基于遗传势场法的足球机器人路径规划

以足球机器人系统为研究背景,采用了人工势场法和遗传算法相结合的方法,实现了足球机器人路径规划．首先根据势场原理设计可调参数的势场函数,再规划出已知环境下可调参数的势场函数,然后设计遗传算法中的相关适应值函数,最后用遗传算法优化势场函数中的参数,得到遗传势场法．同时利用C＋＋编程实现遗传势场法的仿真平台,并在该平台上进行仿真实验,结果表明,遗传势场法具有避障以及适于在实时环境中使用的优点,在解决实际路径规划问题中是行之有效的．     

无压隧洞水流的二维数值模拟

简述了流体体积函数法（VOF 方法）的基本原理,并用它来处理水气交界面,与标准K-ε的二方程紊流模型耦合建立了无压隧洞内流场的数学模型,在数值模拟过程中,采用非结构网格来处理复杂的边界形状,并详细给出了各种边界条件的设置.通过模拟计算,得到隧洞内水流的水面线、速度场等,并与模型试验结果进行对比分析,两者吻合较好.     

基于价值星系的企业成本管理研究

在知识经济占主导的当今社会,企业要不断加强对新知识的学习,而价值星系作为一种全新的价值创造模式,为企业所用是顺应时代潮流、符合时代要求的。文章通过对价值链与价值星系的对比,从而分析出价值星系的优势,并在此基础上提出基于价值星系的成本管理新模式。     

付里叶变换近红外漫反射光谱分析应用基础的研究

本文讨论了NIRDRSA法,该分析是建立在漫反射光谱参数(反射吸光度或KubelkaMunk函数)的线性与加合性基础上。用数学分析和实验验证的方法研究了线性和加合性,样品的近红外反射率R与样品的化学组成存在非线性的关系。当散射系数为常数时,反射吸光度A(A=-logR)和化学组成存在近似线性关系。为了改善线性,可用反射吸光度的一次微分和二次微分光谱。因此样品中任一组份的含量可以用某一多元线性函数来计算。样品的制备技术、颗粒的大小、样品层的厚度、密度可影响散射系数,因此NIRDRSA必须保持制样条件的一致。本研究还说明付里叶变换光谱仪非常适合于NIRDRSA。     

生化法快速测定蔬菜中农药残毒

用自行研制的便携式农药残毒速测仪 ,对蔬菜中残留农药进行生化检测。依据有机磷和氨基甲酸酯类农药对乙酰胆碱酯酶的活性有抑制的原理 ,绘制农药残毒———吸光度标准曲线 ,读出吸光度即得到相应的农药浓度。     

对称地中d轨道的相对能量及d^N组态稳定化能的计算

通过群论的手段，将配位化合物作为点群，得到跚离子各ｄ轨道在对称场中分裂后的洒中约表示的基函数。以此得到分裂后各ｄ轨道的相对能量。在不考虑电子配对能的情况下，计算出各对称场中ｄ＾Ｎ组态的晶体场稳定化能。     

幂赋范极值分布的条件矩刻画

{X_n}为独立同分布的离散型随机变量序列,其分布函数为F(x).得到了F(x)属于幂赋范极值分布吸引场的条件矩刻画.     

青海海北化工厂铬渣堆积场土壤铬污染状况研究

通过野外观测与室内分析相结合的方法,研究了青海海北化工厂铬矿堆渣场土壤铬污染状况。结果表明:渣场附近土壤受到严重的铬污染,其铬含量大幅度超出全国土壤铬含量和青海土壤铬环境背景值。随距离堆渣场距离的增大,土壤铬含量急剧降低。土壤铬含量与距离堆渣场的距离之间的关系均可用线性函数或幂函数来表示,幂函数优于线性函数。铬在土壤剖面中的分布呈现出上低下高的分布趋势,其分布特征与铬的独特的土壤化学特性和土壤水分运动有关。堆渣场附近土壤中铬具有很大的可迁移性,铬进入土壤后主要和土壤碳酸盐、有机质和氧化物相结合,有很大一部分存在于土壤溶液中,显著地改变了原有土壤中铬的形态分布。在对堆渣场土壤污染进行治理时必须综合考虑气候、土壤、地形因素及铬的土壤环境行为。     

不同品种烟叶碘值吸光度值与评吸质量的相关性分析

测定了72个烟叶样品的碘值吸光度值,并分析了不同品种、年份、产区烟叶的碘值吸光度值的差异,结果表明:不同产地烟叶样品的碘值吸光度值集中在4～12之间,且烟叶碘值吸光度值变异系数不大;烤烟和白肋烟不同品种烟叶的碘值吸光度值差异极显著,且烟叶等级越高,烟叶碘值吸光度值越高;2006～2008年不同产区间碘值吸光度值差异显著,且烟叶碘值吸光度值随陈化时间的延长呈现增加趋势;烟叶碘值吸光度值与香气质、浓度显著正相关,与香气量、劲头显著负相关。     

汶川震源有限差分数值模拟研究

2008年5月12日在四川汶川发生8．0级地震,震中位于龙门山断裂带上。地震激发的地震波可以用来研究震源破裂过程及地球内部的层次结构。对地震台站接收到的地震记录的拟合图重新进行了拟合,得到一个极易用数学式表达的震源时间函数,并结合龙门山的实际情况,划分为碎屑岩层、碳酸盐层及基底层模拟区域,并运用交错网格的有限差分法对声波方程进行数值模拟。研究表明,利用3个不同初始震源都能得到较好的波场快照图,而初始震源持续时间短的波场快照精度更高;不同初始震源不同地层的单点P波形图都能与根据地震台站接收记录拟合的P波形图相符合。因此,通过数值模拟能够反映汶川地震波传播的相关特征。     

Size and age of the universe

The age of the universe based on abundances of isotopes is in the range 10 billion to 15 billion years. This is consistent with the age range 12 billion to 20 billion years calculated from the evolution of the oldest galactic stars. A third estimate of the age of the universe is based on the Hubble relation between the velocities of galaxies and their distances from us, where the inverse of the Hubble parameter H is a measure of the age of a uniformly expanding universe. Evidence that has been accumulating over the past few years indicates that the expansion of the universe may exhibit a rather large local perturbation due to the gravitational attraction of the Virgo supercluster. Different types of observations still produce conflicting evidence about the velocity with which the Local Group of galaxies (of which our Milky Way system is a member) is falling into the Virgo cluster. The results to date indicate that this velocity lies somewhere in the range 0 to 500 kilometers per second. The resulting ambiguity in the flow pattern for relatively nearby galaxies makes values of H derived from galaxies with radial velocities less than 2000 kilometers per second particularly uncertain, and this restricts determinations of H to distant galaxies, for which distances are particularly uncertain. The best that can be said at present is that H(-1) yields a maximum time scale in the range 10 billion to 20 billion years.     

Extreme-Ultraviolet Flux from the Virgo Cluster: Further Evidence for a 500,000-Kelvin Component

A surprising discovery in x-ray astronomy was that clusters of galaxies often contain vast quantities of hot (20 million kelvin) diffuse gas. Substantial diffuse extreme-ultraviolet (EUV) emission has recently been detected in the Virgo cluster of galaxies. Depending on the character of the interstellar medium in our galaxy, this emission could be either an aspect of the hot cluster gas or a previously undetected 500,000-kelvin component. Analysis of the observational data in combination with our current knowledge of the interstellar medium revealed that the EUV flux cannot be an effect of the interstellar medium. Hence, a warm cluster component appears likely.     

The origin of galaxies and clusters of galaxies

Debate on how galaxies and clusters of galaxies formed has reached an interesting stage at which one can find arguments for quite different scenarios. The galaxy distribution has a complex "frothy" character that could be the fossil of a network of protoclusters or pancakes that produced galaxies. However, there are galaxies like our own that seem never to have been in a protocluster but are physically similar to the galaxies in dense clusters. Some clues to be assessed in resolving this dilemma are the possible existence of galaxy filaments, the relative ages of galaxies and clusters of galaxies, and the continuity between cluster and field galaxies and between galaxies and clusters of galaxies.     

Hydrogen 21-centimeter emission from a galaxy at cosmological distance

We have detected the neutral atomic hydrogen (HI) emission line at a cosmologically significant distance [redshift (z) = 0.18] in the rich galaxy cluster Abell 2218 with the Westerbork Synthesis Radio Telescope. The HI emission originates in a spiral galaxy 2.0 h65(-1) megaparsecs from the cluster core. No other significant detections have been made in the cluster, suggesting that the mechanisms that remove neutral gas from cluster galaxies are efficient. We infer that fewer than three gas-rich galaxies were accreted by Abell 2218 over the past 10(9) years. This low accretion rate is qualitatively consistent with low-density cosmological models in which clusters are largely assembled at z > 1.     

Percolation and galaxies

A theory is presented in which much of the structure of spiral galaxies arises from a percolation phase transition that underlies the phenomenon of propagating star formation. According to this view, the appearance of spiral arms is a consequence of the differential rotation of the galaxy and the characteristic divergence of correlation lengths for continuous phase transitions. Other structural properties of spiral galaxies, such as the distribution of the gaseous components and the luminosity, arise directly from a feedback mechanism that pins the star formation rate close to the critical point of the phase transition. The approach taken in this article differs from traditional dynamical views. The argument is presented that, at least for some galaxies, morphological and other features are already fixed by general properties of phase transitions, irrespective of detailed dynamic or other considerations.     

A search for intergalactic hydrogen in the virgo cluster

A fixed-horn antenna having a beam 10 degrees by 10 degrees , and a switched-load radiometer with traveling-wave-maser preamplifier were used to observe the 21-cm spectrum of the Virgo cluster of galaxies. An upper limit to the antenna temperature is 0.024 degrees K relative to regions outside the cluster with filters whose width is 2 Mc/sec. If the excitation temperature of the intergalactic hydrogen is enough greater than the background continuum radiation so that absorption can be ignored, and if the velocity spectrum is that defined by the galaxies, the density of optically thin neutral hydrogen in the cluster does not exceed that outside of the cluster by an amount that gives 5.6 x 10(12) solar masses in the cluster.     

The central galaxy in abell 2029: an old supergiant

A mosaic of images shows the extended structure of the cD galaxy that resides at the center of the rich cluster of galaxies Abell 2029. After correcting for the scattered light of nearby stars and galaxies, the faint halo of this giant can be traced out to a distance of more than 1 megaparsec, making it one of the largest and most luminous galaxies known. The smoothness of this halo suggests that it was formed early in the history of the cluster.     

Fermi detection of a luminous γ-ray pulsar in a globular cluster

We report on the Fermi Large Area Telescope's detection of γ-ray (>100 mega-electron volts) pulsations from pulsar J1823-3021A in the globular cluster NGC 6624 with high significance (~7 σ). Its γ-ray luminosity, L(γ) = (8.4 ± 1.6) × 10(34) ergs per second, is the highest observed for any millisecond pulsar (MSP) to date, and it accounts for most of the cluster emission. The nondetection of the cluster in the off-pulse phase implies that it contains <32 γ-ray MSPs, not ~100 as previously estimated. The γ-ray luminosity indicates that the unusually large rate of change of its period is caused by its intrinsic spin-down. This implies that J1823-3021A has the largest magnetic field and is the youngest MSP ever detected and that such anomalous objects might be forming at rates comparable to those of the more normal MSPs.     

Explaining the color distributions of globular cluster systems in elliptical galaxies

The colors of globular clusters in most large elliptical galaxies are bimodal. This is generally taken as evidence for the presence of two cluster subpopulations that have different geneses. However, here we find that, because of the nonlinear nature of the metallicity-to-color transformation, a coeval group of old clusters with a unimodal metallicity spread can exhibit color bimodality. The models of cluster colors indicate that horizontal-branch stars are the main drivers behind the empirical nonlinearity. We show that the scenario gives simple and cohesive explanations for all the key observations and could simplify theories of elliptical galaxy formation.     

IRAS 14348-1447, an Ultraluminous Pair of Colliding, Gas-Rich Galaxies: The Birth of a Quasar?

Ground-based observations of the object IRAS 14348-1447, which was discovered with the Infrared Astronomical Satellite, show that it is an extremely luminous colliding galaxy system that emits more than 95 percent of its energy at far-infrared wavelengths. IRAS 14348-1447, which is receeding from the sun at 8 percent of the speed of light, has a bolometric luminosity more than 100 times larger than that of our galaxy, and is therefore as luminous as optical quasars. New optical, infrared, and spectroscopic measurements suggest that the dominant luminosity source is a dustenshrouded quasar. The fuel for the intense activity is an enormous supply of molecular gas. Carbon monoxide emission has been detected at a wavelength of 2.6 millimeters by means of a new, more sensitive receiver recently installed on the 12-meter telescope of the National Radio Astronomy Observatory. IRAS 14348-1447 is the most distant and luminous source of carbon monoxide line emission yet detected. The derived mass of interstellar molecular hydrogen is 6 x 10(10) solar masses. This value is approximately 20 times that of the molecular gas content of the Milky Way and is similar to the largest masses of atomic hydrogen found in galaxies. A large mass of molecular gas may be a prerequisite for the formation of quasars during strong galactic collisions.