STUDY ON ~(210) Po IN MARINE ORGANISMS IN NORTH CHINA WATERS

INTRODUCTIONWiththedevelopmentofcoastalnuclearpowerandmarinenuclearestablishments,peoplepaymoreandmoreattentiontothedistribution ,behaviorandpathwaysofsomeman maderadionuclidesinmarineenvironment.Thedischargedartificialradionuclidesoverlieabackgroundofnaturallyoccurringradionu clideswhicheitheralreadyexistedinmarineenvironmentorwasenhancedbysomeotherhumanactivi ties.Goodunderstandingofsomeman incurredradionuclides’impactsonpeopleandmarineorganismsrequiresknowledgeofsomecriticalnaturalradi…     

河套地区全新世黄河古河道的分布及期次划分

黄河古河道的分布及其年代学框架的建立对于探讨黄河迁移规律、重建古气候演化历史具有重要意义。通过Landsat8遥感影像解译、1∶5万野外地质地貌调查、钻孔资料分析,结合剖面实测基本判定了色尔腾山以南至现代黄河以北河套平原区黄河埋藏古河道的分布,,采用OSL与14C测年较精确地确定了黄河古河道的年代。依据年代学研究结果,将全新世黄河古河道划分为三期:Ⅰ期古河道,分南北两支,南支分布在复兴镇西北部,埋深2~6 m,北支分布于呼勒斯太中南部,埋深8.2~9 m,时代为9.93~7.4 ka B.P.;Ⅱ期古河道,河道主体分布在色尔腾山山前,呈北西─南东向,埋藏于现今乌加河古河道下部4~11m处,南北最宽处约1.5km。塔尔湖区存在同一期的古河道,埋深7~9 m,以东西向展布为主,时代为7.4~4.1 ka B.P.;Ⅲ期古河道,呼勒斯太中部、塔尔湖中南部及复兴南部都曾发育,但河道主体为塔尔湖区的古河道,埋深2~9 m,时代为4.1~1.2 ka B.P.。黄河古河道分布及时代确定有助于更深入地研究黄河在河套段演化历史,为河套地区的水利建设和农业生产提供参考和借鉴。     

黄土热释光测年问题

回顾了热释光测年的简史,展示了我国黄土热释光测年的现状,表明尚达不到建立可靠而精确的地质年代标尺的要求,其原因在于问题的复杂性,而主要是样品的残余热释光信号问题。目前,红外光释光法的初步成功显示了良好的前景。     

勉略缝合带三岔子辉绿岩墙锆石U-Pb年龄及Hf同位素组成——古特提斯洋壳俯冲的年代学证据

为了弄清楚勉略构造带中三岔子岛弧火山岩的形成时代及源区特征,对南秦岭勉略缝合带三岔子岛弧蛇绿混杂岩中的辉绿岩墙样品进行了锆石U-Pb年代学、锆石Hf同位素组成及微量元素组成研究。结果表明,三岔子辉绿岩中的锆石主要包括2个年龄区间:有8颗锆石记录古生代年龄信息,其n(206Pb)/n(238U)年龄为264~487 Ma,w(Th)/w(U)为0.4~0.8,其中有6颗锆石的N(176Hf)/N(177Hf)初始值为0.281 934~0.282 292,对应的εHf(t)值为-9.4~-16.4,为典型的壳源岩浆锆石,另外2个测点(BQG-014,BQG-021)的N(176Hf)/N(177Hf)为0.282 722~0.282 798,对应的εHf(t)值为4.5~6.3,为典型的幔源岩浆锆石;有15颗锆石记录了元古代—太古代的年龄信息,N(207Pb)/N(206Pb)年龄主要为1 713~2 559 Ma,N(176Hf)/N(177Hf)初始值为0.281 288~0.282 263,对应的εHf(t)值为-1.3~8.7,绝大部分锆石的εHf(t)值大于2,显示出幔源岩浆锆石的特征。根据锆石Hf同位素组成,BQG-014和BQG-021样品为典型的幔源岩浆锆石,因此,其形成年龄(264~295 Ma)应代表了勉略洋消减过程中一次重要的大陆弧岩浆作用时间。     

Characteristics and tectonic setting of volcanic rocks in Early Cretaceous Baiyingaolao Formation of Keyouzhongqi area，Inner Mongolia

The authors studied zircon LA-ICP-MS U-Pb dating,the zircon Hf isotope and geochemistry of acidic volcanic rocks in Baiyingaolao Formation of Keyouzhongqi area,Inner Mongolia,and discussed the chronology, source region and tectonic setting of the volcanic rocks in the studied area． The clear oscillatory zoning of zir- cons indicates a typical magmatic origin,and the results of dating show that the volcanic rocks of Baiyingaolao Formation were formed in Early Cretaceous (121.5 ±1.0 Ma)． The features of major and trace elements show that the rocks are alkali-rich,poor in calcium and magnesium with enrichment in LILEs like Th,U,K and Gd and depletion in HFSEs,e.g. Nb,Ta,Sr and Ti． The fact implies that they were the products of partial melting of the crust． εHf(t) = ( +6.30--+9.06) and TDM2=600--835 Ma,suggest the magma originated from par- tial melting of the young crust． Combined with the evolution of regional tectonic structure,the authors conclude that the acidic volcanic rocks of Baiyingaolao Formation may be formed under the extensional environment relat- ed to the subduction of Paleo-Pacific Plate．     

Petrogenesis and tectonic setting of granite porphyry in Keyouzhongqi area,Inner Mongolia

The authors studied the geochemistry,zircon U-Pb ages,Hf isotope of the granite porphyry and its petrogenesis and tectonic setting in the studied area． The zircon U-Pb dating indicates the formation of the gran- ite porphyry is in Early Cretaceous (125． 1 ±1． 5 Ma)． The granite porphyry has high-SiO2and alkali-rich fea- tures,which belongs to high-K calc-alkaline series rocks (A/CNK = 0． 95%--1． 25%)． The analyses of trace elements show the characteristics of a swallow-shaped ＲEE distribution pattern with enrichment in LＲEEs and most of LILEs and HFSEs,depletion in Ba,Sr,Nb,P and Ti,and especially strong depletion in Eu,which indicates the granite porphyry belongs to the aluminous A-type granite． Their εHf(t)range from 5． 94 to 8． 80 with Hf two-stage model ages (TDM2) of 620 Ma to 803 Ma． Combining with the regional tectonic background, we conclude that the source of the rocks is the new crust materials accreted from depleted mantle in Neoprotero- zoic and is the product of partial melting of middle and lower crustal rocks,which may be suffered from the dual impact of the subduction of the Palaeo-Pacific Ocean and the closure of the Mongol-Okhotsk Ocean．     

X-ray bright sources in the Chandra Small Magellanic Cloud Wing Survey – detection of two new pulsars

We investigate the X-ray and optical properties of a sample of X-ray bright sources from the Small Magellanic Cloud (SMC) Wing Survey. We have detected two new pulsars with pulse periods of 65.8 s (CXOU J010712.6−723533) and 700 s (CXOU J010206.6−714115), and present observations of two previously known pulsars RX J0057.3−7325 (SXP101) and SAX J0103.2−7209 (SXP348). Our analysis has led to three new optical identifications for the detected pulsars. We find long-term optical periods for two of the pulsars, CXOU J010206.6−714115 and SXP101, of 267 and 21.9 d, respectively. Spectral analysis of a subset of the sample shows that the pulsars have harder spectra than the other sources detected. By employing a quantile-based colour–colour analysis we are able to separate the detected pulsars from the rest of the sample. Using archival catalogues we have been able to identify counterparts for the majority of the sources in our sample. Combining this with our results from the temporal analysis of the Chandra data and archival optical data, the X-ray spectral analysis, and by determining the X-ray to optical flux ratios we present preliminary classifications for the sources. In addition to the four detected pulsars, our sample includes two candidate foreground stars, 12 probable active galactic nuclei, and five unclassified sources.     

Optical follow-up of new Small Magellanic Cloud wing Be/X-ray binaries

We investigate the optical counterparts of recently discovered Be/X-ray binaries in the Small Magellanic Cloud (SMC). In total four sources, SXP101, SXP700, SXP348 and SXP65.8 were detected during the Chandra survey of the wing of the SMC. SXP700 and SXP65.8 were previously unknown. Many optical ground-based telescopes have been utilized in the optical follow-up, providing coverage in both the red and blue bands. This has led to the classification of all of the counterparts as Be stars and confirms that three lie within the Galactic spectral distribution of known Be/X-ray binaries. SXP101 lies outside this distribution and is the latest spectral type known. Monitoring of the Hα emission line suggests that all the sources barring SXP700 have highly variable circumstellar discs, possibly a result of their comparatively short orbital periods. Phase-resolved X-ray spectroscopy has also been performed on SXP65.8, revealing that the emission is indeed harder during the passage of the X-ray beam through the line of sight.     

CCD‐Δa and BV R photometry of NGC 7296

The first CCD photometric investigation of the open cluster NGC 7296 up to now was performed within the narrow band Δa photometric system, which enables us to detect peculiar objects. A deeper investigation of that cluster followed, using the standard BV R ‐Bessel filter set. The age and E (B – V ) was determined independently to log t = 8.0 ± 0.1 and 0.15 ± 0.02, respectively by using Δa and broadband photometry. In total five Be/Ae objects and two metal‐weak stars showing significant negative Δa ‐values as well as one classical chemically peculiar star could be identified within that intermediate age open cluster. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Be Stars in Binaries

A brief review of Be stars in binaries is presented. Attention is paid to systems, where the Be phenomenon is clearly connected to the duplicity, but is not a simple consequence of mass transfer.