新疆包古图金矿四矿区L7号脉中的特殊矿物组合及其成矿意义

包古图金矿四矿区L7号脉由浅部的自然砷-石英脉型矿石和深部的辉锑矿-石英脉型矿石组成。矿脉中含罕见的As、Sb矿物,如paakkonenite（Sb₂AsS₂）、自然砷、自然锑、方锑金矿、硫锑金银矿（Au₃Ag₄Sb₁₀S₁₂）等。热液过程划分为5个阶段：黄铁矿-毒砂阶段（Ⅰ）,围岩中形成大量的毒砂和黄铁矿并伴随较强硅化;粗粒石英阶段（Ⅱ）,形成沿围岩壁或围岩角砾的梳状石英;Au-As-Sb矿化阶段（Ⅲ）,形成辉锑矿-自然锑-自然砷-paakkonenite-银金矿-自然金-方锑金矿-硫锑金银矿-辉锑银矿-银锌黝铜矿-斜方砷铁矿-硫铜锑矿-石英;晚期Sb矿化阶段（Ⅳ）,形成与粒状方解石共生的辉锑矿、自然锑和paakkonenite;方解石阶段（Ⅴ）,形成穿切矿体和围岩的方解石（-石英）细脉。辉锑矿和斜方砷铁矿交代毒砂,自然金、方锑金矿、paakkonenite和自然砷交代辉锑矿。辉锑矿的结晶主要受温度和还原S含量的控制,自然砷、自然锑的结晶主要受氧逸度和温度控制。As、Sb分别以自然砷、辉锑矿和自然锑形式存在,同时消耗大量H₂S,流体进入张性空间后也释放H₂S,导致硫逸度急剧降低,含Au络合物失稳而成矿。     

马里亚纳海沟挑战者深渊初期多金属氧化物的 矿物学、地球化学特征及其成因环境研究

对大洋27航次在西太平洋马里亚纳海沟挑战者深渊获取的3个多金属氧化物样品进行了X射线矿物衍射分析、穆斯堡尔谱分析及地球化学元素分析,研究其矿物、地球化学特征差异。结果表明,所取样品处于多金属氧化物发育的初始阶段,具有独特的矿物地球化学特征:(1)相较于太平洋CC区及中太平洋海盆获取的多金属结核样品,本研究样品的矿物组成中含有异常高的石英、斜长石以及黏土矿物,而水羟锰矿和钙锰矿含量较低。(2)样品中铁相矿物主要为正方针铁矿(91.6%),另含少量纤铁矿(8.4%),推测是纤铁矿向更加稳定的正方针铁矿衍变的结果。(3)由于样品中深海黏土组分以及氧化物核心物质的混入,加上吸附金属氧化物时间较短,导致SiO₂和Al₂O₃含量均高于正常结核,而Fe、Mn、Cu、Co、Ni等其余金属元素含量较低。(4)由于形成时间较短,样品中稀土元素含量相对较低,ΣREE仅约为0.4×10^-3(一般太平洋CC区及中太平洋结核中稀土含量均大于1.0×10^-3);加之海水氧化还原作用的降低以及研究区海底热液活动的影响,Ce元素未表现出多金属结核中常见的正异常。     

Application of advanced system identification technique to extract roll damping from model tests in order to accurately predict roll motions

In this paper our previously developed advanced system identification technique [1] has been applied to extract the frequency dependent roll damping from a series of model tests run in irregular (random) waves. It is shown that this methodology accurately models the roll damping which can then be used to produce accurate predictions of the ships roll motion. These roll motion predictions are not only more accurate than the potential flow predictions but more accurate than potential flow models corrected using either empirical prediction methods [2] and even those corrected using roll damping obtained from free decay sallying experiments. This methodology has the potential to significantly improve roll motion prediction during full scale at sea trails of vessels in order to dramatically improve safety of critical operations such as helicopter landing or ship to ship cargo transfer.     

电阻率-孔隙度、电阻率-含油（气）饱和度关系的一般形式及其最佳逼近函数类型的确定（Ⅰ）

本文导出了电阻率-孔隙度、电阻率-含油（气）饱和度关系的一般形式--两个对称的表达式,并给予了实验证明。同时,本文指出,Archie公式、Winsauer公式和双水公式都是一般形式在一定条件下的特例。在一般情况下,本文给出了14个能够逼近这两个表达式的函数类型,通过岩芯数据进行选优,可以得到适合不同地区或地层的最优方程。根据本文理论建立的解释方法和研制的软件已经在油田生产中推广应用并取得了良好效果。 由于涉及内容较多,全文分两部分撰写。以下是本文的第（Ⅰ）部分,即一般形式的导出及实验验证;而最佳函数类型的确定及其在生产中的应用将作为本文的第（Ⅱ）部分发表。     

Contrasting mineralogical and processing potential of two mineralization types in the platinum group element and Ni-bearing Kapalagulu Intrusion,western Tanzania

The Kapalagulu layered ultramafic and mafic intrusion is emplaced between the Paleoproterozoic Ubendian basement and overlying Neoproterozoic Itiaso Group metasedimentary rocks, located near the western shore of Lake Tanganyika. High-grade platinum group element (PGE) mineralization (1–6 g/t Pt + Pd + Au) is associated with chromitite and sulfide-bearing harzburgite within the southeastern extension of the intrusion, known as the Lubalisi Zone, which is covered by a layer of nickel-rich (0.2–2%Ni) laterite regolith that contains linear areas of PGE mineralization.In the Lubalisi Zone, the mineralization may be divided into several significant geometallurgical domains: (a) high-grade PGE mineralization (1–6 g/t Pt + Pd + Au) associated with stratiform PGE reefs and chromitite seams within a harzburgite unit; (b) high-grade PGE mineralization (up to 12 g/t Pt + Pd + Au) associated with small bodies and veins of nickel massive sulfide within harzburgite below PGE-bearing reefs and chromitite seams; (c) low-grade PGE mineralization (0.1–0.5 g/t Pt + Pd + Au) associated with a sulfide-mineralized harzburgite unit above the PGE-bearing reefs; (d) laterite style residual PGE mineralization (0.2–4 g/t Pt + Pd + Au) associated with chromite concentrations in the saprolite and overlying red clay horizons of the laterite regolith; and (e) supergene Ni associated with the saprock and overlying saprolite clay.Mineralogical study of three samples from the PGE reef consisting of high grade PGE chromitite and harzburgite indicate that this mineralization will give a good metallurgical response to conventional grinding and floatation due to the relatively coarse-grained nature of the PGM (P80 from ∼37 to 52 µm), association with base metal sulfides, and unaltered gangue minerals (Wilhelmij and Cabri, 2016). In contrast, mineralogical and metallurgical study of the Ni and PGE mineralized laterite indicate that it cannot be processed using conventional mineral processing techniques but that a hydrometallurgical route should be used to recover the base and precious metals. Because any process is very much deposit-controlled, significant metallurgical and geometallurgical testing of mineralized samples, as well as pilot plant testing, will be required to arrive at feasibility studies.     

Star formation in the Cepheus Flare region – II. A-type stars associated with IRAS sources

In order to reveal the star-forming history of the molecular cloud complex we studied the intermediate mass stellar population in the Cepheus Flare region. (Paper I dealt with the distance and the young stellar object candidates of the region.) Correlating the IRAS Point Source Catalogue and Faint Source Catalogue positions with those of 1214 B8–A8 and 1760 F0–F5 type stars brighter than     and classified during an objective prism survey, we identified 19 stars showing far-infrared excess emission in the Cepheus Flare region. In addition to the 16 stars whose counterparts are given in the IRAS catalogues, we found three more stars with infrared excess not recognized before. In order to identify the young medium-mass stars associated with the Cepheus Flare molecular clouds we observed the optical spectra of the IR-excess stars, and using published optical photometry and the IRAS data we examined their spectral energy distributions (SEDs) and IRAS two-colour diagram. The observations resulted in the discovery of a new Herbig Ae/Be star, BD +68°1118, coinciding with IRAS 21169+6842. More evolved HAe/Be stars may be SAO 19953, BD +67°1314 and BD +69°1231, whose H α lines showed weak emission components. Possible β Pictoris- or Vega-type stars may be HD 203854, HD 212826 and HD 216486, whereas the far-infrared fluxes at the positions of BD +72°1018, HD 210806 and HD 217903 can be attributed to the heating of the interstellar environment. We used distances and radial velocities of the stars derived from the spectroscopy and published optical photometry as indicators of their relations to the clouds. Information on the environment of the observed stars deduced from the diffuse interstellar band at λ 6613 is briefly discussed.     

BVRI photometry of possible standard stars in NGC 188

CCD photometry of possible standard stars, in Cousins B, V, R and I, in a field in the region of NGC 188 is presented.     

女山幔源包体及其寄主岩中微量元素和过渡金属元素的研究

对女山碧玄岩、超镁铁岩包体和高压巨晶中微量元素及过渡金属元素进行探讨。研究表明,碧玄岩中ＬＲＥＥ较之ＨＲＥＥ更为富集,其分配型式属ＬＲＥＥ富集型;包体中ＬＲＥＥ较ＨＲＥＥ略显富集之势,分配型式属平坦型,这与地幔具有平缓的ＲＥＥ模式相符,其中略富ＬＲＥＥ与碧玄岩对应。碧玄岩、包体和高压巨晶中过渡金属元素具有不同的分配型式。但是不管在碧玄岩与包体之间,还是在巨晶与碧玄岩之间,某些过渡金属元素的含量都具有相关关系。可见,碧玄岩与包体具有成因联系,巨晶与碧玄岩也具有成因联系。