be a member of the globular cluster system of the Sagittarius dwarf spheroidal galaxy. We accurately estimate the metallicity of Terzan 8, and provide the first direct determination of the colour excess toward this cluster. Our robust age estimate confirms that this cluster is indeed coeval with typical Galactic globulars of comparable metal content, and thus it is probably significantly older than at least two other Sagittarius clusters, Terzan 7 and Arp 2. The implications of this result on the star formation history of the Sagittarius galaxy are briefly discussed.     

上置晕与物质的“类气相”垂向迁移

阐明了上置晕的术语概念,指出文献中术语运用的失当之处,归纳出以上置晕为基础的各类隐伏矿化探方法。按传统的观念,上置晕主要是由不同形式的水迁移作用造成的。地气法、ＭＦＥ法和离子晕法的出现,揭示出在覆盖层中存在着一种新的元素迁移机制,即元素以非常细小的固相微粒随地气流迁移。一系列实验和实测结果表明,这种固相微粒可能是纳米粒径的物质,它们具有类气相的性状,故可将这种迁移机制称为物质的类气相垂向迁移。这一机制可以说明按传统机制难以解释的现象,对相应化探方法的研制、改善和应用有理论和实践上的指导意义。     

Numerical studies on the structure of the cosmic ray electron halo in starburst galaxies

The structure of the cosmic ray electron halo of a starburst galaxy depends strongly on the nature of galactic wind and the configuration of the magnetic field. We have investigated these dependencies by solving numerically the propagation of electrons originating in starburst galaxies, most likely in supernova remnants. The calculations are made for several models for the galactic winds and for the configuration of the magnetic fields for comparison with observations. Our simulation of a quasi-radio halo reproduces both the extended structure of ∼9 kpc and the subtle hollow structure near the polar region of the radio halo that are observed in the starburst galaxy NGC 253. These findings suggest the existence of strong galactic wind in NGC 253.      

山东金青顶金矿床控矿构造特征及深部预测

金青顶金矿床位于山东牟平-乳山金矿带将军石-曲河庄断裂的南端,矿床围岩为昆嵛山花岗岩,属含金石英脉型金矿。本文通过矿床地质特征、围岩蚀变以及控矿构造特征等方面的研究,认为与成矿有关的构造活动至少划分为4期,基本控制着矿体的定位与分布。深部地球化学原生晕研究表明,矿体在垂向上具有明显的地球化学分带性,且在已知矿体下方出现近矿晕、前缘晕及尾晕特征指示元素构造叠加晕强度升高趋势。结合矿体在断裂中分布的规律以及原生晕特点,对金青顶矿床深部第二富集段进行了预测,推断在-1100m下有第二金富集段存在,且具有很大的经济价值。     

新疆东天山红石金矿床原生晕特征与矿体叠加模型

红石金矿床是新疆东天山康古尔塔格金矿带中的代表性矿床之一。通过对其地表、已开采中段及部分钻孔的岩石系统采样分析和计算统计,研究了各指示元素在不同位置的组合特征。结果表明:指示元素中Au、Ag密切相关,其他元素组合复杂多变,反映了成矿成晕的多期性、多阶段特点。结合实际勘查资料,采用多种计算方法,建立了矿床原生晕轴向分带模式,即矿床轴向分带(自上而下)为Bi-Mo-Hg-Zn-Pb-Ag-As-Cu-Sb-Au。利用不同中段的7个分带评价值指标确定了矿体的叠加模型。     

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

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。     

山东三甲金矿床控矿构造特征及深部预测

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。     

Transfers between libration-point orbits in the elliptic restricted problem

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.