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.     

Low threshold particle arrays

While atmospheric Cherenkov telescopes have a small field of view and a small duty fraction, arrays of particle detectors on ground have a 1 sr field of view and a 100% duty fraction. On the other hand, particle detector arrays have a much higher energy threshold and an inferior hadron rejection as compared to Cherenkov telescopes. Low threshold particle detector arrays would have potential advantages over Cherenkov telescopes in the search for episodic or unexpected sources of gamma rays in the multi-TeV energy range. Ways to improve the threshold and hadron rejection of arrays are shown, based on existing technology for the timing method (with scintillator or water Cherenkov counters) and the tracking method (with tracking detectors). The performance that could be achieved is shown by examples for both methods. At mountain altitude (about 4000 m or above) an energy threshold close to 1 TeV could be achieved. For any significant reduction of the hadronic background by selecting muon-poor showers a muon detection area of at least 1000 m² is required, even for a compact array.     

芳纶纤维／环氧复合材料界面超声连续改性处理

运用超声技术在芳纶/环氧复合材料制备过程中对其界面进行改性处理,分析了超声处理过程中纤维与树脂之间浸润性的变化趋势以及超声作用对复合材料界面性能和力学性能的影响。结果表明:超声是通过改善纤维与树脂之间的浸润性,提高复合材料的界面性能及力学性能。     

基于BP人工神经网络的GPS／SINS组合导航算法

基于扩展Kalman滤波的GPS／SINS组合导航算法，需要对原始的非线性连续系统模型进行线性化和离散化处理，要求系统噪声和测量噪声为零均值的高斯白噪声，且易于出现滤波器发散。BP人工神经网络毋需对所求解的问题建模，能够很好地逼近系统非线性特性，获得较高精度的导航定位信息；还具有计算过程稳定，不涉及矩阵求逆，不需要迭代逼近，以及容易实现并行处理等优点。本文设计适用于GPS／SINS组合导航系统的BP网络模型，并在标准的BP算法基础上，采用共轭梯度法改进网络训练速度及精度。最后，通过仿真算例说明BP网络方法用于GPS／SINS组合导航计算的可行性。     

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。     

Mиг－23飞机尾旋试飞体会

Ｍиг－２３飞机是一种变后掠翼战斗机，它的尾旋动态及改出尾旋的方法很复杂。根据在该机上进行的四次尾旋飞行试验，叙述其尾旋进入的方法、尾旋中的动态和改出尾旋的方法。并举出三个典型的尾旋模态实例，详细记述整个尾旋过程和进行分析，说明Ｍиг－２３飞机尾旋动态的复杂性及其表现出的特点。最后，提出了几点在判断和改出Ｍиг－２３飞机的尾旋时应注意的事项。     

裂解温度对先驱体转化制备2D-Cf／SiC材料结构与性能的影响

以聚碳硅烷(PCS)、二乙烯基苯(DVB)和SiC微粉为原料制备了2D-Cf/SiC材料,考察了首次裂解温度对材料结构与性能的影响.结果表明,首次裂解温度的提高有助于弱化界面结合,形成良好的界面结构,从而提高材料的力学性能.当裂解温度从1000℃提高到1600℃时,材料的弯曲强度由200.7MPa提高到319.2MPa,剪切强度由16.8MPa提高到29.8MPa,断裂韧度由7.4 MPa·m1/2提高到15.0 MPa·m1/2.     

内装式机载发射运载火箭分离方案分析

针对一种内装式投放发射方案，建立了机载发射运载火箭分离过程的数学模型。本发射方案尢需对运载火箭进行改动。数值仿真结果表明．火箭在点火时有较好的姿态，适用于发射现有的中、小型运载火箭。     

中国民航学院法学本科教育的研究与思考——法学本科教育目的的探讨

在法学本科教育开创伊始,对其一系列问题急需进行全面的、系统的研讨,从而推动中国民航学院法学本科教育的发展和繁荣。对法学本科教育的教育目的进行了研究。     

21世纪中国的农业专用飞机

从中国的国情入笔，论速了农业航空在发展国民经济中的重要作用；农业航空采用农业专用飞机是必然趋势；指出农业航空滑坡问题亟待解决。