Symbiotic Stars in the Context of Binary Evolution and Metallicity     

Laurits Leedjärv 《Astrophysics and Space Science》2006,304(1-4):105-107

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Larval life span,larval settlement,and early growth of Evechinus chloroticus (Valenciennes)     

M. M. Walker 《新西兰海洋与淡水研究杂志》2013,47(4):393-397

Development, settlement, and subsequent metamorphosis on several substrata were observed in cultures of Evechinus chloroticus larvae. The period from fertilisation to metamorphosis ranged between 30 and 63 days for larvae collected from spawnings induced at 3 different times. Newly settled sea urchins collected from the field grew about 1 mm per month in aquaria. Correlation of the larval life span with the growth rate of newly settled sea urchins suggested that the earliest spawning could occur was mid‐November. This finding corroborates the results of previous histo‐logical studies of the gonads of adult sea urchins in the Hauraki Gulf, New Zealand.  相似文献   

斑节对虾4个地理群体遗传多样性的AFLP分析     

孙苗苗  杨其彬  陈百尧  朱彩艳  黄建华  江世贵  周发林 《海洋科学》2017,41(3):41-47

为研究斑节对虾(Penaeus monodon)4个地理群体的遗传背景,作者应用AFLP分子标记技术对非洲(F)、中国三亚(S)、泰国(T)和印度尼西亚(Y)的斑节对虾群体进行遗传多样性分析。选取8对引物组合对斑节对虾4个群体共128个个体进行分析比较,共获得1 000个位点,其中多态性位点数为830个,各群体多态位点比率为47.8%~58.5%;群体Nei’s遗传多样性指数为0.0917~0.1271,Shannon’s信息指数为0.1484~0.2032。4个群体间的遗传距离,Y与F之间最大,为0.331,T与S之间最小,为0.217。4个群体UPGMA聚类时,S、T与Y聚为一支,F为单独一支;128个个体的UPGMA聚类结果表明,F群体除4个个体外其余个体聚为一大支,S、T、Y群体的部分个体互相混杂。AMOVA分析发现,35.92%的变异来自于群体间,64.08%的变异来自于群体内,群体间的遗传分化系数为0.3592,表明4个群体间的遗传分化程度很大。本研究为斑节对虾遗传育种提供了种质遗传背景资料,并为斑节对虾资源的开发与利用提供基础数据。  相似文献   

Genetic changes from artificial propagation of Pacific salmon affect the productivity and viability of supplemented populations   总被引：7，自引：1，他引：6  

Reisenbichler  R. R.; Rubin  S. P. 《ICES Journal of Marine Science》1999,56(4):459-466

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Two populations of open clusters     

A. Strobel 《Astronomische Nachrichten》1989,310(5):367-373

The paper proposes a division of the local open clusters into two different disklike subpopulations on the base of the metallicity enhancement history, spatial distribution in the Galaxy and morphology of their C-M diagrams. The thin disk population objects exhibit higher metallicities and are more closely concentrated to the center and the disk of the Galaxy than the thick disk clusters. The former contain also frequently blue stragglers while the later exhibit the presence of Clump giant members, typical for the thick disk globular clusters. Kinematical properties of the two considered open cluster subpopulations remain unknown due to the lack of observational data.  相似文献   

Population statistics study of radio and gamma-ray pulsars in the Galactic plane     

Peter L. Gonthier  Sarah A. Story  Brian D. Clow  Alice K. Harding 《Astrophysics and Space Science》2007,309(1-4):245-251

We present results of our pulsar population synthesis of normal and millisecond pulsars in the Galactic plane. Over the past several years, a program has been developed to simulate pulsar birth, evolution and emission using Monte Carlo techniques. We have added to the program the capability to simulate millisecond pulsars, which are old, recycled pulsars with extremely short periods. We model the spatial distribution of the simulated pulsars by assuming that they start with a random kick velocity and then evolve through the Galactic potential. We use a polar cap/slot gap model for γ-ray emission from both millisecond and normal pulsars. From our studies of radio pulsars that have clearly identifiable core and cone components, in which we fit the polarization sweep as well as the pulse profiles in order to constrain the viewing geometry, we develop a model describing the ratio of radio core-to-cone peak fluxes. In this model, short period pulsars are more cone-dominated than in our previous studies. We present the preliminary results of our recent study and the implications for observing these pulsars with GLAST and AGILE.   相似文献   

Conservation aspects of natural populations and captive-bred stocks of turbot (Scophthalmus maximus) and Dover sole (Solea solea) using estimates of genetic diversity     

Exadactylos  Athanasios; Rigby  Mark J.; Geffen  Audrey J.; Thorpe  John P. 《ICES Journal of Marine Science》2007,64(6):1173-1181

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A review of the biology and genetics of sea lice   总被引：5，自引：0，他引：5  

Boxaspen  Karin 《ICES Journal of Marine Science》2006,63(7):1304-1316

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The resolved red giant branches of E/S0 galaxies     

Regina E. Schulte-Ladbeck  Igor O. Drozdovsky  Michèle Belfort  Ulrich Hopp 《Astrophysics and Space Science》2003,284(2):909-912

Formation paradigms for massive galaxies have long centered around two antipodal hypotheses – the monolithic-collapse and the accretion/merger scenarios. Empirical data on the stellar contents of galaxy halos is crucial in order to develop galaxy formation and assembly scenarios which have their root in observations, rather than in numerical simulations. The Hubble Space Telescope (HST) has enabled us to study directly individual stars in the nearby E/S0 galaxies Cen A, NGC 3115, NGC 5102, and NGC 404. We here present and discuss HST single-star photometry in V and I bands. Using color-magnitude diagrams and stellar luminosity functions, we gauge the galaxies' stellar contents. This can be done at more than one position in the halo, but data with deeper limiting magnitudes are desired to quantify the variation of metallicity with galactocentric radius. We here compare the color distributions of red giant stars with stellar isochrones, and we intercompare the galaxies' halo populations, noting that their total absolute V magnitudes cover the range from about –21.5 to –17.5. In the future, we plan to model the stellar metallicity distributions with the aim to constrain chemical enrichment scenarios, a step towards unravelling the evolutionary history of elliptical and lenticular galaxies. This revised version was published online in August 2006 with corrections to the Cover Date.  相似文献   

The next generation stellar population synthesis library     

Reynier Peletier 《Astrophysics and Space Science》2003,284(2):957-960

Most of the analysis of absorption lines in galaxies is done in the Lick system, defined in the 1970's and 1980's by Faber, Burstein and collaborators. Working in this system is difficult, since it is based on low resolution spectra taken with a non-linear detector without flux-calibration. Due to intrinsic errors in the published indices the Lick system limits the accuracy with which one can analyse galaxy spectra. In the last 2 years we have observed a new stellar library to replace the Lick system. It consists of 1100 stars, covering a wide range in metallicity, abundance ratio, temperature and gravity, observed at a resolution of 2.0Å (9 for Lick) from 3500–7500Å, and calibrated in flux. With this library galaxy spectra can be analysed much more accurately than before, and in much more detail. Most important, the library now makes it possible to study absorption lines of galaxies at intermediate and high redshift, something which was impossible with the Lick system. With this library it will be possible for the first time to synthesise full Spectral energy distributions of galaxies in the optical based fully on observational spectra.  相似文献