White-to-white corneal diameter: normal values in healthy Iranian population obtained with the Orbscan II

AIMTo determine the normative values of white-to-white corneal diameter with Orbscan II Topography System and to compare right and left eyes data in the normal young population.

Influence of Interactions on Populations for Hyperons in Neutron Stars

The numerical results of the populations for the baryon octet in neutron star matter have been presented by solving a set transcendental equations in the framework of the relativistic mean field approximation. The influence of the hyperon interactions on hyperon populations in neutron star matter is discussed. The results manifest that when the ratio of the hyperon-to-nucleon couplings increases, all hyperons appear towards low baryon density direction.

面向多目标柔性作业车间调度的强化学习NSGA-II算法

针对非支配排序遗传算法(NSGA-II,non-dominated sorting genetic algorithm II)在求解柔性作业车间多目标优化调度问题中多样性不足、易于早熟与局部收敛的缺点,提出一种基于强化学习的改进NSGA-II算法(RLNSGA-II,reinforcement learning non-dominated sorting genetic algorithm II)。为避免NSGA-II陷入局部收敛问题引入双种群进化策略,利用性别判定法将种群拆分为两个种群,并在进化过程中采用不同的交叉变异算子,增加算法的局部和全局搜索能力;为解决NSGA-II精英策略造成多样性不足的问题,融合多个多样性度量指标,利用强化学习动态优化种群迭代过程中的拆分比例参数以保持多样性,改善算法收敛性能。最后通过Kacem标准算例进行了仿真实验与性能分析,验证了RLNSGA-II的有效性与优越性。

Radioactive Ages of Metal-Poor Halo Stars

The abundances of long-lived radioactive elements Th and U observed in metal-poor halo stars can be used as chronometers to determine the age of individual stars, and hence set a lower limit on the age of the Galaxy and hence of the universe. This radioactive dating requires the zero-decay productions of Th and U, which involves complicated r-process nucleosynthesis calculations. Several parametric r-process models have been used to calculate the initial abundance ratios of Th/Eu and U/Th, but, due to the sharp sensitivity of these models to nuclear physics inputs, the calculations have relatively large uncertainties which lead to large uncertainties in the age determinations. In order to reduce these uncertainties, we present a simple method to estimate the initial productions of Th and U, which only depends on the solar system abundances and the stellar abundances of stable r-process elements. From our calculations of the initial abundance ratios of Th/Eu and U/Th, we re-estimate the ages of those very metal-poor halo stars with published abundances of Th and U. Our age estimates are consistent, within the errors, with the other age determinations derived from r-process models, and offer useful constrains for r-process theoretical calculations. The advantages and limitations of our simple method of radioactive dating are discussed.

Test observations that search for metal-poor stars with the Guoshoujing Telescope (LAMOST)

Metal-deficient stars are regarded as fossils of the early generation of stars and therefore make crucial observational targets related to stellar astrophysics. They provide fundamental information and insights on properties of the very early stage of the chemical history of the Galaxy and have been investigated for decades. The unique design of the Guoshoujing Telescope （LAMOST）, such as its large field and multi-object observational capability, enables it to be an excellent tool for searching for these metal-poor stars in the Milky Way. This work reports the result of test observations which search for metal-poor stars with LAMOST, during which nine candidate metal-poor stars with [Fe/H] ≤ - 1.0 were newly detected based on the low-resolution spectroscopic observations of the LAMOST commissioning data. The sample of stars demonstrates the efficiency of selecting from the input catalog, as well as the ability of LAMOST to enlarge the sample of metal-poor stars in the Milky Way. Furthermore, the sample of stars could be used for future calibrations of the LAMOST stellar pa- rameter pipeline.

Investigation of star formation toward the Sharpless 155 H II region

We present a comprehensive study of star formation toward the H II re- gion Sharpless 155 （$155）. Star-formation activities therein were investigated based on multi-wavelength data from optical to the far-infrared. The surface density distri- bution of selected 2MASS sources toward S 155 indicates the existence of a compact cluster, which is spatially consistent with the position of the exciting source of the Htt region, HD 217086. A sample of more than 200 sources with excessive emission in the infrared were selected based on their 2MASS color indices. The spatial distri- bution of the sample sources reveals the existence of three young subclusters in this region, among which subcluster A is spatially coincident with the bright rim of the H II region. In addition, photometric data from the WISE survey were used to identify and classify young stellar objects （YSOs）. To further explore the evolutionary stages of the candidate YSOs, we fit the spectral energy distributions of 44 sources, which led to the identification of 14 Class I, 27 Class II and 3 Class Ⅲ YSOs. The spatial distribu- tion of the classified YSOs at different evolutionary stages presents a spatiotemporal gradient, which is consistent with a scenario of sequential star formation. On the other hand, Herschel PACS observations toward the interface between S 155 and the ambi- ent molecular cloud disclose an arc-shaped dust layer, the origin of which could be attributed to the UV dissipation from early type stars, e.g. HD 217061, in S155. Four dusty cores were revealed by the Herschel data, which hints at new generations of star formation.

Genetic polymorphism of mitochondrial DNA HVS-I and HVS-II of Chinese Tu ethnic minority group

We analyzed the two hypervariable segments HVS-I and HVS-II of 108 Chinese Tu ethnic minority group samples for forensic and population genetics purposes, Comparing with Anderson sequence, 79 polymorphic loci in HVS-I and 40 in HVS-II were found in Chinese Tu ethnic minority group mtDNA sequences, and 90 and 64 haplotypes were then defined. Haplotype diversity and the mean pairwise differences were 0.9903±0.0013 and 5.7785 in HVS-I, and 0.9777±0.0013 and 3.5819 in HVS-II, respectively. By analyzing the hypervariable domain from nucleotide 1,6180 to 1,6193 in HVS-I, we defined some new types of sequence variations. We also compared the relationship between Tu population and other populations using mtDNA HVS-I sequences. According to Rst genetic distances, the phylogenetic tree showed that the Tu population, the Xi＇an Han population, the Chinese Korean, and the Mongol ethnic group were in a clade. This indicated a close genetic relationship between them. There were far relations between the Tu population and other Chinese southern Han populations, Siberian, European, African, and other foreign populations. The results suggest that Tu population has a multi-origin and has also merged with other local populations.

Lithium Abundance of Metal-poor Stars

High-resolution, high signal-to-noise ratio spectra have been obtained for 32 metal-poor stars. The equivalent widths of Li γ6708 ? were measured and the lithium abundances were derived. The average lithium abundance of 21 stars on the lithium plateau is 2.33±0.02 dex. The Lithium plateau exhibits a marginal trend along metallicity, dA(Li)/d[Fe/H] = 0.12±0.06, and no clear trend with the effective temperature. The trend indicates that the abundance of lithium plateau may not be primordial and that a part of the lithium was produced in Galactic Chemical Evolution (GCE).

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 important information about the Galactic chemical evolution.

The lack of carbon stars in the Galactic bulge

In order to explain the lack of carbon stars in the Galactic bulge, we have made a detailed study of thermal pulseasymptotic giant branch （TP-AGB） stars by using a population synthesis code. The effects of the oxygen overabundance and the mass loss rate on the ratio of the number of carbon stars to that of oxygen stars in the Galactic bulge are discussed. We find that the oxygen overabundance which is about twice as large as that in the solar neighbourhood （close to the present observations） is insufficient to explain the rareness of carbon stars in the bulge. We suggest that the large mass loss rate may serve as a controlling factor in the ratio of the number of carbon stars to that of oxygen stars.

Multi-wavelength study of triggered star formation around 25 H II regions

We investigate 25 H II regions that show bubble morphology in 13CO（1-0） and infrared data, to search for quantitative evidence of triggered star formation by processes described by the collect and collapse （CC） and radiatively driven implosion （RDI） models. These H II regions display the morphology of a complete or partial bubble at 8 μm, and are all associated with the molecular clouds that surround them. We found that the electron temperature ranges from 5627 K to 6839 K in these H II regions, and the average electron temperature is 6083 K. The age of these H II regions is from 3.0× 10^5 yr to 1.7 × 10^6 yr, and the mean age is 7.7 × 10^5 yr. Based on the mor- phology of the associated molecular clouds, we divide these H II regions into three groups, which may support CC and RDI models. We select 23 young IRAS sources which have an infrared luminosity of 〉 10^3 Lo in 19 H II regions. In addition, we iden- tify some young stellar objects （including Class I sources）, which are only concen- trated in H II regions G29.007＋0.076, G44.339-0.827 and G47.028＋0.232. The poly- cyclic aromatic hydrocarbon emissions of the three H II regions all show a cometary globule. Comparing the age of each H II region with the characteristic timescales for star formation, we suggest that the three H II regions can trigger clustered star forma- tion by an RDI process. In addition, we detect seven molecular outflows in the five H II regions for the first time. These outflow sources may be triggered by the corresponding H II regions.

Classification of stellar populations in globular clusters

Possessing multiple stellar populations has been accepted as a common feature of globular clusters（GCs）. Different stellar populations manifest themselves with different chemical features,e.g. the well-known O-Na anti-correlation. Generally, the first（primordial） population has O and Na abundances consistent with those of field stars with similar metallicity; while the second（polluted） population is identified by their Na overabundance and O deficiency. The fraction of the populations is an important constraint on the GC formation scenario. Several methods have been proposed for the classification of GC populations. Here we examine a criterion derived based on the distribution of Galactic field stars, which relies on Na abundance as a function of [Fe/H], to distinguish first and second stellar populations in GCs. By comparing the first population fractions of 17 GCs estimated by the field star criterion with those in the literature derived by methods related to individual GCs, we find that the field star criterion tends to overestimate the first population fractions. The population separation methods,which are related to an individual GC sample, are recommended because the diversity of GCs can be taken into consideration. Currently, more caution should be exercised if one wants to regard field stars as a reference for the identification of a GC population. However, further study on the connection between field stars and GCs populations is still needed.

A search for metal-poor stars pre-enriched by pair-instability supernovae I. A pilot study for target selection from Sloan Digital Sky Survey

We report on a pilot study on identifying metal-poor stars pre-enriched by Pair-Instability Supernovae（PISNe）.Very massive,first generation（Population Ⅲ） stars（140 M⊙≤M≤260 M⊙）end their lives as PISNe,which have been predicted by theories,but no relics of PISNe have been observed yet.Among the distinct characteristics of the yields of PISNe,as predicted by theoretical calculations,are a strong odd-even effect,and a strong overabundance of Ca with respect to iron and the solar ratio.We use the latter characteristic to identify metal-poor stars in the Galactic halo that have been pre-enriched by PISNe,by comparing metallicites derived from strong, co-added Fe lines detected in low-resolution（i.e.,R=λ/△λ～2000）spectra of the Sloan Digital Sky Survey（SDSS）,with metallicities determined by the SDSS Stellar Parameters Pipeline（SSPP）.The latter are based on the strength of the CaⅡ K line and assumptions on the Ca/Fe abundance ratio.Stars are selected as candidates if their metallicity derived from Fe lines is significantly lower than the SSPP metallicities.In a sample of 12 300 stars for which SDSS spectroscopy is available,we have identified 18 candidate stars.Higher resolution and signal-to-noise ratio spectra of these candidates are being obtained with the Very Large Telescope of the European Southern Observatory and the XSHOOTER spectrograph,to determine their abundance patterns,and to verify our selection method.We plan to apply our method to the database of several million stellar spectra to be acquired with the Guo Shou Jing Telescope （LAMOST）in the next five years.

基于动态双种群NSGA2算法的分布式柔性作业车间调度研究

在分布式柔性作业车间多目标调度问题的求解过程中,存在调度规模大、多个目标难以协调等缺陷。针对上述缺陷,提出了一种改进的非支配排序遗传算法Ⅱ(NSGA2),并对分布式柔性作业车间多目标调度问题进行了求解。首先,建立了以完工时间、机器负荷、能耗为优化目标的分布式柔性作业车间多目标调度模型;然后,基于帕累托(Pareto)等级特点设计了一种动态双种群搜索策略和种群划分机制,以替代传统的选择操作,并对每个种群采用了不同的搜索策略;针对关键工厂,在第二个种群中设计了局部搜索策略,基于Pareto等级的支配关系设计了Q学习的状态、奖励函数,采用Q学习对双种群的数量比例进行了自适应调整;最后,采用扩展的基准算例对该改进算法的有效性进行了验证,并将其与其他算法进行了对比分析。研究结果表明:采用动态双种群搜索策略改进的NSGA2算法能有效保持种群多样性,且不易陷入局部最优,提高了算法的求解质量。该改进算法与传统NSGA2算法相比,多样性评价指标平均提高了15.34%,收敛性评价指标平均提高了76.37%,证明了该算法在解决分布式柔性作业车间多目标调度问题上的优越性。

草酰胺衍生物桥联双核镍配合物从头算研究

采用LanL2DZ基组 ,对N,N′ 双(2 苯甲酸根)草酰胺桥联双核镍配合物Ni(obbz)Ni(H2O)4 进行从头计算研究 ,探讨该配合物单、三重态的电子组态的稳定性、电子结构特征及电子自旋布居规律等。计算结果表明 ,该配合物分子的三重态比单重态稳定 ,因此 ,该配合物择型于三重态的电子组态。电子自旋主要布居于八面体环境的Ni(1)中心上 ,而处于四方配位环境的Ni(2)中心则没有发现电子自旋布居。同时 ,Ni(2)中心主要参与的分子轨道都处于低能区 ,表明Ni(2)中心的配位是相当稳定的 ,这与实验规律相符。

FiSATⅡ软件支持下的体长股分析法探讨

文章重点介绍了运用FiSAT Ⅱ软件以迭代法求解捕捞死亡系数的具体过程,同时比较了传统与FiSAT Ⅱ下的体长股分析法的结果。结果发现,2种方法计算的资源量比值(NF/NT)总体表现为随体长增加而增大,但对于中间体长组,两者差异更小。FiSAT II软件中的实际种群分析模块是推算捕捞死亡系数(F)的好方法。理论上来说,因其利用了反复迭代,使精度提高,其所得鱼类资源量更加真实准确。通过自我控制体长组缺失实验发现,在运用体长股法估算鱼类资源量时,最小体长组的缺失引起最大偏离,达到10%以上。

草酰胺桥联双核铜配合物结构单元的从头算

运用Gaussian 94W量子化学程序包 ,采用LanL2DZ基组 ,对草酰胺桥联双核铜配 (聚 )合物结构单元Cu2 (oxen) (OH) 2 [H2 oxen =N ,N' 二 ( 2 胺乙基 )草酰胺 ](包括顺、反构型及其单、三重态电子组态 )进行从头算研究 ,探讨该配合物结构单元的稳定性 ,并从电荷布居及分子轨道组成等电子结构特征分析这种配合物反式三重态比较稳定的原因 .计算结果与实验规律相符合 .

基于线粒体COⅡ基因序列的中华蜜蜂地理种群的遗传多样性研究

通过分析我国20个不同地理种群中蜂线粒体COⅡ序列的变异,对中华蜜蜂群体遗传分化程度遗传多样性进行全面研究。结果表明：COⅡ基因部分序列中共发现16个变异位点和18个单倍型,核苷酸差异数的平均值为0.939,核苷酸分歧度（Dxy）在0.1%-0.965%之间变化,核苷酸遗传距离为-0.007%-1.489%。总种群的Fst为0.4978,差异均极显著（P〈0.001）。研究结果显示种群总体单倍型多样性较为丰富,种群间核苷酸分歧度差异很大。20个东方蜜蜂不同地理种群间存在显著的遗传分化。

转基因抗虫棉根际卡那霉素抗性细菌种群动态及nptⅡ基因漂移检测

【目的】研究转基因抗虫棉根际卡那霉素抗性细菌的种群动态,检测转基因棉卡那霉素抗性细菌nptII基因漂移。【方法】采用常规培养方法分析了转基因抗虫棉GK12、GK19、33B、SGK321,常规棉泗棉3号、33、石远321等7个棉花品种根际卡那霉素抗性细菌种群在棉花整个生育期的种群动态变化。以质粒pBI121为对照,设计nptII基因特异性引物,采用PCR方法对分离的根际卡那霉素抗性细菌菌株进行nptII基因漂移检测。【结果】7个棉花品种根际卡那霉素抗性细菌数量随时间延长而减少,同一棉花品种不同采样时间卡那霉素抗性细菌数量差异显著,而同一采样时间抗虫棉和对应的受体棉间差异不显著。Simpson、Shannon-Wiener多样性指数以及Pielou均匀度指数计算结果表明,受体棉根际卡那霉素抗性细菌群落的多样性高于转基因棉。PCR检测结果表明,21株卡那霉素抗性细菌菌株中18株发现有阳性片段,但其测序结果与卡那霉素抗性基因序列比对的同源性未能达到100%,不能判断nptII是否发生了转移。【结论】根际卡那霉素抗性细菌的数量在转基因棉与对应受体棉之间差异不显著,受体棉根际卡那霉素抗性细菌群落多样性指数高于转基因棉,更均匀稳定。未发现转基因棉卡那霉素抗性标记基因nptII向根际细菌的基因漂移。

演化的星族合成方法

演化的星族合成方法是在给定恒星形成率和初始质量函数的前提下，利用理论的恒星演化轨迹和恒星光谱库得到的组合特征（光谱，光度），拟合星系、星团等恒星复合天体的观测特征，给出其中星族组成的一种有效方法。对演化的星族合成方法在天体物理研究中的重要意义及其原理和算法以及影响演化星族合成方法结果的最主要的四个输入量：恒星演化轨迹、恒星光谱库、初始质量函数和恒星形成率进行了评述。