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81.
小发动机燃气流火焰温度测量 总被引：1，自引：0，他引：1
小发动机是在高温条件(≈1800℃)下进行头部防热材料模拟试验的设备,是为解决导弹弹头再入大气层时的防热问题而研制的。本文叙述了用光学法测量小发动机燃气流火焰温度、燃气流中模型前端的激波温度及不同材料的模型表面温度。实验表明:不同材料的模型,其表面温度不同。文中对测温误差进行了初步分析。 相似文献
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本文在稀颗粒群双流体简化模型下,采用算子分裂技术,综合应用高分辨率ＧＲＰ格式,全二阶精度的ＦＣＴ格式及预估校正格式,取三种不同粒相固壁边界条件,数值模拟了粉尘气体激波在刚性固壁上的正反射,确证了由理想平衡混合气体分析所预示的三类激波反射结构,给出了非平衡反射时波后流场的松弛特性,并评价了不同的粒相固壁边界条件假定的适用性。 相似文献
84.
Laves相Nb-Cr合金的真空烧结 总被引：1，自引：0，他引：1
研究了真空烧结参数及机械合金化对Laves相Nb-Cr合金致密度的影响,结果表明球磨后粉末烧结试样的致密度增加率是未球磨粉末烧结试样的3~5倍;当烧结温度增加、烧结时间延长,Laves相NbCr2的合成更为充分,试样致密度增加。 相似文献
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大面积表面温度测量技术在风洞测温领域中具有重要意义。为满足更高表面温度的测量需求,亟待开展新型测温技术及温度传感材料的研发。基于稀土离子的热耦合能级荧光强度比进行温度测量是一种新型测温技术。本文合成了一种温敏发光材料（YAG:Dy）,研究了50～1000 ℃范围内稀土Dy3+离子的一对热耦合能级（4F9/2→6H15/2,4I15/2→6H15/2）的跃迁发光强度比与温度的对应关系。基于该材料,本文开展了荧光强度比测温与红外测温仪测温的对比实验,实验结果表明：两者的测量结果有很高的吻合度,证明该温敏发光材料（YAG:Dy）可用于50～1000 ℃范围内的温度测量。 相似文献
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提出了利用高焓气体自发光作为高超声速流场显示的方法,介绍了在使用高焓运行的激波风洞中,对二维模型的高超声速绕流流场使用此种方法的初步结果,可观察到二维棱形柱的尾流和马赫波的相交.结果表明此种方法不需外加光源,对于结构限制无法设置透明部件的模型,无疑是简单可行的. 相似文献
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飞船、宇航探测器、航天飞机等复杂外形航天器给气体动力学,包括稀薄气体动力学提出了新的要求。本文简要介绍了为计算过渡领域中气动力与热而发展的基于位置元概念的DSMC方法的通用算法。该方法解决了计算物面通量量的技术难点并已用于模拟圆球、飞船、类航天飞机的绕流。正在进行的航天实践,如麦哲伦飞船对金星的探测、行星大气中的气动制动、伽利略飞船的木星之行、尾屏蔽在太空中获得高真空的实验等等提出了新的气动力问题,稀薄气体动力学和DSMC方法是有力的工具。 相似文献
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S. M. Krimigis D. G. Mitchell D. C. Hamilton S. Livi J. Dandouras S. Jaskulek T. P. Armstrong J. D. Boldt A. F. Cheng G. Gloeckler J. R. Hayes K. C. Hsieh W.-H. Ip E. P. Keath E. Kirsch N. Krupp L. J. Lanzerotti R. Lundgren B. H. Mauk R. W. McEntire E. C. Roelof C. E. Schlemm B. E. Tossman B. Wilken D. J. Williams 《Space Science Reviews》2004,114(1-4):233-329
The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20RS (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm2 sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm2 sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm2 sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm2 sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 RS every 2–3 h (every ∼10 min from ∼20 RS). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date. 相似文献
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