Global value of Hubble constant

Multiaperture photometry in V (5500Å), r (6738Å) and IV (10500Å) of 52 spirals in nearby clusters Virgo, Fornax and Grus and farther clusters Cancer, Zw 74-23 and Peg I in the redshift range up to 6000 Km s⁻¹ was combined with HI width to derive three independant distances for each galaxy in these clusters.The plot between the mean distance of each cluster and its redshift, indicates the Hubble ratios of distant clusters Cancer, Zw 74-23 and Peg I are about 77 Km s⁻¹ Mpc⁻¹. Further, the Hubble ratios of distant clusters vary only from 76.3 to 78.9 Km s⁻¹ Mpc⁻¹ while those of nearby clusters Virgo, Fornax and Grus vary through a large range of 58.5 to 83.5 Km s⁻¹ Mpc⁻¹. We interpret these data by postulating a systematic motion toward Virgo for the Local Group.The best value for the global Hubble constant from farther and nearby clusters is derived as 74.3± 4 Km s⁻¹ Mpc⁻¹ and an average value of 289±60 Km s⁻¹ for the infall velocity of the Local Group toward Virgo is also derived.     

The X-ray evolution of galaxies: implications for future X-ray observatories

The X-ray evolution of the luminosity of normal galaxies is primarily driven by the evolution of their X-ray binary populations. The imprints left by a cosmological evolution of the star formation rate (SFR) will cause the average X-ray luminosity of galaxies to appear higher in the redshift range 1–3. As reported by White and Ghosh [ApJ, 504 (1998) L31] the profile of X-ray luminosity with redshift can both serve as a diagnostic probe of the SFR profile and constrain evolutionary models for X-ray binaries. In order to observe the high redshift (z>3) universe in the X-ray band, it is necessary to avoid confusion from foreground field galaxies. We report on the predictions of these models of the X-ray flux expected from galaxies and the implications for the telescope parameters of future deep universe X-ray observatories.     

Elliptical model for surface topography prediction in five-axis flank milling

In five-axis flank milling operations, the intersecting surfaces of different cutting edges create roughness on the milled surfaces that cannot be ignored in situations with strict requirements, especially in aeronautical manufacturing. To focus on motion problems in milling operations, this paper presents a new model that utilizes elliptical paths as cutting edge trajectories on 3D surface topography machined by peripheral milling. First, the cutter parallel axis offset and location angle are considered, which change the location of the ellipse center and intersection point of the cutting edges. Then, through the proposed model, the predicted surface topography is obtained, and the factors that affect the development tendency of roughness are analyzed. Next, the effects of the cutter location position (CLP) geometric parameters, cutter parallel axis offset and curvature on the roughness are evaluated by a numerical simulation. Finally, machining tests are carried out to validate the model predictions, and the results show that the surface topography predictions correspond well with the experimental results.     

椭圆轨道卫星编队飞行的最优控制研究

研究了椭圆轨道卫星编队飞行的队形保持问题,设计了李雅普诺夫(Lyapunov)控制律,并用遗传算法对控制律进行了优化。为克服遗传算法局部寻优能力差的缺点,对遗传算法进行了改进,设计了自适应模拟退火遗传算法。仿真结果表明,采用Lyapunov方法进行队形保持能提高位置保持的精度,且在经过遗传算法优化后,所消耗的燃料基本与线性二次型(LQR)方法一致;同时,减少了计算时间,有利于星上计算机的实现。     

The role of ultraviolet imaging in studies of resolved and unresolved young stellar populations. M31 and M33

We discuss the relevance of UV data in the detection and characterization of hot massive stars and young stellar populations in galaxies. We show results from recent extensive surveys in M31 and M33 with Hubble Space Telescope (HST) multi-wavelength data including UV filters, which imaged several regions at a linear resolution (projected) of less than half a pc in these galaxies, and from GALEX far-UV and near-UV wide-field, low-resolution imaging of the entire galaxies. Both datasets allow us to study the hierarchical structure of star formation: the youngest stellar groups are the most compact, and are often arranged within broader, sparser structures. The derived recent star-formation rates are rather similar for the two galaxies, when scaled for the respective areas. We show how uncertainties in metallicity and type of selective extinction for the internal reddening may affect the results, and how an appropriate complement of UV filters could reduce such uncertainties, and significantly alleviate some parameter degeneracies.     

X-ray broad line emission in Seyfert galaxies: Mrk 766 and NGC 4051

Long (>100 ks) observations of the bright Seyfert galaxies Mrk 766 and NGC 4051 have been obtained using XMM-Newton. The RGS 5–38 Å spectra reveal evidence of broad features. These can be modelled with relativistic emission lines coming from the immediate vicinity of a massive rotating black hole. Lines of OVIII, NVII and CVI are required to reproduce the spectrum of Mrk 766, whereas the spectrum of NGC 4051 can be modelled using a single, even broader OVIII line. Both Seyferts also exhibit broad iron line emission in the 2–8 keV range, and the data available thus far suggest that the strength of the low-energy emission lines and the strength of the iron line may be correlated.     

Observations of Metals in the Intra-Cluster Medium

Because of their deep gravitational potential wells, clusters of galaxies retain all the metals produced by the stellar populations of the member galaxies. Most of these metals reside in the hot plasma which dominates the baryon content of clusters. This makes them excellent laboratories for the study of the nucleosynthesis and chemical enrichment history of the Universe. Here we review the history, current possibilities and limitations of the abundance studies, and the present observational status of X-ray measurements of the chemical composition of the intra-cluster medium. We summarise the latest progress in using the abundance patterns in clusters to put constraints on theoretical models of supernovae and we show how cluster abundances provide new insights into the star-formation history of the Universe.     

椭圆形扰流柱冷却通道流动与换热数值研究

采用数值计算方法对涡轮叶片椭圆形扰流柱排冷却通道的流动和换热进行了研究,得到了排列间距、迎角、椭圆长短轴之比等因素对冷却通道流动和换热性能的影响.在相同截面积和排列方式条件下,椭圆形扰流柱迎角为0°时,分析结果表明,椭圆形扰流柱冷却通道压力损失系数约为圆形扰流柱通道的51.7%,平均努塞尔数约为圆形扰流柱通道的83.75%;长短轴比为5/1.8时,压力损失系数仅为圆形扰流柱通道的(长短轴比等于3/3)28.1%～35.5%,平均努塞尔数为圆形扰流柱通道的71.1%～75.06%.      

面向在轨靠泊加注的管路力学分析与优化设计

面向在轨伸出式靠泊加注任务,针对对接过程中加注管路因同步外伸而产生附加力的问题,提出了一种偏置椭圆螺旋构型的加注管路。首先,推导了管路的轴向刚度和应力数学表达式,通过有限元仿真和实验校验了上述两个表达式的准确性。之后,将偏置椭圆螺旋管路与其他三种适用管路在同一设计空间下分别进行了基于最小轴向刚度的构型优化设计,得到了上述四种管路各自的最优构型与最小附加力,形成了该类在轨加注螺旋管路的完整设计方法。与仿真和实验结果对比,所推导的管路轴向刚度与应力数学表达式的相对误差均小于5%,可用于该类管路的设计分析。与无偏圆螺旋管路相比,所提出的偏置椭圆螺旋管路将靠泊加注对接过程中的管路附加力降低了约83.5%,更适用于在轨靠泊加注任务。