非壅塞火箭冲压发动机补燃室两相流数值模拟

采用颗粒轨道模型进行了非壅塞火箭冲压发动机补燃室两相流的数值模拟,其中铝颗粒的燃烧模型采用的是Davis扩散控制燃速的燃烧模型,建立了发动机补然室简单反应流模型,并在该模型下对某实验发动机进行了模拟,得出颗粒在补燃室内的分布,结果表明:与颗粒确定轨道模型相比,颗粒随机轨道模型更加适合模拟冲压发动机中的两相流动,并且颗粒的初始直径对颗粒燃烧效率有很大的影响。     

GPS姿态测量的载波相位整周模糊度快速解算

 根据 ARCE方法可以将模糊度搜索空间从所观测到的 m颗卫星的 m -1维降为 3维独立整周模糊度搜索空间,结合整数高斯变换及基线长度约束减小模糊度搜索空间,利用 Cholesky分解提高模糊度搜索效率,实验结果证明该方法能够快速解算整周模糊度适于实时姿态确定等应用。     

基于相位变化率的无源定位法

无源定位技术有着广阔的应用前景，本文在现有单站无源定位方法的基础上，介绍了相位变化率定位法。该方法利用观测平台上两个相互正交的相位干涉仪接收目标辐射电磁波的相位获取目标的方向信息，利用对应的相位变化率获取目标的径向距离信息，从而实现对目标的实时高精度定位。文中还给出了观测平台飞行姿态变化情况下的定位表达式。仿真结果表明，该方法是一种发展前途较好的单站无源定位方法。     

发动机高速动平衡的振动相位分析

针对发动机转子高速动平衡转速波动、无法保证振动信号同步整周期采样的特点,提出了一种基于转速脉冲的振动信号重构技术,大大提高了相量测量的准确度和稳定性。经试验验证,这项技术是有效、可行的。     

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.     

钛的相变织构及其影响因素研究

通过晶体学取向分布函数（ＣＯＤＦ）法研究了冷轧形变量、再结晶退火和相变循环次数等因素对钛相变织构形成的影响。结果表明冷轧形变量对相变织构的形成影响最大。再结晶退火后钛的相交织构漫散。多次循环相变并不改变相变织构的类型。     

飞行器静稳定裕度定义方法研究

本文研究了对于飞行器如何更加合理地定义其静稳定裕度的问题.常用的静稳定裕度定义为无量纲化的质心位置与气动焦点之间的距离,这种定义对于常见的高升阻比的飞机导弹等飞行器是适用的,然而对于一些非常规飞行器,例如载人飞船返回舱这类大钝头大配平攻角阻力体,这种定义在反映其静稳定程度上存在一定的问题.本文举例说明了这个定义存在缺陷,指出定义静稳定裕度时不能只考虑升力变化的影响,而是应该根据气动合力的变化来进行综合考虑.提出了新的比较完备的静稳定裕度定义方法,指出常用的静稳定裕度定义方法是本文提出的定义方法在特定情况下的表述,并举例说明了本文定义具有更加广泛的适用性.     

超声速进气道内特性数值模拟及性能分析

采用张涵信院士提出的无波动NND格式计算了某二级斜板可调的二元混压式超声速进气道的内部湍流流场 ,较好地模拟了激波间的干扰及激波 -附面层的相互作用 ,并在解法上运用了矢通量分裂算法 ,提高计算的效率、精度和稳定性。通过数值模拟 ,预测了其内流场主要性能参数 ,并分析了飞行条件、几何尺寸调节参数等因素对其性能参数的影响     

一种低噪声和高精度的频率合成技术

介绍了锁相环(PLL)技术和直接数字式频率合成(DDS)技术的基本工作原理,给出了一种提高DDS输出频率精度及减小其相位截断误差的方法。     

Flight Flutter Modal Parameters Identification with Atmospheric Turbulence Excitation Based on Wavelet Transformation

针对基于大气紊流激励的飞机颤振试验数据具有信噪比低以及测量数据以加速度响应形式给出等特点,将小波变换与随机减量法相结合对飞机颤振模态参数进行识别,首先利用随机减量法获得结构在非零初始加速度条件下的自由衰减响应,然后对该自由衰减响应进行Morlet连续小波变换,为使变换简单,本文采用了Parseval定理和留数定理,利用Morlet的带通滤波特性,通过搜索小波变换系数在不同的尺度区域内的极大值,再根据小波变换系数的极大值、相角与固有振动频率及阻尼系数间的关系,即可识别出各模态参数。并对利用小波变换识别颤振模态参数时,实现模态解耦应满足的条件进行了分析研究。通过仿真和飞机颤振试验数据分析,验证了该识别方法不仅简单、有效和可行,而且具有较强的抗噪性。