Properties and organic activation of ocean clay in the East Pacific

In order to make use of ocean clay reasonably and excavate its potential applications the properties of ocean clay in Chinese investigating area of the East Pacific have been tested with the chemical analysis, XRFS, ICP/MAS, granulometry and SSA, etc. The results show that the clay sediments of this area are rich in clay minerals, fine granularity, bigger SSA, bigger water absorbability and lower ion changing ability etc. To improve the adaptability of ocean clay and macromolecule materials, using the dry milling method with silane, aluminate, stearic acid coupling agents etc the properties of ocean clay are improved. The effect has been evaluated by testing the water absorbing of the modified ocean clay and their dispersing in paraffin liquid. The result is that KH550 is better than any other active reagents, and the best activation technics is that 1.5% (volume) of KH550 quantity, 20min of milling time. The DTA, XRD, SEM and IR analyses and SSA testing show that the organic activation can not change the mineral structure but can densify the structure of clay, and activation mechanism is chemical covered mainly and chemical combined secondly.     

DISSOLVED AND PARTICULATE ORGANIC CARBON IN YANTAI SISHILI BAY AQUICULTURE WATERS

Investigation of dissolved organic carbon (DOC) and particulate organic carbon (POC) at 12 stations in Yantal Sishili Bay in May, August, and November of 1997 and March and May of 1998 showed that DOC concentrations varied from 1.14 mg/L to 5.35 mg/L; that the average values at all staticrLs ineach entise varied from 1.52 mg/L to 2.12 mg/L; that POC concentrafions varied from 0.049 mg/L to 1.411mg/L; and averaged 0.159 mg/L to 0.631 mg/L in each cruise. Horizontal distribution of DOC was influ-enced by factors such as continental input, organism activity, temperature, aquieulture environment, etc. The higher POC concentration occurred along the coast. The vertical distribution of DOC and POC changed obviously in spring and summer, but not obviously in autumn and winter. DOC concentration was highest in summer and POC in spring; both were lowest in winter. The seasonal change of DOC was con-sistent with primary productivity seasonal variation, and that of POC was consistent with ehlorophyll-a sea-sanal variation. The seasonal change trend of the C/N ratio of dissolved organic matter was obvious, but the C/N ratio of particulate organic matter had no such trend.     

A 16 ka climate record deduced from δ^13C and C/N ratio in Qinghai Lake sediments, northeastern Tibetan Plateau

1 INTRODUCTION δ13C in organic matters from lacustrine sedi- ments varies with several factors including aquatic plants, vegetation type in the catchment, atmos- pheric CO2 concentration, climate (temperature and precipitation), and properties of water, …     

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.     

川东北地区上二叠统盘龙洞生物礁成岩作用研究

本文对宣汉盘龙洞上二叠统生物礁古油气藏成岩作用进行了详细的研究。其主要成岩作用类型有胶结作用、新生变形作用、白云岩化作用、去白云岩化作用以及压溶和溶解作用等。根据岩石中胶结物的胶结结构和矿物特征,初步判断该生物礁主要经历了海底成岩环境、大气淡水渗流潜流环境、海水与淡水混合带成岩环境和埋藏成岩环境。该区的白云岩主要是混合白云岩化形成的。值得强调的是,该区白云岩化作用和溶蚀作用对该生物礁岩石孔隙度的增加贡献很大,提供了良好的油气储集空间,这对恢复该生物礁储层孔隙发育历史,以及油气勘探和评价都有很重要的意义。     

Dust formation and inhomogeneous mass-loss from asymptotic giant branch stars

We examine the flow from asymptotic giant branch (AGB) stars when along a small solid angle the optical depth resulting from dust is very large. We consider two types of flows. In the first, small cool spots are formed on the surface of slowly rotating AGB stars. Large quantities of dust are expected to be formed above the surface of these cool spots. We propose that if the dust formation occurs during the last AGB phase when the mass-loss rate is high, the dust shields the region above it from the stellar radiation. This leads to both further dust formation in the shaded region and, owing to lower temperature and pressure, the convergence of the stream toward the shaded region, and the formation of a flow having a higher density than its surroundings. This density contrast can be as high as ∼4. A concentration of magnetic cool spots toward the equator will lead to a density contrast of up to a few between the equatorial and polar directions. This process can explain the positive correlation between high mass-loss rate and a larger departure from sphericity in progenitors of elliptical planetary nebulae. In the second type of flow, the high density in the equatorial plane is formed by a binary interaction, where the secondary star is close to, but outside the AGB envelope. The shielding of the radiation by dust results in a very slow and dense flow in the equatorial plane. We suggest this flow as an alternative explanation for the equatorial dense matter found at several hundred astronomical units around several post-AGB binary systems.     

Stellar structure and mass loss on the upper asymptotic giant branch

We examine the envelope properties of asymptotic giant branch (AGB) stars as they evolve on the upper AGB and during the early post-AGB phase. Because of the high mass-loss rate, the envelope mass decreases by more than an order of magnitude. This makes the density profile below the photosphere much shallower, and the entropy profile much steeper. We discuss the possible role of these changes in the profiles in the onset of the high mass-loss rate (superwind) and the large deviation from spherical mass loss at the termination of the AGB. We concentrate on the idea that the shallower density profile and steeper entropy profile allow the formation of cool magnetic spots, above which dust forms much more easily.     

西藏尼玛盆地东部油气显示带的发现及其勘探意义

野外地质调查过程中,在尼玛盆地东部字康勒—康嘎勒一带发现长约55 km的油气显示带,在1：25万尼玛县地质图上标注为白垩系竟柱山组。通过剖面实测及样品地球化学特征分析,采集的24件样品泥页岩有机碳含量较高,平均TOC含量为1.32%,平均生烃潜量为7.38 mg/g,有12件样品TOC大于1%,成熟度也较适中,属好—极好生油岩级别。由此认为,尼玛盆地东部赛布错坳陷生油条件好于达则错坳陷,可作为下一步盆地重点工作区域。油气显示带的发现为尼玛盆地与伦坡拉盆地的地层对比提供了依据,也为盆地下一步的重点工作开辟了新的方向。     

碳酸盐岩中有机质组成特征分析

对碳酸盐岩有机质组分进行分类时，有两种分类标准，一是主要采用煤岩学方法，二是采用孢粉学研究方法。本文使用煤岩学方法作为标准，对碳酸盐岩有机质的组成特征进行分析。按有机质来源和有机组分光性和形态等方面差别划分为内源有机质、次生有机质和陆源有机质三类。内源有机质类中分腐泥组和动物有机组，前者主要来源于菌藻类，后者则主要来源于浮游动物有机体；次生有机质中区分出微粒体、有机包裹体、沥青；陆源有机质类分类术语仍沿用煤显微组分分类系统和术语。碳酸盐岩烃源岩的有机质主要为腐泥型，有机质来源以低等藻类为主，且有机质组成特征与碳酸盐岩烃源岩的地质年代有关。碳酸盐岩还存在着差异演化的特征。