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551.
激波速度测量是激波管和激波风洞运行状态的一个重要参数,压电传感器或光学方法测速系统成本高,而传统电离探针在激波马赫数较低、波后温度达不到空气电离程度的情况下无法满足实验要求。提出了一种使用同轴热电偶作为测速探针来测激波速度的方法,弥补了电离探针在激波马赫数较低时的不足。介绍了同轴热电偶探针测速原理,并设计了测量激波速度的系统电路。通过信号放大电路锁定激波冲激信号,触发脉冲信号发生电路,实现了一种单通道、多测点的激波风洞测速系统。分别开展以温度与热流为触发信号的风洞实验,结果表明只有使用热流信号才能满足激波测速的时间要求。 相似文献
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553.
使用面元法气动分析软件VSAERO对机翼与翼梢小翼组合体模型进行数值模拟,并采用Steve Smith提出的诱导阻力优化方法对翼梢小翼的定位进行优化设计。结果表明,能够有效地预测出翼梢小翼的最优定位,在翼梢小翼优化设计中具有很好的适用性。 相似文献
554.
Y12─Ⅱ型飞机结冰对其飞行特性影响的试飞研究 总被引:1,自引:0,他引:1
以Y12─Ⅱ型飞机防冰系统适航验证试飞为例,就确定飞机结冰部位与防护方法,结冰对飞机飞行性能和操稳特性的影响,带冰着陆的可能性及其安全措施等问题进行了分析和讨论。通过飞行试验,初步检查出飞机结冰造成飞机飞行性能的损失和操稳特性的降低。仅在新机研制中,为防冰系统适航性验证工作提供参考。 相似文献
555.
本文给出M_∞=7.8和6.72,Re=3.5×10 ̄7/m和5.4×10 ̄7/m气流绕迎角为20°、30°和35°尖前缘翼运动时,平板锥型干扰区的壁面压力和热流率分布。结果表明:(1)平板锥型干扰区的特征几何尺度与无粘激波角β_0和翼迎角α相关,而壁面压力和热流率的峰值与法向马赫数M_n相关。(2)翼面压力和热流率分布由于受拐角涡影响,前者在翼根部呈波谷状,而后者呈波峰状,影响尺度与翼前缘处来流边界层厚度有关。 相似文献
556.
Ueno K. Itanami T. Kumazawa H. Ohtomo I. 《IEEE transactions on aerospace and electronic systems》1995,31(2):600-607
Feasibility studies on a multiband communication satellite antenna system and the key technologies involved in devising this system are described. The proposed multiband communication satellite utilizes four frequency bands: Ka (30/20 GHz), Ku (14/12 GHz), C (6/4 GHz), and S (2.6/2.5 GHz). It has six beam configurations, three multibeam and three shaped-beam. The following key technologies are presented: (1) a low-loss frequency selective subreflector (FSR) for compact feeds, (2) a low-loss and broadband frequency selective surface (FSS), and (3) a highly accurate and reliable mesh reflector 相似文献
557.
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559.
Alexeev Igor I. Belenkaya Elena S. Bobrovnikov Sergey Yu. Kalegaev Vladimir V. 《Space Science Reviews》2003,107(1-2):7-26
A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological
conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component
normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the
solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented.
In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition
of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of
the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and
the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the
magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe
the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux
structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the
observational data for September 24–26, 1998 magnetic storm (Dst
min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
560.
Frey H.U. Mende S.B. Immel T.J. Gérard J.-C. Hubert B. Habraken S. Spann J. Gladstone G.R. Bisikalo D.V. Shematovich V.I. 《Space Science Reviews》2003,109(1-4):255-283
Direct imaging of the magnetosphere by instruments on the IMAGE spacecraft is supplemented by simultaneous observations of the global aurora in three far ultraviolet (FUV) wavelength bands. The purpose of the multi-wavelength imaging is to study the global auroral particle and energy input from the magnetosphere into the atmosphere. This paper describes the method for quantitative interpretation of FUV measurements. The Wide-Band Imaging Camera (WIC) provides broad band ultraviolet images of the aurora with maximum spatial resolution by imaging the nitrogen lines and bands between 140 and 180 nm wavelength. The Spectrographic Imager (SI), a dual wavelength monochromatic instrument, images both Doppler-shifted Lyman-α emissions produced by precipitating protons, in the SI-12 channel and OI 135.6 nm emissions in the SI-13 channel. From the SI-12 Doppler shifted Lyman-α images it is possible to obtain the precipitating proton flux provided assumptions are made regarding the mean energy of the protons. Knowledge of the proton (flux and energy) component allows the calculation of the contribution produced by protons in the WIC and SI-13 instruments. Comparison of the corrected WIC and SI-13 signals provides a measure of the electron mean energy, which can then be used to determine the electron energy flux. To accomplish this, reliable emission modeling and instrument calibrations are required. In-flight calibration using early-type stars was used to validate the pre-flight laboratory calibrations and determine long-term trends in sensitivity. In general, very reasonable agreement is found between in-situ measurements and remote quantitative determinations. 相似文献