小行星探测最优两脉冲交会轨道设计与分析

小行星探测已经成为新世纪深空探测的一个新热点和未来世界航天发展的一个新方向。转移轨道的设计和探测目标可接近性的分析是小行星探测的关键技术之一。现利用了任意两个非共面非共轴椭圆轨道之间的最优两脉冲转移方法，对我国提出的探测Ivar小行星的交会转移轨道进行了设计与分析，给出了全局最优两脉冲交会轨道的设计参数，并利用此方法对近地小行星的可接近性进行了分析和排序，给出了可接近性较好的40颗近地小行星的转移轨道设计参数。这些研究结果对于近地小行星探测任务的目标选择和发射机会的预测都有重要的参考价值。     

放置倾角对轴向槽道热管传热特性影响的实验研究

对常温梯形轴向槽道热管在不同放置倾角下的传热特性进行了实验研究，着重分析了热管的放置倾角对轴向温度分布、最大轴向温差、总热阻、当量换热系数、最大传热量的影响，旨在为航空热管的地面性能测试提供参考。实验结果表明：热源在下垂直放置热管的蒸发段和冷凝段的当量换热系数分别是水平放置热管的1．5倍和2．5倍。热源在上倾斜放置的热管，水平放置的热管、热源在下倾斜放置的热管的平均总热阻成一个数量级递减，蒸发段的最大输入热流量依次递增一个数量级。     

多级航天器在有限推力情况下的最优变轨问题探讨

与航天运载器类似,航天器也可以有单级与多级之分。一个多级航天器是由几个具有动力装置的航天器经串联而成的组合体。本文研究这类航天器的最优变轨问题。多级航天器在有限推力情况下的最优变轨问题,实质上属于多级最优控制问题。本文应用多级最优控制问题的求解原理,讨论有限推力情况下,两级航天器在两共面圆轨道之间的两类最优转移问题,给出了确定最优推力程序和最优转移轨迹的定解方程和定解条件,特别考察了级间分离时刻应满足的条件。本文给出的原理同样适用于非圆形、非共面轨道之间的最优转移问题。     

关于鲁棒Kx观测器设计的几个问题

对于具有结构不确定性的线性系统,本文研究了与Kx观测器设计有关的几个问题。文中建立了观测器应满足的条件,并对控制器设计时的分离原理和闭环系统的鲁棒性进行了讨论。     

红外热波成像法测量薄板局部换热系数

通过连续激光调制对薄板试样进行局部周期加热，采用红外扫描测温技术记录动态温度分布。利用博里叶变换分析温度基波相位和幅值变化，进而推算壁面的局部换热系数。介绍了该方法的测量原理，在风洞中对两种不同厚度的薄板进行了实验研究，并对实验结果进行了分析和讨论。     

X-ray radiation from accreting, magnetized neutron stars

A review is given of recent developments in the theory of emission from a magnetized plasma for accreting neutron star conditions. Some observational data on X-ray pulsars are discussed, and present problems are indicated.     

热防护系统的硅纤维隔热层复合传热数值计算

鉴于热防护系统的硅纤维隔热层是各向异性的非灰体材料，其复合传热计算是复杂且耗时的，提出了一种简便方法用于硅纤维这类各向异性非灰体材料的复合传热计算。该方法借鉴了医学领域断层摄影法（局部X射线检测法）中对光沿各向异性散射介质传播分析的思路，得到了各向异性扩散的热辐射方程（RTE—D）并把该方程用于求解非灰体半透明介质的辐射热通量。计算结果与文献中基于辐射传递方程（RTE）求得辐射热流的复合传热数值结果相比较，其最大相对误差为1．5％，并且其计算时间也由Pentium Ⅱ的3297．66分钟缩短为PentiumⅣ的约5分钟。最后，该方法被用于真实热环境下刚性隔热瓦L1900（高空隙率硅纤维隔热材料）的复合传热计算，计算结果与实验数据有较高吻合度。数据结果表明，各向异性的扩散近似被用于求解非灰体半透明介质的辐射热通量的方法用在热防护系统的硅纤维隔热层复合传热数值计算中是简便高效的。     

燃气源控制气流热效应数值模拟研究

为了解迷宫形导热套环与流体之间的热交换对控制气流温度及压力的影响,采用整体求解法求解控制气流与多层套环之间的耦合传热问题。为确保计算结果在物理上的真实性,采用“假密度法”求解以温度T为求解变量的能量方程。计算得到了控制气流参量随时间的变化情况以及迷宫形多层导热套环的温度在不同时间点的分布情况,结果表明流场的三维复杂结构使得每个小孔射流与各层套环的传热情况都不同,流体与固体区域之间的换热量随时间变化,其中内套环和中套环对流体的吸热量随时间的增长而急速下降,从而导致控制气体的温度和压力都随时间而逐渐增大。计算所得的控制气流温度和压力与试验测量值的变化趋势相同,验证了计算方法的有效性。     

Influence of ionospheric perturbations in GPS time and frequency transfer

The stability of GPS time and frequency transfer is limited by the fact that GPS signals travel through the ionosphere. In high precision geodetic time transfer (i.e. based on precise modeling of code and carrier phase GPS data), the so-called ionosphere-free combination of the code and carrier phase measurements made on the two frequencies is used to remove the first-order ionospheric effect. In this paper, we investigate the impact of residual second- and third-order ionospheric effects on geodetic time transfer solutions i.e. remote atomic clock comparisons based on GPS measurements, using the ATOMIUM software developed at the Royal Observatory of Belgium (ROB). The impact of third-order ionospheric effects was shown to be negligible, while for second-order effects, the tests performed on different time links and at different epochs show a small impact of the order of some picoseconds, on a quiet day, and up to more than 10 picoseconds in case of high ionospheric activity. The geomagnetic storm of the 30th October 2003 is used to illustrate how space weather products are relevant to understand perturbations in geodetic time and frequency transfer.     

New field of application of the IRI modeling – Determination of ionosphere transfer characteristic for radio astronomical signals

We suggest a new field of application of IRI modeling – determination of ionosphere transfer characteristic (ITC) for radio astronomical signals (RAS). VHF and HF RAS are widely used for observations of the Sun and pulsars. It is necessary to take into account possible distortions of RAS in the Earth ionosphere. However, in contrast to modern navigation systems (GPS, GLONASS, GALILEO), where very accurate reconstruction of ionosphere parameters is a built-in function, in present-day radio astronomy a retrieve of ITC has not been appropriately worked out yet. It collides with increasing requirements to accuracy of the analysis of RAS amplitude profile and to the angular and polarizing resolution of radio telescopes of new generation. We have developed a method and software for calculation of the ionosphere measure of rotation (RM) and the measure of dispersion (DM). We used the ionosphere model IRI-2001, magnetic-field model IGRF-10 and values of ionosphere total electron content as deduced from GPS measurements. The obtained values of the ionosphere DM and RM were recalculated into characteristics of phase delay, Faraday amplitude modulation and polarization changes. We made calculations for different levels of geomagnetic activity and for different angular position of radio sources as well.