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11.
气泡和液滴在上升或下降时大变形的数值模拟 总被引:4,自引:0,他引:4
本文在考虑界面张力的条件下用涡片方法导出了二维无粘气泡和液滴在另一种静止无粘流体中上升或下降时运动和变形的支配方程,提出了求解支配方程的数值方法,并在数值模拟的例子中研究了空气泡和煤油滴在水中上升时及水滴在煤油中下降时的变形规律,研究了数值模拟中界面张力对界面形状的影响,气泡上升的数值模拟结果与相应的试验结果基本一致。数值模拟结果表明本方法可正确模拟饣泡和液滴在上升或下降过程中的大变形,直到界面发 相似文献
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本文提出了一种由表面摩擦测量旋涡脱落频率的方法,阐述了其原理,给出了实验研究的结果,可作为涡街式流量计测量旋涡脱落频率的一种途径。 相似文献
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本文对平板附面层在有和没有涡流器情况下的传热性能进行了试验研究。测量了两种情况下的附面层速度分析和温度分布。结果表明,在涡流器排的近下游,传热性能有很大提高,附而层的速度分布有很大改变,壁面处的速度梯度大大增加,而温度梯度大大减少,原因是旋涡发生器产生的流向涡与附面层的相互作用。 相似文献
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栅格翼尾流中的发卡涡 总被引:1,自引:2,他引:1
介绍了在水漕中用氢气泡法显示的斜置蜂窝式栅格翼尾流流态 ,发现在中等迎角下 ,相交翼元的每个交叉处邻近壁面的尾流中 ,有伴随着壁面流动分离而周期性脱落的发卡涡 ,它们相互连接 ,形成“涡链”。还介绍了栅格翼尾流中发卡涡的主要流动特征 ,并对其产生的流动机理作了初步探讨。 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 20R
S (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 R
S every 2–3 h (every ∼10 min from ∼20 R
S). 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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亚,超声速旋涡流动特征的定性分析研究 总被引:2,自引:4,他引:2
本文研究了沿其轴向运动的亚声速和超声速旋涡的性状,指出两者完全不同。在加速区,于涡轴附近,亚声速旋涡的横截面流线即横截面上的速度场的向量线为由外向内转的稳定螺旋点形态,空间流线沿其轴向是收缩的,而超声速旋涡的横截面流线为由内向外转的不稳定螺旋点形态,空间流线沿其轴向是散开的。在减速区,两者的情况也恰好相反,此外,当旋涡由加速区过渡到减速区时,两者横截面流线方程在涡轴附近的Hopf分叉情况也不同,亚 相似文献
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本文利用自适应区域方法调节机翼后每个Trefftz平面上的计算域,使得尾涡对这个计算域边界的影响足够小,从而提高了计算的精度和时间。考虑到间断面的影响,在尾涡面上引入有旋项对流场进行计算。椭圆载荷机翼计算表明本文计算结果与经典Betz理论一致。用本文方法对某轰炸机进行了计算,计算结果已用于预计其实际飞行的尾涡面。 相似文献
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本文将一台TSI 9100-7型两分量激光测速仪改进为可测三个速度分量的LDV系统,并用于测量风洞中椭球体模型、双三角翼模型大迎角下的复杂流场三维速度分量。流场横截面内的速度矢量分布与相同实验条件下的流态显示结果相符合,并对涡流场加以分析。 相似文献