铅同位素地球化学示踪进展   总被引：1，自引：0，他引：1  

何琼  李向阳 《地质找矿论丛》1998,13(3):79-82

本文论述了铅同位素示在地学中的最新应用和发展。由于它在示踪物质来源,圈定找矿靶区,判别构造环境等方面的优势,是当前最重要的地球化学示踪手段之一和同位素地球化学研究的热点。  相似文献   

西秦岭三叠系一个浊积岩序列金的地球化学特征     

赖旭砻  谢树成  杜远生  章传玲  朱敬宾 《地球学报》1998,19(2):210-214

本文在详细分析沉积韵律、沉积构造、成分及粒度的基础上,论证了四川省若尔盖县阿西乡牙相一带上三叠统卡车组一套浊积岩沉积。通过对牙相浊积岩序列的２３个采自各浊积旋回各层段的系列样品的金分析,发现这一浊积岩序列具有：以泥质粉砂岩、泥质岩为主的鲍玛序列的Ｄ—Ｅ段与其上旋回的以含砾砂岩、粗砂岩为特征的Ａ段含金量呈线性关系,表明这两段之间元Ａｕ元素发生了循环,进一步揭示了浊积岩具有金的可迁移性这一矿源层的重要特征。另外,砂质单元金含量比细粒的粉砂岩和泥岩要高,从浊积岩序列的底部旋回至上部回金的含量降低并由不稳定到稳定  相似文献   

模式识别技术在油气化探中的应用   总被引：3，自引：0，他引：3  

任春  夏响华  邓平 《安徽地质》1998,(2)

本文将模式识别技术应用于油气化探,给出了方法的逻辑框图,剖析了一个典型实例,其结果说明运用模式识别方法获得地球化学场的基本结构及其变异特征,反映了地球化学场的变化规律。结合地质条件提炼出的成藏模式能为预测油气藏指明方向。  相似文献   

江苏丰、沛、铜地区高氟地下水成因探讨   总被引：4，自引：0，他引：4  

张景荣  朱法华  陈汝秀  缪晓图  姚素平 《高校地质学报》1998,(2)

通过该区太古界一新生界氟的地层地球化学剖面及岩浆岩和土壤中氟的丰度的研究,论证了该区为一高氟的地球化学区。根据重矿物对比研究和地貌分析,阐明了泰沂隆起区太古界和元古界的高氟古老岩系为该区土壤沉积物源,黄河多次泛滥堆积（粘土矿物对氟的吸附）对土壤氟起了叠加富集的作用。研究揭示该区土壤水溶氟较高,经降水淋滤和浸取作用氟转入地下水,并在凹陷区或河间洼地中聚集,水体停泄、蒸发浓缩形成高氟地下水区。  相似文献   

云贵高原湖泊沉积物碳酸盐和有机质的同位素组成及环境信息记录   总被引：1，自引：0，他引：1  

肖保华 《矿物岩石地球化学通报》1998,(1)

云贵高原湖泊沉积物碳酸盐和有机质的同位素组成及环境信息记录＠肖保华￥中国科学院地球化学研究所高原湖泊,碳酸盐,有机质,碳同位素,地球化学记录,环境气候信息云贵高原湖泊沉积物碳酸盐和有机质的同位素组成及环境信息记录肖保华（中国科学院地球化学研究所,贵阳５５０...  相似文献   

Preparation of Two New GSJ Geochemical Reference Materials: Basalt JB-1b and Coal Fly Ash JCFA-1   总被引：1，自引：0，他引：1  

Shigeru Terashima  Masahiro Taniguchi  Masumi Mikoshiba  Noboru Imai 《Geostandards and Geoanalytical Research》1998,22(1):113-117

  相似文献   

宝石颜色的命名与判定方法评述     

张庆麟 《上海国土资源》1998,(3):24-29

较系统评述了现有的各种命名与判定宝石颜色的方法,如命名法中的二名法、类似法、色度法和三要素法;判定法中的目测法、仪器测量法和对比法。指出它们均存在有不同程度的缺点,但相对比较起来,用色谱图系的对比法是目前较好的方法。  相似文献   

A new population of brown dwarfs     

M. R. S. Hawkins  C. Ducourant  H. R. A. Jones  & M. Rapaport 《Monthly notices of the Royal Astronomical Society》1998,294(3):505-512

In this paper we report the first results from a survey for low-mass stars and brown dwarfs, based on a photographic stack of around 100 Schmidt plates. This survey extends photographic searches by about 2 mag, and covers an area of 25 deg². Some 30 faint objects with large R − I colours were selected for further study, and were found to have very strong molecular absorption in their spectra, but only moderately red infrared colours. Five of these stars were selected for a parallax programme; three of these were found to be at a distance of around 45 pc, implying a very low luminosity. On the basis of their luminosity alone it is clear that these stars are field brown dwarfs, and we discuss their likely evolutionary status in the context of current models of low-mass stellar evolution.  相似文献   

The light curves of soft X-ray transients     

King  & Ritter 《Monthly notices of the Royal Astronomical Society》1998,293(1):L42-L48

We show that the light curves of soft X-ray transients (SXTs) follow naturally from the disc instability picture, adapted to take account of irradiation by the central X-ray source during the outburst. Irradiation prevents the disc from returning to the cool state until central accretion is greatly reduced. This happens only after most of the disc mass has been accreted by the central object, on a viscous time-scale, accounting naturally for the exponential decay of the outburst on a far longer time-scale (τ20–40 d) than seen in dwarf novae, without any need to manipulate the viscosity parameter α. The accretion of most of the disc mass in outburst explains the much longer recurrence time of SXTs compared with dwarf novae. This picture also suggests an explanation of the secondary maximum seen in SXT light curves about 50–75 d after the start of each outburst, since central irradiation triggers the thermal instability of the outer disc, adding to the central accretion rate one viscous time later. The X-ray outburst decay constant τ should on average increase with orbital period, but saturate at a roughly constant value ∼40 d for orbital periods longer than about a day. The bolometric light curve should show a linear rather than an exponential decay at late times (a few times τ). Outbursts of long-period systems should be entirely in the linear decay regime, as is observed in GRO J1744−28. UV and optical light curves should resemble the X-rays but have decay time-scales up to 2–4 times longer.  相似文献   

The dwarf galaxy population of the Coma cluster to M_R=−11: a detailed description     

Neil Trentham 《Monthly notices of the Royal Astronomical Society》1998,293(1):71-88

We present the luminosity function and measurements of the scalelengths, colours and radial distribution of dwarf galaxies in the Coma cluster down to R =24. Our survey area is 674 arcmin²; this is the deepest and most detailed survey covering such a large area.
Our measurements agree with those of most previous authors at bright and intermediate magnitudes. The new results are as follows.
(1) Galaxies in the Coma cluster have a luminosity function φ( L )∝ L ^α that is steep (α∼−1.7) for −15< M_R <−11, and is shallower brighter than this. The curvature in the luminosity function at M_R ∼−15 is statistically significant.
(2) The galaxies that contribute most strongly to the luminosity function at −14< M_R <−12 have colours and scalelengths that are consistent with those of local dwarf spheroidal galaxies placed at the distance of Coma.
(3) These galaxies with −14< M_R <−12 have a colour distribution that is very strongly peaked at B − R =1.3. This is suggestive of a substantial degree of homogeneity in their star formation histories and metallicities.
(4) These galaxies with −14< M_R <−12 also appear to be more confined to the cluster core ( r ∼200 kpc) than the brighter galaxies. Alternatively, this observation may be explained in part or whole by the presence of an anomalously high number of background galaxies behind the cluster core. Velocity measurements of these galaxies would distinguish between these two possibilities.  相似文献