旋转同心双轴间流动的热态实验

某型发动机高、低压涡轮轴间环形气流通内的流动可以简化为两个独立旋转同心双轴环道内的流动问题。对其控制方程以及边界条件进行无量纲化，得出了实验准则，设计并建立了实验台，以实验方法研究了具有轴向通流的独立旋转同心双轴环道内的流动规律。结果表明，随着冷气雷诺数增大，阻力系数总体趋势减小；冷气雷诺数的影响远大于内轴和外轴旋转对流动的影响。     

高能氧化剂二硝酰胺铵的热分解研究

为深入了解二硝酰胺铵(ADN)的热分解，为该氧化剂在推进剂中应用提供必要的技术保障和实验依据，采用热重分析法(TG)及差示扫描量热法(DSC)，实验研究了氮气流量、合成中间体烷基羰基N-硝酰胺铵(AUN)及硝酸铵(AN)对ADN热分解过程的影响，并利用model-free isoconversional方法模ADN热分解过程的活化能曲线。结果表明：氮气流量和硝酸铵(AN)对ADN的热分解过程有显著影响，而AUN可使ADN热分解曲线产生肩峰，但基本不影响ADN的热分解过程。     

Calibration of the MERIC full-polarimetric radar: theory and implementation

This paper describes the architecture and calibration design of the experimental ground based radar station MERIC. This full-polarimetric radar is conceived for the analysis and the recognition of non cooperative aircraft in flight.We carefully study how the full-polarimetric capability is obtained for a simultaneous transmit (simultaneous transmission of two linear FM with opposite slopes) radar system, using analogue deramping with a replica.The phase distortions of the signal propagating in the four polarimetric channels are carefully estimated. We define a phase calibrating method compatible with the outdoor measurements conditions and few constraints on reference targets.We show the phase accuracy obtained with the proposed calibration method on real measurements.     

组合催化剂MT在丁羟推进剂中的应用

研究试验了组合催化剂MT在丁羟推进剂中提高燃速和降低燃透压强指数的作用。结果表明，MT与不同含量和粒度小于10μm的AP匹配使用，燃速可在9mm／s～30mm／s范围内调节；压强指数均小于0．2（压强范围3MPa～9MPa），出现“平台”燃烧效应；发动机实测的压强指数与试验结果基本一致；选用合理的M与T组合比，可不影响推进剂制造工艺性能和药柱力学性能。对结果的理论分析认为，M与T对改善AP低压下热分解具有协同效应。     

基于解析及特征造型的涡轮冷却叶片参数化设计

基于数学解析与特征造型技术相结合的方法,建立了基于构造过程的复杂涡轮冷却叶片的参数化设计技术。用五次多项式描述叶身型线,根据壁面厚度函数求解冷却通道外形,定义冷却通道隔板位置及厚度等参数,计算得到叶身及冷却通道各截面造型数据;以特征造型方法完成对涡轮冷却叶片转弯流道、缘板、榫头及叶片相关特征的参数化设计;利用CAD系统的二次开发接口,实现了多腔回流式涡轮冷却叶片的自动建模。     

一种模拟喷管二维流场的新方法

采用ＳＩＭＰＬＥ方法对固体火箭发动机喷管进行了纯气相流场的数值模拟。推导了建立在同位网格之上利用协变物理速度分量为计算变量的离散方程，采用协变物理速度分量推导压力修正方程，对密度采用一阶迎风格式插值，将ＳＩＭＰＬＥ方法扩大到计算可压流动。计算结果表明：本方法计算精度高，收敛速度快，程序编写简单。     

A Correlation Polarimeter for Noise-Like Signals

Optimum estimation (tracking) of the polarization plane of a linearly polarized electromagnetic wave is determined when the signal is a narrow-band Gaussian random process with a polarization plane angle which is also a Gaussian random process. This model is Compared to previous work and is applicable to space communication. The estimator performs a correlation operation similar to an amplitude -comparison monopulse angle tracker, giving the name correlation polarimeter. Under large signal-to-noise ratio (SNR), the estimator is causal. Performance of the causal correlation polarimeter is evaluated for arbitrary SNR. Optimum precorrelation filtering is determined. With low SNR, the performance of this system is far better than that of previously developed systems. Practical implementation is discussed. A scheme is given to reduce the effect of linearly polarized noise.     

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.     

激光微推进器用于微小卫星的姿轨控仿真

为研究激光微推进器用于微小卫星在轨空间飞行任务的可行性,利用已建立的激光推进微小卫星仿真平台,对微小卫星在轨姿态调整、轨道维持和轨道转移等飞行任务进行了仿真和分析。仿真结果表明,星载激光微推进器可满足在轨微小卫星的高控制精度姿态调整、近地观测轨道维持以及较长时间要求的轨道转移等空间任务对推进系统的要求。     

含能工质激光烧蚀推进效率分析

为了分析在高能脉冲激光作用下,含能工质化学能对推进性能的影响,在实验的基础上,对固体含能工质激光烧蚀推进过程中的能量效率进行了初步分析。结果表明:含能工质自身化学能在激光推进中具有重要的作用;与火箭推进方式相比,固体含能材料激光烧蚀推进方式的能量利用效率更高。