头部鼓包对不同截面机身侧力影响研究

 飞机或导弹在大迎角下飞行时会形成非对称涡，从而产生很大的侧滑力和偏航力矩。为了寻求消除侧滑力和偏航力矩或利用流动的非对称来提供飞机飞行所需的航向控制能力，研究了机头上放置小鼓包对3种不同截面的机身前体模型的影响。研究过程中采用了风洞测力和水洞流动显示的实验方法。结果表明，在20°~70°的迎角范围内，鼓包对圆锥的影响最大，对椭圆截面模型有一定的影响，对带棱截面模型的影响最小。鼓包越靠近前体头部，对侧力的影响越大。对圆锥柱体模型鼓包只能改变侧力最大值出现的迎角，而对减小最大侧力值作用不明显。对椭圆截面模型，可使最大侧力系数从1.98降到0.53，很大程度上降低了侧力。带棱截面模型对鼓包的大小和位置均不敏感。     

涡流器排对附面层热传输的影响

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。     

涵道螺旋桨桨叶涡强度分布计算

本文依据开式螺旋桨理论 ,涵道后缘的库塔条件以及微元涡丝的诱导方程 ,建立了涵道螺旋桨叶片涡强度分布的计算模型并进行了数值计算。结果显示 ,涵道螺旋桨桨叶涡强度在桨尖处达到最大     

航空发动机主燃烧室稳定工作范围研究

应用火焰传播理论、二维两相紊流燃烧的k-ε模型、EBU-Arrhen ius模型、颗粒群轨道模型和AD INA软件,计算出了某型在研航空发动机在不同飞行状态下的主燃烧室贫油熄火时的流场、温度场和压力场;计算值与试验结果比较吻合,证实了数值模拟的合理性和可行性。     

栅格翼尾流中的发卡涡

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。     

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.     

进口流量对无管式减涡器流阻特性影响研究

为分析进口流量对压气机引气系统无管式减涡器压力损失的影响及无管式减涡器减阻效果,采用数值模拟与试验研究相结合的方法对无管式减涡器开展研究,并与直喷嘴模型进行了对比。模型试验验证了数值模拟方法的可靠性,通过数值模拟,建立了无管式减涡器流阻特性"S"形曲线三分区模型,分析了无管式减涡器各截面间压力损失及其占比随无量纲质量流量变化规律。在计算流量范围内,与直喷嘴模型相比,无管式减涡器平均可降低压气机引气系统压力损失约45.9%。在第二拐点处,共转盘腔内压力损失降低了96.44%,此时无管式减涡器减阻效果最佳,较直喷嘴模型压力损失降低了73.44%。     

亚,超声速旋涡流动特征的定性分析研究

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     

航空发动机燃烧室主燃区的数值模拟分析

概述了先进燃烧室的主燃区数值模拟,论述了采用气动喷嘴时确定边界条件的方法和模拟燃油喷嘴油滴轨迹的结果。对某型发动机燃烧室的主燃区进行了数值模拟,给出了熄火时主燃区流场,分析了主燃区温场对出口温场的影响     

航空发动机燃烧室蠕变屈曲研究

根据试验与计算分析,提出了确定构件蠕变屈曲临界时间的“曲率极大点”法。理论计算与试验结果的一致性表明该方法合理、有效、可行;通过对板、圆柱壳蠕变屈曲的试验与计算分析,为航空发动机燃烧室的蠕变屈面研究提供了模型简化的基础和方法上的准备;最后,对某型航空发动机燃烧室蠕变屈曲进行了计算分析。