某型发动机进气总压畸变试验稳态流场数值分析

进气总压畸变是影响发动机稳定性的上,对获得的大量流场数据进行了处理与分析,得出了畸变指数、总压周向不均匀度分量指数、低压区角度等多项技术参数,并且绘制出了周向压力分布图和流场畸变图谱.将这些技术参数和图谱与模拟板的目标图谱数据、风洞吹风试验数据及高空台试验推算结果进行了综合分析与对比,较完整地表述了发动机进口的流场品质.     

变唇口加板模拟总压畸变流场

采用变唇口加板或加杆的方法,模拟某飞机进气道出口截面不同型式的总压畸变流场。变唇口加板能模拟具有中心低压区的总压分布;变唇口加杆可模拟具有中心高压区且周向畸变较小的总压分布。采用圆弧切割法能较正确地模拟总压等值线形状。所模拟的稳态周向总压畸变指数(DC₆₀)、平均湍流度(T_u)和最大瞬时总压畸变指数(K_θmax或K_tmax)均能达到规定的精度要求。该方法不仅能模拟复杂的总压分布和稳态畸变指数;也能模拟动态畸变指数。     

扰流板进气总压畸变试验

在吊舱进气道进口安装扰流板进行试验,研究扰流板进气畸变的影响因素及总压畸变特征。试验得到了进气道出口若干马赫数下进气总压畸变的定量数据,研究了进气道出口压力分布和畸变指数随飞行马赫数、扰流板堵塞比、进气道出口马赫数的变化关系。试验结果表明：进气道出口对应点总压恢复系数随扰流板堵塞比和进气道出口马赫数的减小而增大,几乎不随飞行马赫数发生变化;受扰流板、飞行侧滑角以及发动机低压转子转向影响,进气道出口局部区域存在高压区,高压区域的大小和位置随飞行马赫数、扰流板堵塞比、进气道出口马赫数的变化而变化;各总压畸变指数随扰流板堵塞比和进气道出口马赫数增大而增大,飞行马赫数对畸变指数影响很小。同时,数值计算了不同飞行马赫数下进气道出口总压畸变特征及周向稳态畸变指数,与试验结果结论一致,验证了试验结果的可靠性,也证明了数值计算在总压畸变研究中的有效性。研究工作为进一步的空中逼喘试验奠定了基础。     

缩尺模拟板相关性研究

介绍了模拟板由小模型到大模型的研制过程，着重讨论了模拟板小模型与大模型在流场总压恢复系数、周向不均匀度、低压区范围等方面的相关性问题。研究结果表明由小模型到大模型的研制方案是正确可行的。     

模拟板全尺寸吹风试验技术

为了对某航空发动机流场畸变模拟板进行设计验证和修型，需要对其进行吹风试验，测取其在一定板后马赫数下的压 力分布。为此，通过进气和引射相结合的方式，在某试验设备上开展了模拟板全尺寸吹风试验，并进行了模拟板全尺寸畸变吹风 试验技术研究。针对模拟板板后马赫数计算方法、板后AIP稳态总压测点布局、板后测点小角度偏斜、板后测点轴向位置以及物 理/换算流量对畸变度的影响进行了试验。结果表明：在非回流区内板后马赫数采用总静压法进行计算的结果更接近真实值；板 后AIP稳态总压测点布局、测点轴向位置对畸变度测量有影响；板后测点小角度偏斜对畸变度测量基本无影响；综合压力畸变指 数随着换算流量的增大逐渐增大；在换算流量相同时，综合压力畸变指数不随物理流量的变化而变化。     

测点布局对航空发动机总压畸变指数的影响

为了阐明测点布局对航空发动机进气总压畸变测试结果的影响，利用旋转总压测量耙对5种畸变流场的稳态和动态总 压畸变成分进行了测试，计算了旋转总压测量耙位于不同位置时畸变流场的稳态周向总压畸变指数和动态总压畸变指数，分析了 不同测点布局下总压畸变指数计算结果的偏差。结果表明：测量耙/测点与畸变流场的相对周向位置对总压畸变指数计算结果的 准确性至关重要，对于所分析的5种畸变流场，增加测量耙/测点周向数目并不能使总压畸变指数计算结果的偏差单调减小，但可 降低其对测量耙/测点周向位置的敏感度。基于畸变区域周向分布设计稳态总压畸变测量耙的周向位置，组合使用不同相对半径 处测点对动态总压畸变进行监测，可提高总压畸变指数计算结果的准确性。     

变唇口型总压畸变流场的模拟技术

本文对变唇口型总压畸变流场模拟技术进行了试验研究。一方面总结分析了各种唇口几何参数对总压分布谱图和总压脉动紊流度的影响, 从而将这些一般的规律应用于特定总压分布谱图, 总压脉动紊流度及其畸变指数的模拟。另一方面, 对给定的二个不同类型的总压畸变流场进行模拟, 所模拟的稳态周向总压畸变指数, 平均总压脉动紊流度和最大瞬时畸变指数均能达到规定偏差的要求。      

进口畸变下非定常数值模拟进口边界数学模型

进口畸变下压气机内存在的不同空间和时间尺度的非定常流动之间的相互作用是进口畸变对压气机性能影响的重要流动机理.介绍了一种用于周向进口总压畸变下单转子通道内非定常数值模拟的进口边界简化模型,并基于该模型进行了三维非定常数值模拟.数值模拟结果显示了进口周向总压畸变的大尺度总压脉动和压气机转子通道非定常分离流场的相互作用过程.该模型为周向进口畸变的三维非定常数值模拟提出了一种简化方法.      

畸变模拟板的设计与试验研究

通过对模拟板的设计研究，提出了一种半经验、半数学的模拟方法。实例表明，该方法简单有效，较为满意地模拟了给定流场的总压恢复系统分布图形。按模拟方法初次制作的模拟板，经过数次的试验调整其畸变指数即可达标。此外，还介绍了试验的调整方法，该方法经试验证明是行之有效的。     

扰流板式畸变模拟装置的数值计算及人工神经网络建模

数值计算了用于某型空中试车台吊舱的扰流板式畸变模拟装置,应用总压恢复系数、周向畸变指数评价了该装置的畸变效果并与试验数据进行了对比分析,为后续发动机在空台上确定临界畸变指数及敏感系数提供了可用量值的参考.根据部分计算数据,建立了该扰流板式畸变模拟装置的人工神经网络模型,并预估了12个状态的畸变模拟效果,验证了该人工神经网络模型的有效性,为减少试验点数节省试验经费提供了有效的途径.     

NETEX UWB test results

The goal of the Defense Advanced Research Projects Agency's (DARPA) Networking in Extreme Environments (NETEX) program is to create a wireless networking technology for the military user that enables robust connectivity in harsh environments and support its integration into new and emerging sensor and communication systems. Phase 1, resulted in a thorough understanding of the effects of ultra wide band (UWB) system operation on existing military spectrum users based on modeling, simulation, and measurements. In order to accomplish this task, the DARPA Advanced Technology Office (ATO) procured a set of UWB emitters and broadband antennas to use as interference sources and contracted with the Naval Air Warfare Center Aircraft Division (NAWC AD) Electromagnetic Environmental Effects (E/sup 3/) Division to provide candidate victim systems from the existing (legacy) US naval aircraft and shipboard inventory for testing. Testing was conducted on seventeen legacy systems during October 2002 through March 2003. The purpose of this paper is to provide a brief overview of the results of these tests. This paper will provide a brief discussion of the UWB emissions as described by the US Federal Communications Commission (FCC) and describe the generic UWB emitter used for these tests. It will then provide a discussion of the results as they apply to the purpose of the NETEX program.     

Recent results from COMPTEL

The COMPTEL telescope aboard the Compton Gamma Ray Observatory has put MeV -rays into the midst of astronomy. Among recent highlights are the discovery of intense MeV emission from blazar-type active galactic nuclei, the surprising non-detection of any Seyfert galaxy at MeV energies, the first image of the Milky Way in the light of the²⁶Al line at 1.809 MeV (possibly including a detection of the Vela supernova remnant), the discovery of 3–7 MeV emission from the Orion complex, which can be identified with nuclear interaction lines of¹²C and¹⁶O at 4.44 and 6.13 MeV, the detection of the⁴⁴Ti line at 1.15 MeV from the supernova remnant Cas A, and the first results on the spectrum and propagation of low-energy (1–100 MeV) cosmic-ray electrons.also Leiden Observatory     

关于CFD计算结果的不确定度问题

本文研究CFD的准确度和不确定度问题,希望给出一种说法,以此说明CFD的可用性、面临的现状和问题,并进一步研究提高CFD准确度的措施.     

Lunar photography: Techniques and results

Conclusion The lunar photography missions have included flyby, impacter, lander, and orbiter spacecrafts. These missions have provided photographs of the far side of the moon and a ten-fold increase in frontside resolution plus higher resolution of selected frontside areas. The resolutions which have been achieved vary from 1 m for the Lunar Orbiter to 1/2 m for the impacting Ranger to millimeters for Luna-IX and the Surveyors. The return from these missions have resolved much of the mystery surrounding the moon.The prime objective of the U.S. photographic missions has been the support of the Apollo-manned lunar landing program. The Ranger program, the Surveyor program, and the Lunar Orbiter program provided a logical progression in the utilization of a developing space exploration technology. These programs have provided the required information and have confirmed that the Apollo landing vehicle design is compatible with the conditions to be experienced on selected areas of the lunar surface.The future manned landing missions can be expected to provide additional lunar photography. Since the astronauts can be more selective in their photography, even more outstanding and informative results should be achieved. The addition of movies and even live television coverage will permit earth-based man to share more directly in the manned exploration of the moon.The unmanned photographic exploration of the moon has provided much of the technology required for similar missions to the planets. The U.S. Mariner-IV was the first successful mission to obtain close-up photographs of the planet Mars. It can be expected that both the U.S.A. and Russia will try for further photographic successes in the exploration of our solar system.This paper presents the results of one phase of research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under Contract No. NAS 7-100, sponsored by the National Aeronautics and Space Administration.     

Orion-2: First scientific results

The ultraviolet spectral images of thousands of faint stars, up to the 13th mag., in the wavelength region of 2000–5000 Å are obtained by means of the space astrophysical observatory Orion-2 aboard the spaceship Soyuz-13. These spectrograms were designed generally for an investigation of the continuous spectra of the stars in ultraviolet. The processing and measurement of part of the material available confirm the expectations for the solution of a large number of problems concerning the physics of stars and stellar atmospheres. Some of the results obtained are included in the present review. Particularly, the observed distribution of continuous energy in the ultraviolet of normal hot stars is in line, according to Orion-2 data, with theoretical prediction; the existence of a new type of high temperature (> 20000K) and low absolute luminosity stars is noticed; the blocking effect of the ultraviolet absorption lines expected for the A-type stars is confirmed; a number of empirical regularities concerning the behaviour of the ultraviolet doublet of ionized magnesium, 2800 Mg ii, in the stellar spectra are derived; the chromosphere in cold stars is detected; the role of a multiplet of ionized titanium, 3080 Ti ii, in stellar spectra is revealed; probably an abnormal silicon-rich stellar envelope around a Be-type star is discovered; a new method for the spectral classification of the stars by their ultraviolet spectral images is developed; a range of interesting facts relating to the structure of the ultraviolet spectra of middle type stars (F-K) come to the fore; an exceptional ultraviolet spectrogram for the planetary nebula II 2149 and its nuclei is obtained; the blocking effect of emission lines in the spectrum of the B-type emission and normal O-type stars has been detected; a remarkably faint (12^itm.6) and high temperature star (No. 1) of strange spectral structure has been discovered.     

Attitude determination with GPS: experimental results

An approach to global positioning system (GPS) attitude determination and the results of an experimental evaluation are presented. The most outstanding features of the method are the fundamental observable used for attitude calculation, the triple difference, and the introduction of a new parameter, the differential dilution of precision (DDOP), which relates the GPS satellite geometry to the GPS accuracy when measuring angular magnitudes. The experiment used two commercial off-the-shelf GPS C/A code receivers delivering integrated Doppler measurements. The algorithm is robust with respect to phase cycle slips and does not require solving the usual integer ambiguity of the measurements. The preliminary results show that absolute attitude determination requires a calibration of the baseline and that the relative attitude accuracy is on the order of 0.1° or 2 mrads for the case of a 2-m-long baseline     

Initial ISEE magnetometer results: magnetopause observations

The magnetic field profiles across the magnetopause obtained by the ISEE-1 and -2 spacecraft separated by only a few hundred kilometers are examined for four passes. During one of these passes the magnetosheath field was northward, during one it was slightly southward, and in two it was strongly southward. The velocity of the magnetopause is found to be highly irregular ranging from 4 to over 40 km s^-1 and varying in less time than it takes for a spacecraft to cross the boundary. Thicknesses ranged from 500 to over 1000 km.Clear evidence for reconnection is found in the data when the magnetosheath field is southward. However, this evidence is not in the form of classic rotational discontinuity signatures. Rather, it is in the form of flux transfer events, in which reconnection starts and stops in a matter of minutes or less, resulting in the ripping off of flux tubes from the magnetosphere. Evidence for flux transfer events can be found both in the magnetosheath and the outer magnetosphere due to their alteration of the boundary normal. In particular, their presence at the time of magnetopause crossings invalidates the usual 2-dimensional analysis of magnetopause structure. Not only are these flux transfer events probably the dominant means of reconnection on the magnetopause, but they may also serve as an important source of magnetopause oscillations, and hence of pulsations in the outer magnetosphere. On two days the flux transfer rate was estimated to be of the order of 2 × 10¹² Maxwells per second by the flux transfer events detected at ISEE. Events not detectable at ISEE and continued reconnection after passage of an FTE past ISEE could have resulted in an even greater reconnection rate at these times.