DCS－偶氮胂光度法测定钛酸锶烧结物中游离的氧化锶

ＤＣＳ－偶氮胂光度法测定钛酸锶烧结物中游离的氧化锶胡浩，周宏实江苏海安磷肥厂２２６６００ＤＣＳ－偶氮肿［２－（２－胂酸基苯偶氮）－７－（２，６－二氯－４－磺酸基苯偶氮）－１，８－二羟基－３，６－二磺酸萘］属双偶氮变色酸类显色剂，主要用于稀土元素的高灵...     

510—1铀矿床构造、地球化学特征及其成因探讨

本文根据510—1铀矿床形成的构造条件和地球化学特征,认为该富铀矿床的成因是地洼阶段壳幔混合型深源热液上升侵位,与贡巴—益哇逆冲推覆构造上盘中、下志留统羊肠沟组硅灰岩含水含矿层屏蔽构造相结合的结果。并指出古今统一的四维空间屏蔽构造是找矿的方向。     

甘孜嘎拉金矿金的赋存状态初步研究

甘孜嘎拉金矿位于川西甘孜-理塘断裂带北段,该矿床具一定规模。笔者对该矿床自然金的产出状态,以及超显微金在黄铁矿、毒砂、辉锑矿主要载金矿物和各类矿石中的分布特征初步研究后,认为该矿床的金只有少量呈显微自然金形式赋存,大部分都是以超显微金的自然元素金混入各类载金体中,金的赋存状态指示该区金物源广,具良好的找金前景。     

新疆北准噶尔泥盆纪洋内弧及博宁岩

博宁岩(Boninite),以其低钛、低MREE、富镁区别于岛弧拉斑玄武岩和钙碱系列玄武岩,为洋内弧特征产物。新疆北准噶尔中泥盆统北塔山组火山岩基本为博宁岩,系拉张阶段深海喷发物。汇聚型过渡壳阶段生成的辉长岩-钠质花岗岩建造也反映其洋内弧环境。     

中国矿产资源国情调查评价历史回顾及对推动国民经济发展的作用

矿产资源储量家底是一个国家的基础根基，矿产资源及矿产品(含重要工业产品)是一个国家实施工业化及促进现代化建设的物质基础，是一个国家综合国力的体现。要以科学的精神，评价矿产资源。有多少家底，办多大事情，一步一个脚印地支撑国家经济建设。本文在回顾1949年新中国建立以来70余年地质矿产资源勘查、矿产资源开发利用及工业化取得了举世瞩目的成就的基础上，对自1952年以来中国矿产资源国情调查与评价历史进行系统评价，经综合集成研究，总结提出中国矿产资源国情调查与评价的发展演变规律，所得出的研究结论与认识对于推进我国矿产资源国情调查与评价工作具有一定的现实意义。研究认为：矿产资源在我国工业化与经济社会发展中发挥着重要作用，基于中国矿产资源储量管理体制及职能的变化，以矿产资源储量管理为核心，将中国矿产资源国情调查与评价的发展演变阶段划分为5个时期：启动期(1952～1965年)、规范期(1966～1993年)、改革期(1994～2006年)、发展期(2007～2017年)与深化期(2018年-),阐述了各时期的特点与发展演变规律，以及查明资源储量和矿产品的变化规律。在每个时期，我国均依靠国家力量，组织...     

赤峰哈拉道口早石炭世花岗闪长岩年代学、地球化学及其地质意义

以内蒙古赤峰哈拉道口地区花岗闪长岩为研究对象，利用锆石LA-ICP-MS U-Pb测年技术进行年代学研究，测试结果为352.4~355.9Ma，显示其形成时代为早石炭世早期，为华北板块北缘早石炭世岩浆岩活动研究提供了新的资料.地球化学特征显示，花岗闪长岩总体上贫Si、Al，总碱量偏高，Eu仅有轻微的亏损，属铝未饱和、高钾钙碱性系列岩石.同时花岗闪长岩具有较高Sr含量，较低的MgO、Y、Yb含量，富集LREEs，亏损HREEs和HFSEs，Sr/Y比值介于34.62~48.43之间，（La/Yb）_N比值为15.31~17.14，显示"C型埃达克岩"特征.较高的K₂O、Cr、Ni含量和较低的Mg^#值说明其不可能是由拆沉下地壳物质的熔融形成，而是形成于增厚下地壳镁铁质岩的部分熔融.微量元素特征显示花岗闪长岩形成于活动大陆边缘弧环境.所以，早石炭世早期，本区处于古亚洲洋板块向南俯冲的大地构造背景.     

华北地台西南缘矿床的亲缘性及其找矿意义

华北地台西南缘山西中条山和河南小秦岭两地区在晚太古宙—元古宙曾是豫—晋—陕三向裂陷槽的主要组成部分,均发育具大陆裂谷环境双模式的拉斑玄武岩、碱性玄武岩及部分钙碱性火山岩建造,构建了两个地区的原始地壳和初始矿源层。稀土元素配分模式和常量元素及微量元素特征表明二者均具相同的富集型和亏损型,表现出成矿物质来源的同源性及成矿演变的继承性。在层位和岩性控矿、同位素地球化学特征、成矿溶液组成及成矿物化条件等方面两地非常近似,并表现出成矿的多元、多源、多期、多阶段的明显层控矿床的特征,佐证了中条山和小秦岭两个地区矿源层和矿床亲缘性的存在,由此认为在"富铜"的中条山地区应注意找金,在"富金"的小秦岭地区应注意找铜。通过华北地台西南缘矿床亲缘性的研究,可以有助于华北地台西南缘地区的新一轮找矿工作的开展。     

A New Catalogue of Fine Structures Superimposed on Solar Microwave Bursts

The 2.6-3.8 GHz, 4.5-7.5 GHz, 5.2-7.6 GHz and 0.7-1.5 GHz component spectrometers of Solar Broadband Radio Spectrometer (SBRS) started routine observations, respectively, in late August 1996, August 1999, August 1999, and June 2000. They just managed to catch the coming 23rd solar active maximum. Consequently, a large amount of microwave burst data with high temporal and high spectral resolution and high sensitivity were obtained. A variety of fine structures (FS) superimposed on microwave bursts have been found. Some of them are known, such as microwave type Ⅲ bursts, microwave spike emission, but these were observed with more detail; some are new. Reported for the first time here are microwave type U bursts with similar spectral morphology to those in decimetric and metric wavelengths, and with outstanding characteristics such as very short durations (tens to hundreds ms), narrow bandwidths, higher frequency drift rates and higher degrees of polarization. Type N and type M bursts were also observed. Detailed zebra pattern and fiber bursts at the high frequency were found. Drifting pulsation structure (DPS) phenomena closely associated with CME are considered to manifest the initial phase of the CME, and quasi-periodic pulsation with periods of tens ms have been recorded. Microwave “patches”, unlike those reported previously, were observed with very short durations (about 300ms), very high flux densities (up to 1000 sfu), very high polarization (about 100% RCP), extremely narrow bandwidths (about 5%), and very high spectral indexes. These cannot be interpreted with the gyrosynchrotron process. A superfine structure in the form of microwave FS (ZPS,type U), consisting of microwave millisecond spike emission (MMS), was also found.     

Rotational Brightness Modulation and Starspots on the RS CVn-type Stars IN Com, IL Com, UX Ari, and V711 Tau

UBVRI photometric observations and models of spotting are presented for four noneclipsing RS CVn systems: IN Com (G5III/IV), IL Com (F8V+F8V), UX Ari (K01V+G5V), and V711 Tau (K1IV+G5V). A low amplitude variability caused by cold (T=1700K)spots which can occupy up to 19% of the star's surface is confirmed for the little-studied star IL Com. Long-term light curves are constructed and the stellar magnitudes and color indices of the unspotted photospheres are estimated for IN com, UX Ari, and V711 Tau. It is shown that UX Ari becomes bluer with decreasing brightness, so its variability cannot be fully explained in terms of cold spots. Models of spotting on In Com and V711 Tau are constructed from the full set of available photometric observations. The spots on both of these variables lie at middle latitudes and occupy up to 22% (In Com) and 33% (V711 Tau) of the stars' surfaces. Both stars manifest a tendency for the width of the spots to decrease as their area increases. This is a crude analog of the Maunder butterflies. These stars experience cyclical spot activity and have a differential rotation of the type found on the sun.     

“Small Equipment Strategy” in the Development of Astronomy

Astronomy is an observational science. This paper points out that in the development of astronomy, the means of observation at every stage has as its main body the large equipment of the time, but equally important is the simultaneous development of small equipment as strategic complement. A number of historical examples are cited. The recently suggested“Special Radio Telescope Dedicated to Pulsar Research” originates in the small equipment strategy, and a brief introduction to this instrument is included here.