黄土高原西部地区黄土地层有机质主要来源分析*

黄土有机质的主要来源是决定其稳定碳同位素(δ13Corg.)能否应用于重建过去C3/C4相对丰度变化及相应的古气候变化的关键基础科学问题.如若黄土地层当中的有机质主要由粉尘携带而来,而非当地植被,显然其δ13Corg.不是一个局地植被过去C3/C4相对丰度变化及古气候变化的良好指示器.本文对黄土高原西部地区(六盘山以西)新获得和已发表的相关数据进行综合分析,尝试对该地区黄土有机质的主要来源进行定量的分析.结果表明,总体而言,该地区黄土地层有机质主要来源于当地植被,由粉尘携带而来的有机质贡献量不超过8％,所造成的有机碳同位素变化幅度不超过1.7‰.这些结果说明该地区的黄土地层有机质δ13Corg.是可以用来重建过去C3/C4植物相对丰度及相应的古气候变化的.为了更精确的重建,后续的工作应当更多考虑粉尘搬运过程当中的有机质输入以及粉尘沉积之后的微生物活动的可能潜在影响.     

Studies of community structure and seasonal dynamics of planktonic copepods in saline-alkaline ponds

Abstracts Species abundance and seasonal succession of copepods in saline-alkaline ponds were studied in Zhaodian Fish Farm, Gaoqing County, Shandong Province, from 5 April 1997 to 1 September 1998. The results indicated that in the conditions of salinity ranging from 1.36 to 20 g/L, total alkalinity changing from 2.4 to 7.2 mmol/L and pH 8-9, zooplankton in saline-alkaline ponds was composed of freshwater salt-tolerated species or halophile species, some of which are halobiont species and usually occurs in freshwater. In our study, copepods were predominant in many fish-culture ponds and all control ponds without fishes in spring, late autumn and early winter. Dominant species of copepods were Sinocalanus tenellus, Cyclops vicinus, Thermocyclops taihokuensis. The biomass of copepods in the control ponds without fishes was higher than that of the fish-culture ponds.     

Automatic Normalization and Equivalent-Width Measurement of High-Resolution Stellar Spectra

It is well known that normalization, radial velocity correction and equivalent-width measurement of high-resolution stellar spectra are time-consuming work. In order to improve the efficiency we present an automatic method for these routines. The continuum is determined by fitting the 'high points' in the spectrum. After continuum normalization, the program automatically searches for the position of the Ha line and obtains a rough radial velocity, then computes an accurate radial velocity by cross-correlation between the given spectrum and the solar spectrum. In this method, the equivalent-width is automatically measured using Gaussian fitting. A comparison between our results and those from traditional analysis shows that the typical error for equivalent width is around 3.8% in our method. Developing such automatic routines does not mean to replace the interactive reduction method: it is just for a quick extraction of information from the spectra, especially those obtained in large sky surveys.     

A Statistical Model for Predicting the Average Abundance Patterns of Heavier Elements in Metal-Poor Stars

We have collected nearly all the available observed data of the elements from Ba to Dy in halo and disk stars in the metallicity range -4.0 <[Fe/H]< 0.5. Based on the observed data of Ba and Eu, we evaluated the least-squares regressions of [Ba/Fe] on [Fe/H], and [Eu/H] on [Ba/H]. Assuming that the heavy elements (heavier than Ba) are produced by a combination of the main components of s- and r-processes in metal-poor stars, and choosing Ba and Eu as respective representative elements of the main s- and the main r-processes, a statistical model for predicting the Galactic chemical evolution of the heavy elements is presented. With this model, we calculate the mean abundance trends of the heavy elements La, Ce, Pr, Nd, Sm, and Dy with the metallicity. We compare our results with the observed data at various metallicities, showing that the predicted trends are in good agreement with the observed trends, at least for the metallicity range [Fe/H]> -2.5. Finally, we discuss our results and deduce some importa     

A Differential Abundance Analysis of HD219175 A and B

The abundances of the wide binary pair HD 219175 A and B are determined and compared using a line-by-line differential analysis. No evidence for difference has been found in the abundances of Fe, O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Cr, Mn, Ni, Cu and Ba. Our results support a physical relation between the two components of HD 219175.     

低部主序恒星锂和铍的衰减

根据化学非均匀恒星的非局部对流理论,计算了质量为0．7-1．15M(?)恒星主序演化模型锂和铍的衰减,并将理论和不同年龄疏散星团锂丰度的观测进行了比较．结果表明,贯穿对流混合能重现温度低于6400 K的晚型主序星锂丰度观测的一般性质．贯穿对流混合可能是晚型矮星锂衰减的一种重要机制．     

桂东寒武系水口群岩石地球化学特征及其与金矿化关系

桂东寒武系水口群分布范围很大,是一套巨厚的地槽型细碎屑岩建造,据硅质条带及岩性变化特征可划分清溪和边溪两个亚群及五个岩性段。本文重点论述了区域及矿区内地层及各类原岩中Au、Ag等指示元素的地球化学特征:水口群各类原岩中Fe、Mg含量比世界同类岩石高;水口群各岩性段Au的丰度值与地壳丰度值相比差别不大,以水口群顶部的丰度值相对较高,各类原岩中以炭质砂页岩最高;矿区内地层及各类原岩金的丰度值相应要高得多;而水口群及各类原岩中Ag、As、Sb.Hg等指示元素和Pb、Zn、Mo等微量元素含量高,且矿区比区域内同种元素含量还高。据此探讨了水口群与金矿化的关系,初步认为可把水口群视为该区金的衍生矿源层,为该区各类金矿的成矿作用提供了一定的物质来源。     

巨早型星系的近红外谱合成

在8000至8670的波长范围内,利用一个由144颗恒星光谱组成的光谱厍,我们对57个巨椭圆和S0星系(M_B<-21)的光谱和它们的平均光谱进行了光谱合成.这个光谐库包括了光谱型为G,K和M的巨星和矮星,它具有的金属丰度[Fe/H]覆盖了-0.1到-0.5的范围,表面重力log g为1.0至5.0.光谱合成的结果表明:巨椭圆和S0星系的金属丰度约为太阳的一倍半;有效表面重力分布在3.2—4.1的范围内;矮星在8400附近光的贡献可与巨星相比较.     

我国某地沥青铀矿中U^235相对富集的初步研究

The discovery of the gamma spectrum abnomal is reported for the uranium ore sample No. 15, In comparison with a parallel investigation on a reference natural uranium saraple the relative abundance of U^235 is obtained and the U^233 content of sample No. 15 turns out to be 5 percent higher than that of the reference natural sample, Discussion is given to the mechanism by which U^235 is enriched in the ore.     

吉林陨石锂同位素相对丰度的初步探讨

陨石、地球、太阳、恒星和宇宙线中锂同位素组成的对比研究,不仅可为阐明太阳系锂的起源提供一定依据,而且对于了解太阳系历史中的天然核作用过程和天体化学过程也具有一定价值。 各类陨石的锂同位素组成,已用经典质谱法、二次离子质谱法和热离子质谱法进行了研究。经典质谱法与热离子质谱法的结果表明,石陨石的锂同位素组成在实验