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11.
本文介绍了在电控双驱动激波风洞中进行的平面运动激波在有定常超音速绕流的尖劈表面马赫反射的实验。这种反射现象属于准定常的,在实验中观察到了四种反射(RR,SMR,CMR和DMR)。本文还计算了三波点Τ的迹线及弯折点Κ的迹线分别和劈面的夹角χ和χ',以及各种反射相互转变的边界。发现运动激波波前定常超音速气流马赫数Μ_0会影响χ和χ'角,使(θ_ω+χ,Μ_s)平面上各种反射的转变边界发生变化,但不影响(θ_w,Μ_s)平面上的各条转变边界线。 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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合并会计报表中内部存货交易抵销的理论与方法 总被引:1,自引:1,他引:1
随着经济的迅速发展,合并会计报表越来越重要.文章系统完整地论述了适用于任意条件的内部存货交易抵销(包括内部销售损益抵销和存货跌价准备抵销)方法,首次提出并验证了存货跌价准备的两种抵销方法,即分析抵销法和综合抵销法. 相似文献
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粘流与无粘流的相互作用计算 总被引:1,自引:1,他引:1
本文总结了粘流/无粘流的各种计算方法和结果。重点在于介绍定常流动中的弱相互作用。首先叙述了弱相互作用的数学模型。给出了不可压流动和跨音速流动中粘流/无粘流相互作用的某些正耦合的计算结果。讨论了在分离区附近边界层正方法失效的原因。然后介绍了边界层反方法和适用于带分离的流动中半反方法耦合的粘流/无粘流的相互作用方法。文中也简单地总结了三维情况的应用和强相互作用。 相似文献
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采用流固耦合的数值计算方法研究了NACA 0 0 15翼型在大迎角 ( 15°~ 6 0°)范围的颤振 ,以及在翼型背部部分引入射流的减振技术。在流体区域用高精度、高分辨率算法求解Farve平均的Navier Stokes方程 ,在固体区域用四阶Runge Kutta法求解振动方程 ,并且每一个时间步后都在两个区域之间传递边界条件。计算结果表明在翼型背部引入适当射流会降低翼型的振动 ,并提高升力。但如果引入射流的速度过高 ,会在叶背处形成新的分离流 ,升力反而会下降 相似文献
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超声速流中激波/湍流附面层干扰数值模拟 总被引:6,自引:1,他引:6
采用修正的B/L湍流模型以及多块结构化网格求解了二维N-S方程。分别对超声速流和高超声速流中的激波/湍流附面层干扰进行了数值研究。本文首先研究了进口马赫数为2.96的超声速流。计算结果准确预测了入射斜激波在平直壁面引起湍流附面层分离的流动特征:分离点的反射激波、分离包引起的膨胀扇以及再附点的反射激波。计算的壁面压力分布与实验值吻合较好,计算的分离区长度与实验值比较有一定误差。本文还对进口马赫数为9.22的高超声速流中压缩角引起的激波/湍流附面层干扰进行了数值研究。计算结果与实验结果吻合较好。 相似文献