流动控制技术在航空涡轮推进系统上的应用

介绍了主动流动控制在风扇／压气机、主燃烧室、涡轮和排气系统中的应用情况。阐明了流动控制在大幅度地提高发动机的性能、增加发动机的稳定性、减轻发动机的重量等方面的巨大潜力。同时指出分步实施流动控制的过程也就是应对其重大技术挑战的过程。     

Impact of Distance Determinations on Galactic Structure. I. Young and Intermediate-Age Tracers

Here we discuss impacts of distance determinations on the Galactic disk traced by relatively young objects. The Galactic disk, \(\sim40~\mbox{kpc}\) in diameter, is a cross-road of studies on the methods of measuring distances, interstellar extinction, evolution of galaxies, and other subjects of interest in astronomy. A proper treatment of interstellar extinction is, for example, crucial for estimating distances to stars in the disk outside the small range of the solar neighborhood. We’ll review the current status of relevant studies and discuss some new approaches to the extinction law. When the extinction law is reasonably constrained, distance indicators found in today and future surveys are telling us stellar distribution and more throughout the Galactic disk. Among several useful distance indicators, the focus of this review is Cepheids and open clusters (especially contact binaries in clusters). These tracers are particularly useful for addressing the metallicity gradient of the Galactic disk, an important feature for which comparison between observations and theoretical models can reveal the evolution of the disk.     

用Newton子迭代方法计算前飞旋翼粘性绕流

通过求解Navier-Stokes方程数值模拟了直升机旋翼前飞非定常流场，为了同时保证计算的时间精确性和计算效率，时间推进格式采用了双时间推进方法，在该方法中，子迭代过程由十分高效的LU-SSOR方法完成，且使子迭代过程成为Newton子迭代，空间上应用中心平均的有限体积法进行离散，为了模拟前飞桨时间的相对运动，网格布局采用了运动嵌套网格方法，应用本文方法对-悬停流场进行了数值计算，计算结果与实验吻合较好，尽管缺乏实验数据的验证，对-有升力前飞状态的数值模拟结果是可信的。     

利用微气囊扰动进行流动控制的数值模拟研究

探讨一种可以用来模拟“三角翼上分布微气囊，从而控制流动获得滚转力矩”的数值方法。为微型飞机的气动设计提供一种工具。研究的内容包括：考虑微气囊的三角翼网格生成、流场NS方程计算、微气囊不同布局对流动的扰动等。     

ZA27Ce合金组织形态对阻尼性能的影响

对铸态ZA2 7Ce合金进行固溶处理 ,获得单一均匀的固溶体后 ,分别进行 96℃ ,180℃和 2 5 0℃人工时效。采用悬挂弯曲共振法测量阻尼性能Q-1值 (阻尼本领 ) ,结果是 ,96℃人工时效后阻尼性能好于 180℃以及 2 5 0℃人工时效后的阻尼性能。利用SEM研究时效后微观组织 ,结果发现 ,96℃人工时效获得粒状组织 ,180℃以及2 5 0℃人工时效获得层片状组织。利用等轴晶界面滑动内耗机理分析认为 ,ZA2 7Ce合金粒状组织的阻尼性能好于层片状组织的阻尼性能     

Small-Scale Solar Magnetic Fields

As we resolve ever smaller structures in the solar atmosphere, it has become clear that magnetism is an important component of those small structures. Small-scale magnetism holds the key to many poorly understood facets of solar magnetism on all scales, such as the existence of a local dynamo, chromospheric heating, and flux emergence, to name a few. Here, we review our knowledge of small-scale photospheric fields, with particular emphasis on quiet-sun field, and discuss the implications of several results obtained recently using new instruments, as well as future prospects in this field of research.     

On the fundamental acoustic mode in variable area,low Mach number nozzles

We consider the propagation of sound in nozzles of substantially varying cross-section, taking into account reflections from the tapering walls and non-uniform convection by the axially accelerated or decelerated mean flow. Exact solutions of the acoustic equations are obtained for the simplest case of the fundamental longitudinal mode in quasi-one-dimensional, low Mach number nozzle flow. The effects of non-uniform mean flow on sound are demonstrated by comparing horns with nozzles, and 15 properties (stated in italics and labelled P1, P2 ... P15 in the text) are proved and discussed, viz. concerning (1) relations between acoustic pressure and velocity; (2) equipartition or biasing of kinetic and compression energies; (3) conservation or evolution of wave action; (4) existence of elementary or special solutions and (5) cut-off frequencies, and amplitude and phase laws. We conclude with a simple formula for the approximate calculation of the acoustic fields; the formula can be made more accurate by using a correction factor for amplitude and phase, which is plotted against area ratio for propagation upstream or downstream in diffusers and convergent nozzles.     

Analysis of total visual and CCD V-broadband observations of Comet C/1995 O1 (Hale-Bopp): 1995–2001

We developed a general method for determination of water production rates from groundbased visual observations and applied it to Comet Hale–Bopp. Our main objective is to extend the method to include total visual magnitude observations obtained with CCD detector and V filter in the analysis of total visual magnitudes. We compare the CCD V-broadband careful observations of Liller [Liller, W. Pre-perihelion CCD photometry of Comet 1995 O1 (Hale-Bopp). Planet. Space Sci. 45, 1505–1513, 1997; Liller, W. CCD photometry of Comet C/1995 O1 (Hale-Bopp): 1995–2000. Int. Comet Quart. 23(3), 93–97, 2001] with the total visual magnitude observations from experienced international observers found in the International Comet Quarterly (ICQ) archive. A data set of ∼400 CCD observations covering about the same 6 years time span of the ∼12,000 ICQ selected total visual magnitude observations were used in the analysis. A least-square method applied to the water production rates, yields power laws as a function of the heliocentric distances for the pre- and post-perihelion phases. The average dimension of the nucleus as well as its effective active area is determined and compared with values published in the literature.