Calculation of the transonic dip of airfoils using viscous-inviscid aerodynamic interaction method

A numerical procedure for the calculation of the transonic dip of airfoils in the time domain is presented. A viscous-inviscid aerodynamic interaction method is taken to calculate the unsteady aerodynamic loads. In the present case the integral boundary layer equations are coupled with the Transonic Small Disturbance (TSD) Potential Equation. The coupling between structural motion and aerodynamic loads is carried out using State Space equation. It is solved by State Transition Matrix technique. Results are presented for NACA 64A010 and NLR 7301 airfoils with structural data from Isogai and DLR, respectively. Comparisons show good agreement with other numerical results. Certain deviations of experimental data taken from literature need more insight in the detailed test conditions.     

平面运动激波在定常超音速劈表面马赫反射的研究

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。     

六类高超声速激波-激波干扰的数值模拟研究

基于粘性全N-S方程，利用有限体积法进行数值离散，对Ⅰ到Ⅵ六种类型的激波一激波干扰现象进行了数值模拟，其中采用了二阶Harten-TVD格式，LU隐式算法以及Baldwin-Lomax代数湍流模型。每种类型都得到了清晰的干扰流场结构，其中Ⅳ型干扰的模拟结果与实验结果进行了比较，符合较好。数值模拟结果的对比指出，由入射位置差异引起的不同类型激波-激波干扰结构有很大不同，对壁面压强分布的影响也存在较大差异。     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

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.     

粘流与无粘流的相互作用计算

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。     

超声速流中激波/湍流附面层干扰数值模拟

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。     

上游转子对下游静子叶片气动力的影响

为研究轴流压气机下游静子叶片非定常气动力的大小和频率的变化规律,采用在静子叶片表面埋设微型动态压力传感器的方法,在低速单级轴流压气机实验器上进行了静子叶片表面压力的测量。测量了不同轴向间距、不同转速下从近堵塞到近失速的宽广流量范围,并对所测得的静子叶片非定常气动力进行了离散傅立叶变换,以分析其频谱特性。实验结果表明：在转子尾迹的影响下,静子叶片表面的波动频率是转子的尾迹频率及其倍频。转子尾迹频率的高频分量对静子叶片吸力面前缘的影响比对其他位置的影响大。叶片表面的非定常压力和气动力随压气机流量、转速和轴向间距的变化而变化。     

基于重力模型阶次自适应的实时重力补偿系统研究

为了解决探测器在月面工作时惯性导航系统的误差累积问题,克服现有研究对环境敏感或是需要定期停止才能进行误差修复的短板,结合探测器的行驶行为,将探测器使用零速更新（ZUPT）原理修正误差的过程分解成了无ZUPT、完全ZUPT、水平动态ZUPT和垂向动态ZUPT 4种子模型的叠加,并分别推导了它们的系统矩阵和测量矩阵。针对月面导航系统提出了一种新型多模型零速更新（MMZUPT）算法。该算法应用多模型交互原理,允许多种更新模型同时工作,可以通过计算每个模型的权重在每个定位历元输出最优导航结果并约束误差。在精心挑选的受限环境中对月面导航进行了模拟实验,结果表明,所提MMZUPT方法无需频繁地主动停车以满足传统ZUPT使用边界就可以取得良好的效果,并且通过对包含错误的校准信号加以识别和利用可以获得更好的性能。     

流向涡与斜激波相互作用的试验研究和数值模拟

为研究流向涡与斜激波相互作用在超声速燃烧中的应用,进行了由翼产生的流向涡与楔块产生的二维斜激波相互作用的燃烧室冷流试验研究.在不同激波强度下,纹影仪捕捉到了强、中、弱不同的涡/波作用现象.仿真与试验结果符合得较好.试验结果表明:对马赫数为2.3流场,在翼攻角10°时,能产生强流向涡,此工况下,锲角越大,涡/波作用越强.仿真结果表明:马赫数对涡/波作用影响较大,总压影响不明显,总温可影响亚声速回流区的尺寸.      

上游尾迹与涡轮转子泄漏流相互作用数值模拟

叶轮机内部流动本质上是周期性非定常的,研究涡轮转子叶尖区域的非定常相互作用机理,对提高小展弦比高负荷涡轮性能具有重要意义.利用数值模拟方法研究了上游静子尾迹与涡轮转子叶尖泄漏流的非定常相互作用,分析了定常结果、时间平均结果以及瞬时时刻结果的流动图画.结果表明:上游静子尾迹与涡轮转子尖区二次流的相互作用能明显影响泄漏涡和机匣通道涡的时空演化规律,从而改变转子尖区的损失分布.上游尾迹在转子通道中传播时,诱导泄漏涡和通道涡区域出现周期性的扰动涡对,扰动涡对沿着泄漏涡和通道涡的轨迹向下游运动,使得转子尖区二次流结构呈现周期性变化.