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。     

布撒器气动特性分析

为了确定布撒器的气动特性 ,在中国空气动力研究与发展中心高速所 0 .6m× 0 .6m风洞中进行了 1 :7缩比模型常规测力试验。实验结果表明 :在实验攻角下 ,布撒器横向稳定 ;在小攻角下布撒器呈方向静安定 ;如果俯仰舵偏为可用偏转角度的一半 ,布撒器纵向最大配平攻角约为 4°～ 6°之间 ;如果采用全部舵偏 ,布撒器在所有实验攻角下均可配平。     

Highlights of the Brazilian Solar Spectroscope

The digital, decimetric (950–2500 MHz) Brazilian Solar Spectroscope (BSS, Sawant, H.S., Subramanian, K.R., Faria, C., et al. Brazilian Solar Spectroscope (BSS). Solar Phys. 200, 167–176, 2001) with high time (10–1000 ms) and frequency (1–10 MHz) resolution is in regular operation since April, 1998, at the National Space Research Institute (INPE) at São José dos Campos, Brazil. The BSS has now been upgraded with a new digital data acquisition and data processing system. The new version of the BSS has improved the observational possibilities with the capability to record up to 200 frequency channels available in the selectable frequency range 950–2500 MHz. The GPS receiver permits the acquisition of data with time accuracy in the order of 0.1 ms. The software system of the BSS is composed by two distinct modules: the first, data acquisition system provides a flexible Graphical User Interface (GUI) that allows one to choose the observational parameters. The second module is the real time visualization system that permits real time visualization of the observed dynamic spectrum and additionally allows procedures for visualization and preliminary analysis of the recorded solar spectra. Using the new visualization system, we have realized two new types of dm-radio fine structures: narrow band type III bursts with positive as well as negative group frequency drift and dots emissions arranged in zebra-like and fiber-like chains. Furthermore, we have found flare generated fast wave trains according to their tadpole signature in wavelet power spectra for a decimetric type IV radio event (June 6, 2000 flare).     

基于传动误差设计的弧齿锥齿轮啮合分析

 提出了基于传动误差设计的弧齿锥齿轮啮合质量控制的新概念。首先分析了传动误差所反映的弧齿锥齿轮传动的动态特性、强度性能等众多信息,包括设计重合度、实际重合度、振动激励、边缘接触、载荷齿间分配和齿面印痕相对于误差的敏感性。在此基础上,提出了高重合度传动误差曲线的设计,通过齿面接触路径方向的倾斜,重合度能够高至 2.0～ 3.0,有效地改善了齿轮动态特性,提高了强度。进一步又提出了几何传动误差曲线幅值的设计,结合承载传动误差,使齿轮在不同载荷条件下既能具有高的重合度,又保证了相对低的误差敏感性。其后提出的四阶传动误差曲线的设计,除上述优点外,还改进了齿轮的轻载振动和噪声。最后论述了基于传动误差设计的弧齿锥齿轮的相应制造方法。该研究为高性能弧齿锥齿轮的开发开辟了途径。     

三维离散矢量场中的涡核识别

基于临界点理论，使用特征矢量方法在三维离散矢量场中进行了涡核寻找的研究。该方法能够快速准确地找到三维矢量场中的涡核，为CFD工作提供了一个有效的数值分析工具，搜寻结果与其它方法（如流线法等）进行了比较。     

美国航空推进系统关键技术

在美国的国防关键技术计划中，航空推进技术受到重视。通过对美国国家级计划－－高性能涡轮发动机综合技术计划、脉冲式爆震波产生推力的新概念发动机计划、燃烧室内气流过渡为超声速的冲压发动机计划的研究，对美国选择推进系统的理由作了分析，并对各国在航空推进系统的研究和发展工作进行了评估。可以看出，日本、德国继美、英、法、俄后在航空航天的推进系统方面已完成了一系列的研究。日本斥巨资建立发动机模拟高空试验台。最后详细列出了燃气涡轮发动机，其它航空动力和燃料三类中的10项关键技术。     

Magnetic Flux Ropes in the Martian Atmosphere: Global Characteristics

We report observations of magnetic fields amplitude, which consist of a series of individual spikes in the Martian atmosphere. A minimum variance analysis shows that these spikes form twisted cylindrical filaments. These small diameter magnetic filaments are commonly called magnetic flux ropes. We examine the global characteristics of magnetic flux ropes, which are observed on 5% of the elliptical orbits of Mars Global Surveyor. Flux ropes are more often observed in Venus' atmosphere (70% of the orbits). In this paper we report some of the global characteristics of the flux ropes identified in the Martian atmosphere. No flux ropes are observed in the southern hemisphere of Mars. Most of them occur at high solar zenith angles, close to the terminator plane, and at high latitude with altitudes below 400 km. The orientation of the flux ropes appears random while in the case of Venus the orientation is more horizontal near the terminator for altitudes greater than 200 km. We have identified fewer flux ropes for SZA between 40 to 60 deg and for SZA lower than 20 deg, like in the case of Venus (Elphic and Russell, 1983b). Statistically, Mars' ionosphere with SZA range between 40^circ to 60^circ is less magnetized than near the subsolar point. As the Martian ionosphere is quite often magnetized by the magnetic components of the crustal field, this crustal magnetic field seems to inhibit the flux ropes formation in the southern hemisphere. However, some orbits without crustal magnetic field, called magnetic cavities, were observed without flux ropes. So the flux ropes formation process seems to be uppressed by another factor, like the solar wind dynamic pressure for Venus (Krymskii and Breus, 1988).     

Bow Shock and Upstream Phenomena at Mars

Mars Global Surveyor is the sixth spacecraft to return measurements of the Martian bow shock. The earlier missions were Mariner 4 (1964), Mars 2 and 3 (1972), Mars 5 (1975) and Phobos 2 (1989) (see reviews by Gringauz, 1981; Slavin and Holzer, 1982; Russell, 1985; Vaisberg, 1992a,b; Zakharov, 1992). Previous investigations of planetary bow shocks have established that their position, shape and jump conditions are functions of the upstream flow parameters and the nature of the solar wind — planet interaction (Spreiter and Stahara, 1980; Slavin et al., 1983; Russell, 1985). At Mars, however, the exact nature of the solar wind interaction was elusive due to the lack of low altitude plasma and magnetic field measurements (e.g., Axford, 1991). In fact our knowledge of the nature of the interaction of Mars with the solar wind was incomplete until the arrival of MGS and the acquisition of close-in magnetic field data (Acuña et al., 1998). As detailed by a series of review papers in this monograph, the Mars Global Surveyor (MGS) mission has now shown that the Mars environment is very complex with strong, highly structured crustal magnetic remnants in the southern hemisphere, while the northern hemisphere experiences the direct impingement of solar wind plasma. This review paper first presents a survey of the observations on the Martian bow shock and the upstream phenomena in the light of results from all the missions to date. It also discusses the kinetic properties of the Martian bow shock compared to the predictions of simulations studies. Then it examines the current status of understanding of these phenomena, including the possible sources of upstream low-frequency waves and the interpretations of localized disturbances in the upstream solar wind around Mars. Finally, it briefly discusses the open issues and questions that require further study.     

Mars Crustal Magnetism

Mars lacks a detectable magnetic field of global scale, but boasts a rich spectrum of magnetic fields at smaller spatial scales attributed to the spatial variation of remanent magnetism in the crust. On average the Mars crust is 10 times more intensely magnetized than that of the Earth. It appears likely that the Mars crust acquired its remanence in the first few hundred million years of evolution when an active dynamo sustained an intense global field. An early dynamo era, ending in the Noachian, or earliest period of Mars chronology, would likely be driven by thermal convection in an early, hot, fluid core. If crustal remanence was acquired later in Mars history, a dynamo driven by chemical convection associated with the solidification of an inner core is likely. Thermal evolution models cannot yet distinguish between these two possibilities. The magnetic record contains a wealth of information on the thermal evolution of Mars and the Mars dynamo, but we have just begun to decipher its message.