Deep Impact Mission Design

The Deep Impact mission is designed to provide the first opportunity to probe below the surface of a comet nucleus by a high-speed impact. This requires finding a suitable comet with launch and encounter conditions that allow a meaningful scientific experiment. The overall design requires the consideration of many factors ranging from environmental characteristics of the comet (nucleus size, dust levels, etc.), to launch dates fitting within the NASA Discovery program opportunities, to launch vehicle capability for a large impactor, to the observational conditions for the two approaching spacecraft and for telescopes on Earth.     

The History and Dynamics of Comet 9P/Tempel 1

Since its discovery in 1867, periodic comet 9P/Tempel 1 has been observed at 10 returns to perihelion, including all its returns since 1967. The observations for the seven apparitions beginning in 1967 have been fit with an orbit that includes only radial and transverse nongravitational accelerations that model the rocket-like thrusting introduced by the outgassing of the cometary nucleus. The successful nongravitational acceleration model did not assume any change in the comet’s ability to outgas from one apparition to the next and the outgassing was assumed to reach a maximum at perihelion. The success of this model over the 1967–2003 interval suggests that the comet’s spin axis is currently stable. Rough calculations suggest that the collision of the impactor released by the Deep Impact spacecraft will not provide a noticeable perturbation on the comet’s orbit nor will any new vent that is opened as a result of the impact provide a noticeable change in the comet’s nongravitational acceleration history. The observing geometries prior to, and during, the impact will allow extensive Earth based observations to complement the in situ observations from the impactor and flyby spacecraft.     

TiC/Al复合材料在锌液中均匀化机理分析

采用自蔓延高温合成（SHS）法制备高TiC颗粒含量的TiC／Al复合材料。利用自制的实验装置研究复合材料中TiC颗粒在静止锌液中的均匀化过程。结果表明：当锌液温度低于铝的熔点时，TiC／Al复合材料置于锌液后，锌向其内部扩散，引起复合材料表层内液相线温度降低，当表层内Al-Zn合金的液相线温度等于或低于锌液温度时，Al-Zn合金便处于熔融状态，TiC颗粒随其一起从TiC／Al复合材料块上脱落，并不断地向锌液内部传输，最终均匀分布在锌液中；而当锌液温度高于铝熔点时，TiC／Al复合材料置入后，锌和铝同时进行扩散，但是当复合材料表面温度达到铝熔点时，铝开始熔化，铝的熔化导致TiC颗粒的脱落，脱落下来的TiC颗粒不断向锌液内部传输，最终均匀分布在锌液中。     

有1的结合环的交换性

本文证明了有１的结合环的两个交换性定理，推广了Ｇｉｒｉ．Ｒ．Ｄ等人在参考文献１中的结果。     

应用模拟退火算法求解飞机调度问题

通过分析飞机运行的时区集合特点,将飞机调度问题转化为固定工件排序问题。根据工件占用机器的时间区间,利用划分时间片算法把需要平行作业的工件挑选出来组成无向图的相邻顶点,从而将固定工件问题转化为图的k-顶点着色问题,然后建立0-1整数规划数学模型,并设计出相应的模拟退火算法。最后应用该算法针对飞机调度问题进行了仿真研究,结果表明:在可接受的时间内能够得到该问题的满意解。     

SN 1987A and SN 1993J: Testing stellar evolution theory?

Nearby supernovae like SN 1987A and SN 1993J provide valuable constraints on the late evolution of massive stars. For this purpose, we review evolutionary models for the progenitor of SN 1987A and confront them with five observational/theoretical tests we devised. We show that single-star models (with the possible exception of rapid-rotation models) fail at least two of these tests, while two binary models (accretion and merger models) are consistent with all available constraints. We conclude that it is most likely that the progenitor of SN 1987A had a binary companion, either at the time of the explosion or at least in the not-too-distant past, and that SN 1987A should therefore not be used to calibrate single stellar evolution theory. For SN 1993J, we infer from the presupernova photometry and the early light curve that its progenitor was a 15M star that lost almost all of its hydrogen-rich envelope prior to the supernova. This seems to require that the progenitor underwent stable case C mass transfer. We discuss future observational tests of binary models for both supernovae.     

检定结果A类标准不确定度的评定方法

介绍了检定工作中检定结果A类标准不确定度的评定方法及一些应用中的问题。     

1/f波动数据的产生及其舒适感分析

为了获得使人感到舒适的自然风,提出了对风扇转速进行1/f控制的方案,详细论述了1/f波动数据的生成和对风扇电机电压的控制方法,并用单因素方差分析的方法将1/f波动控制产生的舒适感的效果与白噪和1/f 2波动控制方式的情况进行比较,证明了1/f波动控制方式对于提高人的舒适感的有效性.     

一种高性能24通道模入数据采集控制卡的设计

介绍了一种基于A／D转换芯片MAXl97的高性能数据采集控制卡的设计方案，列出了它的主要性能参数，并给出了它的具体应用实例。     

正确实施CE106发射试验的两个基本条件

提出了正确实施GJB151A/152A-97CE106发射试验的两个基本条件。只要发射机天线端口基波峰值功率和测试系统配置参数符合了这两个基本条件,超过极限值的任何谐波和杂波将会显示在测试结果中。