Bolometric luminosities and brightness temperatures of BL Lac Objects and FR I radio galaxies

To understand the connection among the subclasses of BL Lac Objects, FR I radio galaxies and Flat spectrum radio quasars (FSRQs), here the correlations of the bolometric luminosities with redshifts and brightness temperatures of these objects are studied. The bolometric luminosities vary linearly with redshifts, but few objects are scattered at high redshift. The bolometric luminosity versus brightness temperature distribution shows a correlation between these two components, except a few scattered objects, mostly RBLs. The bolometric luminosities and brightness temperatures of FR I radio galaxies with low redshift (<0.1) and low spectral index (α_rx < 0.75) are comparable to those of XBLs and those characteristics of FR I radio galaxies, with relatively high redshift (>0.2) and high spectral index, can be comparable with RBLs with low redshift (z < 0.5) and low bolometric luminosity. Those scattered RBLs with high redshifts (z > 0.5) are believed to be in complex environment with companion galaxies, most of these RBLs are still unresolved. The bolometric luminosity and brightness temperature of these scattered RBLs are comparable to those of quasars. The FSRQs are at high redshifts and bolometric luminosities and the brightness temperatures are also high relative to BL Lac Objects. These results support the FRI/BL Lac unification scheme. It suggests that, the FR I radio galaxies may be the parent populations of the BL Lac Objects, but it needs more investigation to confirm the unification of FR I radio galaxies, XBLs and RBLs.     

镍基单晶合金蠕变细观结构演化及表征模拟

分析了NASAIR100在高温下不同应力和温度的蠕变及细观结构演化的异同,得到了材料4个主要的细观结构演化参数及其与蠕变的对应关系,在筏化模型的基础上建立了计及沉淀相筏化过程中厚度和基体通道宽度变化的细观结构演化模型,得到材料沉淀相和基体的细观演化过程及蠕变.结合试验结果,给出了不同细观演化方式对蠕变曲线的影响.在高温下同时考虑基体和沉淀相的4个细观参数变化可以使模型更贴近细观实际,并能较好地模拟材料在不同应力和温度下的蠕变.      

船用惯导系统的发展综述

从1852年傅科提出陀螺仪的概念到今天,陀螺技术走过了158年的历史。船用惯导设备也经历了从陀螺罗经到平台惯导再到激光捷联惯导系统的逐步演化的过程。本文综述了船用惯导设备的发展历程,总结了发展特点,为我国船用惯导系统的进一步发展提供了一些启示。     

TC11钛合金焊接接头低周疲劳分形损伤演化研究

基于损伤力学和分形理论,在金属材料疲劳断口的形貌特征具有统计自相似性的基础上建立了表征焊接接头断口损伤的面分形损伤演化模型.利用TC11合金低周疲劳试验后所得到的断口测得其面分维数,结合试验数据拟合获得该材料损伤演化方程参数;从而建立了TC11合金焊接接头三级载荷下的疲劳损伤演化方程;同时将该模型与基于断口表面裂纹扩展的线分形损伤演化模型加以比较.      

The Milky Way 3-Helium Abundance

We are making precise determinations of the abundance of the light isotope of helium, ³He. The ³He abundance in Milky Way sources impacts stellar evolution, chemical evolution, and cosmology. The abundance of ³He is derived from measurements of the hyperfine transition of ³He⁺ which has a rest wavelength of 3.46 cm (8.665 GHz). As with all the light elements, the present interstellar ³He abundance results from a combination of Big Bang Nucleosynthesis (BBNS) and stellar nucleosynthesis. We are measuring the ³He abundance in Milky Way H ii regions and planetary nebulae (PNe). The source sample is currently comprised of 60 H ii regions and 12 PNe. H ii regions are examples of zero-age objects that are young relative to the age of the Galaxy. Therefore their abundances chronicle the results of billions of years of Galactic chemical evolution. PNe probe material that has been ejected from low-mass (M≤ 2M _⊙) to intermediate-mass (M∼2–5M _⊙) stars to be further processed by future stellar generations. Because the Milky Way ISM is optically thin at centimeter wavelengths, our source sample probes a larger volume of the Galactic disk than does any other light element tracer of Galactic chemical evolution. The sources in our sample possess a wide range of physical properties (including object type, size, temperature, excitation, etc.). The ³He abundances we derive have led to what has been called “The ³He Problem”.     

失速团动态演变特性试验

对一台单级低速轴流压气机进行了节流特性试验,通过周向布置动态压力传感器测得了节流过程的动态压力信号,结合时域、频域及极坐标可视化的分析方法,研究了节流过程的失速团动态演变特性.结果表明:失速先兆类型为模态波失速先兆,其传播频率约为40%转子转动频率;压气机进入失速初期349.5r时周向形成两个失速团,360r时两个失速团合并为单个失速团,压气机进入深度失速时单个失速团重新分裂并在410r时稳定为两个失速团;压气机退出失速的过程中,665r时两个失速团重新合并为单个失速团,674.5r时压气机退出失速.      

Microstructure evolution and mechanical anisotropy of M50 steel ball bearing rings during multi-stage hot forging

This study aimed to explore the evolution of flow lines and microstructures of M50-steel bearing ring and the anisotropy of its tensile mechanical properties after Multi-Stage Hot Forging (MSHF) and subsequent spheroidizing annealing (MSHFA). To this end, the present study mainly employed stereo microscopy, Optical Metallurgical Microscopy (OMM), Scanning Electron Microscopy (SEM), and Electron Backscatter Diffraction (EBSD) to characterize and analyze the workpiece at each processing stage of MSHF while performing microhardness measurement and uniaxial tensile experiment to test and analyze the mechanical properties of the workpiece. Macro-structure observation showed that the simulation results of flow lines at each stage were consistent with the experimental results. Microscopic observation showed that, after MSHF, deformation gradually became less significant along the outward radial direction of the bearing ring. After MSHFA, the microstructures of the bearing ring became uniform, whereas primary carbides did not dissolve. The mechanical properties were better in the axial direction (AD) than in the radial (RD) and circumferential directions (CD) after MSHF due to the smaller grain width. After MSHFA, the mechanical properties in the ADs and CDs were better than those in the RDs, which was due to the large cross-sectional area of carbides along the flow-line direction.     

空间物体解体碎片云的长期演化建模与分析

空间碎片云由空间物体解体产生的大量空间碎片组成,由于其相对集中地分布在有限的空间内,将会对临近航天器产生较大的碰撞威胁。为了分析解体碎片云长期分布特点,文章首先利用数值积分方法对空间碎片云短期分布规律进行了研究;在此基础上,针对处于环状分布的碎片云,根据碎片所在的轨道高度和具有的面质比值,将碎片划分到不同分组,以每个组作为研究对象,建立了描述碎片云在大气阻力作用下的解析演化模型。模型避免了对单个解体碎片的运动状态进行积分,可大大降低对计算资源和计算时间的需求。考虑在高度为1422km 圆轨道上运行的物体,解体产生了1780个碎片,利用解析演化模型得到碎片云未来50年内的演化分布状态。数值结果表明,碎片云的峰值密度在解体物体轨道高度附近,并在大气阻力作用下向更大高度区间内扩散;较低高度区间内碎片密度具有先增加,然后在大气阻力作用下不断减少的特点。     

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.