跨音压气机确定应力场分析

采用全三维黏性定常、非定常数值模拟技术,对NASA 67第1级的固有非定常流动进行了研究.首先分析了定常流场和非定常时均流场间的差别以及压气机中典型的转、静干涉现象,然后对通道内确定应力的分布规律和转、静交界面确定应力各项的分布特点进行了较为深入的研究,揭示了现有确定应力模型的一些局限性,可为确定应力建模提供一定的指导作用.     

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。     

Evolution of the Protosolar Nebula and Formation of the Giant Planets

The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models” in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth. We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation from the molecular cloud onto the disk, disk evolution and migration of solids. Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and their global composition. This revised version was published online in August 2006 with corrections to the Cover Date.     

三维管道超声速气固两相流动的CFD/DSMC仿真

采用NND格式求解气相N-S方程，采用DSMC方法模拟固相颗粒运动，数值模拟了三维管道超声速气固两相流场，分析了固体颗粒对流场结构产生的影响。计算结果表明，将DSMC方法与CFD方法相结合是解决气固两相流动问题的一种有效途径。     

单晶高温合金接近使用条件下的寿命估算与损伤分析

针对发动机热端部件承受的典型载荷谱，发展了一种通用的寿命预测方程和损伤分析方法。这个方法是在疲劳蠕变交互作用断裂特征图及其最大应力修正的寿命方程基础上建立的。根据ＤＤ３单晶合金的疲劳蠕变交互作用断裂特征图及其最大应力修正的寿命方程，验证了本方法是切实可行的。预测精度是符合要求的。     

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。     

共轴式直升机旋翼气动干扰对航向操纵的影响

利用共轴式旋翼风洞实验结果，结合轻型共轴式直升机M16飞行中的现象，分析了上下旋翼气动干扰对共轴式直升机过渡飞行中航向操纵的影响。介绍了直升机由悬停转入垂直上升、平飞中加减速和转入爬升与下滑等过程中，由于上下旋翼干扰发生了变化，使直升机航向发生偏转后飞机的反应情况，以及在这种情况下应进行的相应操纵。所得结果对研究共轴式直升机的操稳特性有重要意义。     

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。