机载小惯量探针研制及在飞机武器发射中的应用

介绍了一种用于飞机武器发射时测量发动机进口动态温升时序的机载小惯量探针,以其独特的研制方法,较好地解决了机载小惯量测温装置、频响与可靠性兼顾这一测试难题,并在武器发射时,成功地用来评价发动机工作稳定性的影响。     

高超声速无粘流场的推进计算

本文将文[1]中用于时间相关法计算的NND格式推广到定常超声速流动的空间推进计算,采用二步的预测、校正方法保证了推进方向的二阶精度,可以证明,这种二阶精度的NND格式具有TVD性质,是MacCormack二步显式格式的推广。本文首先将格式应用于二维平板上斜激波反射流场的推进计算,以检验格式捕捉激波的能力,同时研究了不同的通量分裂方法对格式捕捉激波能力的影响,得到了相当满意的结果。在此基础上,计算了航天飞机简化外形的身部超声速流场,给出了M_∞=10,α=0°,和M_∞=5,α=5°两种状态的部分结果,计算结果清楚地描绘了由于气流在机翼附近受到强烈压缩而产生的内嵌激波与外激波相交的复杂流场结构,与文[7]相比,流场结构更为清晰。     

失重环境下圆柱形容器内稳态旋转液体的液面形状

1.引言 在航天高技术中,由于星体充液量的增大以及飞行器姿态指向精度的严格要求,从而液体晃动问题受到了国内外科技界的广泛重视。飞行器在外层空间正常飞行时,液体处于失重状态,此时,不能忽视表而张力的作用,静止自由液面呈特殊曲面,其形状直接影响着液体的动力学特性由于卫星在入轨后处于稳定的自旋状态,这时液面由液体表面     

基于图像识别的发动机内窥智能检测系统研究

介绍了一种基于图像识别技术的航空发动机内窥检测的新方法，采用最大类间方差法计算二值化分割的最佳阈值，并将提取的图像特征输入神经网络进行分层识别，最后由专家系统对损伤程度进行了诊断。通过现场测试，证明了该方法的有效性和实用性．     

月球探测器姿态大角度机动的反作用轮控制

研究了月球探测器转速与控制力矩受限的姿态大角度机动问题。根据时间变尺度思想，提出了双回路反馈的姿态大角度机动控制方法。以某型月球控测器为例，对该方法进行了仿真验证。结果表明，利用该控制方法，可使探测器以期望的角速度转动，从而完成探测器的姿态大角度机动。     

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.     

可重复使用运载器磁悬浮助推发射参数研究

针对磁悬浮助推水平起飞运载器这种新型发射概念,采用概念性分析方法,研究地面发射参数对可重复使用运载器性能的影响规律。结果表明,助推发射水平起飞运载器在降低初始推重比、推进剂和结构质量等方面具有优势,最后得出地面发射参数的一组优化值。     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.     

一种能同时测量喷嘴下游气液流强的两相探针的研制

 针对液体火箭发动机喷注器下游燃料和氧化剂两相流场分布的实验研究，研制了能同时对其流强及混合比进行测量的两相探针，并对其进行了标定。利用两相探针对不同反压下同轴式喷嘴下游的流强和混合比分布所进行的试验研究，证明探针的设计是成功的     

航天飞机三维最优再入轨道及气动加热过程

本文应用现代控制理论研究了航天飞行器三维最优再入轨道和与轨道参数密切相关的气动加热过程。文中选择飞行器迎角和倾斜角作为控制变量,以飞行器气动加热率和飞行过载沿轨道积分最小作为优化性能指标,按极大原理导出最优再入轨道有约束控制的非线性两点边值问题。采用了数值优化方法——共轭梯度法求解有升力飞行器的最优再入轨道及其热过程。文中以允许误差法讨论了权系数和罚函数的选取方法;对不同速度范围研究了不同的加热模型;按热平衡方程与优化轨道同步迭代的方法求得了算例数值结果。算例的数值结果与文献[13]的量值是一致的。