藏北高原双湖地区中侏罗统海相油页岩生物标志化合物分布特征及其意义

重点报道了藏北双湖地区中侏罗统海相油页岩的生物标志化合物特征,首次在该层位油页岩中检出丰富的正烷烃、类异戊二烯烷烃、萜类化合物及甾类化合物。正烷烃图谱呈单峰形,nC₁₅、nC₁₆或nC₁₇为主峰碳,轻烃组份占有绝对优势,OEP值 0.93～ 1.0 1,无明显的奇偶碳数优势分布;Pr/Ph值为 0.77～ 1.5 9,在剖面序列中呈波动分布,显示弱植烷优势或姥鲛烷优势;藿烷以C₃₀ 占优势,萜烷相对丰度五环三萜烷 >三环萜烷 >四环萜烷;规则甾烷∑ (C₂₇+C₂₈) >∑C₂₉,∑C₂₇/∑C₂₉值为 0.79～ 1.2 0,在剖面序列中下部C₂₇甾烷略占优势,上部C₂₉甾烷略占优势,重排甾烷C₂₇/规则甾烷C₂₇值为 0.5 1～ 3.6 3,在剖面序列中具有显著的波动性,同时检出了少量孕甾烷和 4-甲基甾烷。有机质母质构成中,既有丰富的藻类等低等水生生物,可能还有一定比例陆生高等植物输入混合的特点。油页岩处于成熟阶段,整个油页岩剖面序列具有一致的热演化程度。剖面中部油页岩具有极高的原始生产力,氧化-还原条件也是控制油页岩TOC和沥青“A”含量在剖面垂向变化的重要因素.     

南和沟铜矿床地质特征及成矿地质条件分析

研究表明南和沟铜矿床受剥离断层和变质热液两重成矿作用控制，具有多因成矿特征。     

阿希金矿地质特征及成因初探

阿希金矿产于下石炭统大哈拉军山组,第五岩性段构成的古火山机构西南缘。矿体产出形态及空间分布,严格受近南北向弧形张扭性断裂控制。主矿体呈厚大似板状体,以南北两个富集中心向NE50°倾角侧伏。矿石以石英脉型为主,其次为蚀变岩型。围岩为英安岩和角砾熔岩。属中一低温火山期后热液型金矿床。     

湖南内生金属矿床成矿分带及其与区域地质背景的关系

湖南主要内生金属矿床的成矿作用，存在明显的分带性，自南东向北西，成矿元素逐渐减少，成矿温度逐渐降低，由与酸性，中酸性侵入岩有关的矿床为主，渐变为与沉积期后成矿作用有关的层控矿床为主，赋矿层位亦有逐渐降低之规律，据此，可将湖南内生金属矿床划分为４个矿带。燕山期构造岩浆活动，是上述成矿分带的主要原因。     

祁连山蛇绿岩型超镁铁岩铬铁矿床成矿的主要特征

祁连山造山带目前已发现不同规模的超镁铁岩体（群）1000余个,产有铬铁矿床（点）和矿化点80余处,这些岩体及其矿产主要产在北祁连优地斜增生地体边部的海沟带中,少数产在祁连中间地块的边部。岩体成因类型为蛇绿岩组合中的超镁铁质单元,铬铁矿的富集部位是地幔橄榄岩和堆积杂岩带底部的纯橄榄岩。岩石多为铝过饱和系列,岩体的平均化学成分接近于斜辉橄榄岩;Cr₂0₃的平均含量大于0.40％,Al₂0₃的平均含量近于或者大于1％。铬尖晶石的化学参数特征反映出低铁富镁的介质对形成富铬尖晶石是有利的。富铬岩体中Cr、Co、Ti、V的含量较高。     

钨的地球化学性质与华南地区钨矿成因

在地球演化早期的强还原条件下,钨表现为中等亲铁元素,因此地球中 90%的钨进入地核。在地幔和地壳的演化过程中,钨是极度不相容亲石元素,从而导致钨元素在地壳中的丰度约是地幔丰度的250倍。钨在岩浆熔体中主要以钨酸的形式迁移,在成矿热液中主要以氟、硼化合物或其络合物的形式运移。钨的矿化需要其在部分熔融、岩浆演化和晚期热液等各阶段逐渐富集。中国是世界上钨矿产资源最丰富的国家,约占世界总储量的60%以上,其中绝大多数矿床产在华南地区,与华南大规模的中生代岩浆活动具有密切的时空联系。微量元素特征(高Rb/Sr和K/Rb比值,低Nb/Ta和Zr/Hf比值)显示它们往往经历了强烈的岩浆分异,这可能与这些花岗岩通常具有高挥发分含量(如F)有关。岩浆中高的F含量对钨的富集和矿化十分重要,它可以降低熔体固相线、粘度和密度,有利于提高岩浆的结晶分异程度,因而使得高度不相容的钨元素在岩浆演化过程和后期热液阶段的富集与矿化。富挥发分岩浆的形成可能与俯冲板块后撤,软流圈物质上涌导致的多硅白云母等富F矿物的高温分解有关。研究表明,华南南岭地区侏罗纪的钨矿化花岗岩主要形成于太平洋板块的俯冲后撤,而华南南部晚白垩世钨成矿作用与新特提斯洋的俯冲后撤有关。     

DIAGNOSIS ON LOW FREQUENCY COMPONENT OF ENSO VARIABILITY—PART Ⅱ:ORIGIN OF THE COMPONENT

Diagnosis is undertaken on the origin for the low-frequency component (LFC) of ENSOvariability in the context of 1979—1990 OLR and u-wind datasets.Evidence suggests that ① apower spectrum-yielded maximum,significant statistically,is derived from the OLR monthlyanomalies in a 3—5-year period range over the tropical central/western Pacific;②compositeanalysis of the signals of the monthly anomaly low frequency component (period>3 years)confirms further the dynamic features of the component as documented in Part Ⅰ:③serving asforcing on ENSO,the related monsoon region represents the source area of the component;④theone-point correlation maps of unfiltered OLR monthly anomalies with zonal wind on a lagged,asimultaneous and a leading basis show clearly the close relation between the u wind-associatedeastward travelling low-frequency wave and the low-frequency oscillation of low-latitude central/western Pacific large-scale convection and the east-moving mode is likely to be excited by theoscillation at a 3—5-year period range.It follows that the large-scale convection oscillation showsup as the origin of the eastward waves,i.e.,ENSO LFC.     

Characteristics of melt inclusions in skarn minerals from Fe,Cu(Au) and Au(Cu) ore deposits in the region from Daye to Jiujiang

The skarns and skarn deposits are widely distributed at home and abroad. The skarn deposits include many kinds of ores and higher ore grade. Some of them are broad in scale. Scientists of ore deposits from different countries have paid and are paying grea…     

Planetary Embryos Never Formed in the Kuiper Belt

We study the orbital evolutions of various systems of planetary embryos in the transneptunian region, undergoing mutual scattering and perturbations from the giant planets. We show that about 15-20% of the original embryos should survive in the transneptunian region at the current epoch. The orbital dispersion of the surviving embryos depends on their individual mass, so that only lunar mass embryos could survive with semimajor axis smaller than 50 AU. In all cases, we show by a Monte Carlo model that at least one of the surviving embryos should have already been discovered by one of the most effective Kuiper-belt surveys. This implies that planetary embryos did not form in the transneptunian region (or have been removed by some external and unknown mechanism). Therefore, we conclude that the Kuiper belt was not excited by resident planetary embryos, unlike the asteroid belt. We also compute with the Monte Carlo model that a significant number (order 10) of Pluto-size bodies could exist only on very eccentric and long-periodic orbits, typical of the scattered disk, while the existence of about 30 bodies brighter than absolute magnitude 4 in the classical belt is compatible with the discovery of Varuna by the Spacewatch survey.