排序方式: 共有16条查询结果,搜索用时 15 毫秒
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涡轮叶栅端壁区流动的实验研究 总被引:1,自引:0,他引:1
本文在大尺寸低速开式叶栅传热风洞中对一种高压涡轮导向叶栅中的流场进行了实验研究。采用五孔针对5个雷诺数下的叶栅端壁区三维流场进行了测量,并用线簇和小球浮动法对5个工况的流动进行了流场显示。实验结果表明:马蹄涡压力面分支在向吸力面运动的过程中,破坏了来流附面层的结构,在马蹄涡压力面分支之后,叶栅通道中产生了一个新的从压力面到吸力面的新附面层,新附面层的厚度小于来流附面层厚度;三维流动区约占叶栅通道的40%;雷诺数的增大将增强端壁区的三维流动。从流场显示图片可以观测叶片吸力面靠近端壁的角涡形成与发展,以及吸力面上的三角形区域;流场显示的通道涡大小与流场测量结果吻合。本文的实验结果有助于分析端壁表面和叶片表面换热特性的形成机理。 相似文献
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背景对目标红外辐射测量影响的实验研究 总被引:2,自引:0,他引:2
在排气引射红外抑制系统的实验研究中, 通过对目标背景的各种处理方法、实验对比及分析, 了解背景对目标红外辐射特性测量的影响规律。实验结果表明:在大背景小目标情况下, 必须十分注意对背景进行遮挡和冷却处理。在选择遮挡材料时, 如果被遮挡部位处于高温部件的直接辐射场中, 则应选用表面发射率高的板材, 否则应选用高反射板材。遮挡板的定向应使其板面垂线与探测器轴线有较大夹角。 相似文献
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对于高精度测量和导航,GPS载波相位整周模糊度的快速求解仍然是一个难点,尤其对于单频接收机。本文提出一种动态快速求解整周模糊度的方法,其基本思想先对系数阵进行QR分解,然后通过矩阵变换使模糊度参数和位置参数分离,从而降低矩阵的维数,满足实时动态求解的要求,最后应用LAMBDA方法搜索模糊度。为验证该算法,我们用单频GPS接收机进行了两种实验(静态和动态),利用本文方法解算,静态误差小于1.5cm,动态误差小于4cm。实验结果表明:对于动态用户,该方法是快速和有效的。该方法可应用于高精度的导航和定位。 相似文献
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B. Nikutowski R. Brunner Ch. Erhardt St. Knecht G. Schmidtke 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
In the field of terrestrial climatology the continuous monitoring of the solar irradiance with highest possible accuracy is an important goal. SolACES as a part of the ESA mission SOLAR on the ISS is measuring the short-wavelength solar EUV irradiance from 16–150 nm. This data will be made available to the scientific community to investigate the impact of the solar irradiance variability on the Earth’s climate as well as the thermospheric/ionospheric interactions that are pursued in the TIGER program. Since the successful launch with the shuttle mission STS-122 on February 7th, 2008, SolACES initially recorded the low EUV irradiance during the extended solar activity minimum. Thereafter it has been observing the EUV irradiance during the increasing solar activity with enhanced intensity and changing spectral composition. SolACES consists of three grazing incidence planar grating spectrometers. In addition there are two three-signal ionisation chambers, each with exchangeable band-pass filters to determine the absolute EUV fluxes repeatedly during the mission. One important problem of space-borne instrumentation recording the solar EUV irradiance is the degradation of the spectrometer sensitivity. The two double ionisation chambers of SolACES, which could be re-filled with three different gases for each recording, allow the recalibration of the efficiencies of the three SolACES spectrometers from time to time. 相似文献
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C.L. Stokely E.G. Stansbery R.M. Goldstein 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
The continual monitoring of the low Earth orbit (LEO) debris environment using highly sensitive radars is essential for an accurate characterization of these dynamic populations. Debris populations are continually evolving since there are new debris sources, previously unrecognized debris sources, and debris loss mechanisms that are dependent on the dynamic space environment. Such radar data are used to supplement, update, and validate existing orbital debris models. NASA has been utilizing radar observations of the debris environment for over a decade from three complementary radars: the NASA JPL Goldstone radar, the MIT Lincoln Laboratory (MIT/LL) Long Range Imaging Radar (known as the Haystack radar), and the MIT/LL Haystack Auxiliary radar (HAX). All of these systems are highly sensitive radars that operate in a fixed staring mode to statistically sample orbital debris in the LEO environment. Each of these radars is ideally suited to measure debris within a specific size region. The Goldstone radar generally observes objects with sizes from 2 mm to 1 cm. The Haystack radar generally measures from 5 mm to several meters. The HAX radar generally measures from 2 cm to several meters. These overlapping size regions allow a continuous measurement of cumulative debris flux versus diameter from 2 mm to several meters for a given altitude window. This is demonstrated for all three radars by comparing the debris flux versus diameter over 200 km altitude windows for 3 nonconsecutive years from 1998 to 2003. These years correspond to periods before, during, and after the peak of the last solar cycle. Comparing the year to year flux from Haystack for each of these altitude regions indicate statistically significant changes in subsets of the debris populations. Potential causes of these changes are discussed. These analysis results include error bars that represent statistical sampling errors. 相似文献
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