一种混合粒子群优化算法在翼型设计中的应用

提出了一种分层交换差分粒子群优化算法。作为一种混合算法,将粒子群优化算法与差分进化算法有机地结合了起来,使得粒子种群和差分种群分层交换,共享最优信息,加快了收敛速度,降低了陷入局部最优的风险,函数测试结果表现出算法具有更好的寻优性能。将算法应用到翼型设计之中,取得了良好的优化效果。     

基于线粒体细胞色素b基因序列的骨舌鱼科鱼类分子系统发育的研究

为阐明骨舌鱼科鱼类的遗传结构和进化关系,测定了美丽硬仆骨舌鱼Scleropages formosus的3个品种金龙(Gold arowana)、红龙(Red arowana)、青龙(Green arowana)细胞色素b(cyt b)基因全序列(1 141 bp),结合来自GenBank中珍珠龙Scleropages leichardti、星点珍珠龙S. jardini、非洲龙Heterotis niloticus、黑龙Osteoglossum ferrerirai、银龙O. bicirrhosum、海象Arapaima gigas的全序列,用邻接法(NJ)和最大简约法(MP)构建分子系统树,初步分析了骨舌鱼科鱼类的系统发育关系.NJ树和 MP树均一致表明,骨舌鱼类为单系类群,分为4支,支持骨舌鱼科下设4个属(坚体鱼属Scleropages、异耳鱼属Heterotis、骨舌鱼属Osteoglossum、巨骨舌鱼属Arapaima)阶元的分类系统,4个属的系统关系与其形态、生态特征表型进化和地理分布较为一致.而金龙、红龙和青龙的mtDNA Cytb的碱基差异小于1%,说明这3个龙鱼品种还在同一种的水平上.     

吸收变异的粒子群算法及应用

提出了一种改进的粒子群算法,称为ConvergencemutationPSO(CM_PSO)。该算法根据粒子群中各粒子的适应值动态地调整粒子数量,把部分适应度差的粒子适当汇聚到适应度好的区域,在不损失全局搜索能力的同时,增强局部搜索能力。在将该算法应用于雷达组网误差配准问题中,提出了一种基于CM_PSO的误差配准技术。仿真表明,该算法能有效配准,与对比方法相比较,具有更好的收敛精度和更快的进化速度。     

Observations of the atmospheres and winds of O-stars,LBVs and Wolf-Rayet stars

This review summarises recent studies of O-stars, Luminous Blue Variables (LBVs) and Wolf-Rayet (WR) stars, emphasising observations and analyses of their atmospheres and stellar winds yielding determinations of their physical and chemical properties. Studies of these stellar groups provide important tests of both stellar wind theory and stellar evolution models incorporating mass-loss effects. Quantitative analyses of O-star spectra reveal enhanced helium abundances in Of and many luminous O-supergiants, together with CNO anomalies in OBN and Ofpe/WN9 stars, indicative of evolved objects. Enhanced helium, and CNO-cycle products are observed in several LBVs, implying a highly evolved status, whilst for the WR stars there is strong evidence for the exposition of CNO-cycle products in WN stars, and helium-burning products in WC and WO stars. The observed wind properties and mass-loss rates derived for O-stars show, in general terms, good agreement with predictions from the latest radiation-driven wind models, although some discrepancies are apparent. Several LBVs show similar mass-loss rates at maximum and minimum states, contrary to previous expectations, with the mechanism responsible for the variability and outbursts remaining unclear. WR stars exhibit the most extreme levels of mass-loss and stellar wind momenta. Whilst alternative mass-loss mechanisms have been proposed, recent calculations indicate that radiation pressure alone may be sufficient, given the strong ionization stratification present in their winds.     

The massive star distribution in the Galaxy and the Magellanic Clouds

The numbers and distribution of Population I O-type stars and Wolf-Rayet stars are reviewed. The numbers of known WR stars in the Galaxy, the LMC and the SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.     

A spectroscopic analysis of B stars in the SMC cluster NGC 330

Medium resolution (2A/px) but high s/n spectra of approximately twenty of the brightest blue stars in the young open cluster NGC 330 in the SMC have been analyzed in order to determine their atmospheric parameters and the evolutionary status. Stellar parameters are determined by comparison with LTE and NLTE model atmosphere calculations and an HR diagram constructed. Luminosities of the sample stars lie in the range 4.0L _*/L )<5.0 and spectral types between O9 and late-B. The stars in our sample appear to define 4 groups: main-sequence B-stars (B2-B4), B-supergiants (B4) in a blue-loop phase of evolution, a small number of blue stragglers (O9-B0 near main-sequence stars) and a group of luminous giants (B1-B2) which reside in the so-called post main-sequence gap of the HR diagram. Furthermore, we have confirmed spectroscopically the very high incidence of Be stars in this cluster. Finally the almost complete absence of metal lines (at this resolution) is in keeping with the expected very low metallicity of the SMC.     

基于适当控制翼型演化历程的气动设计方法

本文提出一种翼型设计的新方法,它基于适当控制翼型演化历程,采用求解非定常流动控制方程的方法,实现了翼型反问题的高效求解.同时在笛卡尔坐标系中应用Level-Set函数,避免了贴体动网格的采用,从而大大减少了所需计算工作量.     

非平行边界层C型失稳的非线性演化(英文)

提出用抛物化稳定性方程(PSE)新方法,研究非平行边界层从层流向湍流转捩的C型失稳的演化过程,特别是非线性演化问题。研究了至关重要的初始条件,包括各扰动谐波的初始解、初始站均流变形的模拟、以及通过对线性 PSE 的求解获得 TS波和C型亚谐扰动的初始站值等。发展了高精度的数值方法,满足PSE的关键性正规化条件,实现非线性抛物化稳定性方程的有效求解和稳定推进。算例展示了Blasius边界层的C型失稳的非线性演化过程,与典型实验结果相吻合。     

Primordial Helium and ΔY/ΔZ from H II Regions and from Fine Structure in the Main Sequence Based on Hipparcos Parallaxes

The primordial helium abundance YP is important for cosmology and the ratio Y/Z of the changes relative to primordial abundances constrains models of stellar evolution. While the most accurate estimates of YP come from emission lines in extragalactic H II regions, they involve an extrapolation to zero metallicity which itself is closely tied up with the slope Y/Z. Recently certain systematic effects have come to light in this exercise which make it useful to have an independent estimate of Y/Z from fine structure in the main sequence of nearby stars. We derive such an estimate from Hipparcos data for stars with Z Z and find values between 2 and 3, which are consistent with stellar models, but still have a large uncertainty.