信鸽归巢导航的多信息融合

信鸽远距离导航能力一直以来都是生物导航领域研究的热点问题,其奥秘的逐步展露和揭示对仿生导航乃至仿生学的发展都有着十分重要的启发意义.论文归纳了基于环境的信鸽导航理论、基于信鸽感测能力的导航理论以及基于信鸽生理特征的导航理论的研究情况,介绍了近些年信鸽导航研究领域的新进展,展望了未来可能取得的突破方向.     

导航显示管理计算机的设计及关键技术

导航信息显示管理计算机通过人机交互向飞机驾驶人员提供各种飞行状态及飞行指引参数,本文以某飞机测控平台辅助导航显示管理计算机设计实现为例,介绍了导航信息显示管理计算机的工作方式、工作流程并探讨了导航信息显示管理计算机的设计特点和关键技术。     

组合导航技术在可重复使用运载器再入段的应用研究

结合国内外可重复使用运载器的发展现状及各导航方法的特点,根据飞行器再入飞行段动力学方程,建立再入段飞行轨道并提出适用于再入飞行其各段的导航方法。对再入飞行中的末端能量管理段进行全面研究,设计并进行INS和INS/SAR导航滤波计算机仿真,并对仿真结果进行了误差分析。     

地形景象匹配辅助导航可视化仿真研究及软件实现

为了直观有效验证地形景象匹配算法和演示地形辅助导航的过程,设计了地形景象辅助导航可视化仿真软件系统.利用Visual C 和OpenGL的功能实现了对导航数据和飞行过程的动态二维可视化曲线显示,对匹配区域中的实测图和参考图进行动态显示,能够直观地分析匹配结果的正确性;并在此基础上着重对地形景象匹配辅助导航过程实现了可视化仿真显示,能形象直观地演示地形景象辅助导航的过程及其性能.通过多次试验表明,该软件能很好地演示地形景象辅助导航系统的全过程及其性能,具有很好的实际应用价值.     

直升机飞行参数记录系统设计及典型故障诊断研究

飞行参数记录系统能有效提高飞行训练的安全性.根据直升机飞行安全需要,结合工程经验,对直升机加装飞行参数记录系统进行分析研究,介绍飞行参数记录系统的基本组成和原理、加装原则和相关标准以及飞行参数的校准方法;对飞行参数记录系统两个典型故障进行诊断分析,并提出解决方案.飞行参数记录系统相关设计的研究能够为工程技术人员在进行设计应用时提供一种思路和参考.     

卡尔曼滤波在弹道组合导航仿真中的应用

根据捷联惯性导航(INS)和GPS导航两个系统不同的特点,通过卡尔曼滤波方法实现了INS/GPS组合导航,以速度差和位置差作为卡尔曼滤波的量测量信息,建立了组合导航的简化滤波方程.在实际陀螺器件含有零偏的情况下,通过在角速度上引入定量的零位偏置来进行弹体模拟投放过程.将仿真导航结果和弹道参数比较,引入的陀螺偏置引起姿态角误差,而速度误差和位置误差比较小,导航计算参数误差在允许范围之内.     

可重复使用飞行器导航制导控制技术展望

针对当前可重复使用飞行器的发展现状,总结了其特点、优势和发展趋势.通过飞行任务,分析了可重复使用飞行器所面临的复杂环境特性和飞行控制特性.从飞行控制角度出发,概括了可重复使用飞行器导航制导控制所面临的技术挑战,包括高精度导航技术、多约束航迹优化技术、再入段和能量管理段的制导技术以及强耦合强不确定强鲁棒姿态控制技术等.最后,针对技术挑战,对可重复使用飞行器导航制导控制技术提出了若干建议.     

基于六自由度方程的飞机结冰问题仿真

基于六自由度方程对飞机的结冰飞行动力学问题进行了仿真研究。首先针对飞机遭遇结冰时的结冰飞行过程进行仿真,开发了一种结冰过程中飞机结冰严重程度及气动参数的计算方法。通过在各仿真时刻对飞机气动参数进行结冰影响修正以实现对飞机结冰飞行过程的模拟,同时分析了结冰过程对飞行特性的影响。进而对飞机结冰后带冰飞行时不同结冰严重程度下的操纵面阶跃响应进行了仿真,并对仿真结果进行了分析。     

气压垂直导航中修正高度分析

在世界海拔最高民用机场四川稻城亚丁机场的基于性能导航(PBN)飞行程序设计过程中,由于GPS在垂直方向精度较低,最后进近航段采用气压垂直导航(Baro-VNAV).但机场海拔高,这种导航方式受到修正高度的影响较大.因此通过对ISA偏差对气压高度的影响公式进行推导,得出修正高度公式,利用Matlab对机场温度、航段高、机场标高与修正高度H修的关系进行分析,并以四川稻城亚丁机场Baro-VNAV实例进行了验证.最终给出了在PBN飞行程序设计过程中的建议.     

地形辅助导航综述

介绍了地形辅助导航原理和系统构成;提供几种适于直升飞机和固定翼飞机的惯性地形辅助导航算法;以及平坦地形上空的地形辅助导航技术,并提供仿真,飞行结果数据。     

Mars Global Surveyor Observations of Solar Wind Magnetic Field Draping Around Mars

We examine the magnetic field in the martian magnetosheath due to solar wind draping. Mars Global Surveyor provided 3-D vector magnetic field measurements at a large range of altitudes, local times, and solar zenith angles as the spacecraft orbit evolved. We choose orbits with very clean signatures of draping to establish the nominal morphology of the magnetic field lines at local times of near-subsolar and near-terminator. Next, using a compilation of data from Mars Global Surveyor, we determine the average magnetic field morphology in the martian magnetosheath due to the solar wind interaction. The topology of the field is as expected from previous observations and predictions. The magnetic field magnitude peaks at low altitude and noon magnetic local time and decreases away from that point. The magnetic field has an inclination from the local horizontal of 5.6° on average in the dayside magnetosheath and 12.5° on the nightside. The inclination angle is closest to zero at noon magnetic local time and low altitude. It increases both upward and to later local times. The magnetic field in the induced magnetotail flares out from the Mars—Sun direction by 21°. Finally, we compare the observations to gasdynamic model predictions and find that the shocked solar wind flow in the martian magnetosheath can be treated as a gasdynamic flow with the magnetic pileup boundary as the inner boundary to the flow.     

涡产生器倾角对换热器内流动与换热特性的影响

为优化涡产生器强化传热的性能,通过改变三角翼式涡产生器的倾角,数值分析了倾角变化对板式换热器通道内流动与换热特性的影响,倾角变化范围为-30°～30°。获得了不同倾角下通道内的纵向涡、涡量分布,换热及阻力特性。结果表明涡产生器倾斜方向对流动与换热的影响不同,存在最佳的涡产生器倾角-10°,使得换热通道内涡产生器强化换热的性能最优;改变倾角可进一步提高涡产生器的强化传热性能,不同倾角对应努塞尔数和热性能评价因子间的最大差值分别达到8.9%和5.7%。     

Global solar magnetic field evolution inferred from geomagnetic variations

I have analyzed geomagnetic disturbance index C9, mean solar magnetic field observed at Stanford Solar Observatory for the interval January 13, 1976 – December 30, 1993. It has been established a good correspondence between high-intensity geomagnetic recurrent and solar magnetic field patterns during whole period analyzed. A surprising thing is that the behavior of the solar mean field and interplanetary medium in the latest two solar cycles is very similar. Geomagnetic activity variations actually could serve as an ecliptic monitor of solar magnetic field structure and its evolution.     

基于弹道模型的磁测系统偏航干扰误差分析

常规弹丸在使用地磁算法测量滚转角的过程中,常将偏航角设为0°解算弹丸滚转角。当弹丸在飞行过程中偏航角发生变化时,滚转角解算精度受到一定影响。针对偏航角变化带来的误差与多种因素有关,且规律不清楚。在建立偏航角误差系数的基础上,使用Matlab软件建立了弹丸在不同偏航角、俯仰角、射向条件下的误差模型。首先建立了横风修正的质点弹道模型,通过蒙特卡罗方法仿真弹丸的轨迹分布,分析了弹载环境下磁测算法的滚转角误差,并验证了误差系数的准确性。通过仿真验证,误差系数可以较准确地表示滚转角误差与偏航角变化之间的关系,误差系数计算的误差与理论误差的差值小于10%,为后续实弹试验做好理论准备。     

The interplanetary magnetic field. Solar origin and terrestrial effects

Many observations related to the large-scale structure of the interplanetary magnetic field, its solar origin and terrestrial effects are discussed. During the period observed by spacecraft the interplanetary field was dominated by a sector structure corotating with the sun in which the field is predominantly away from the sun (on the average in the Archimedes spiral direction) for several days (as observed near the earth), and then toward the sun for several days, etc. The average sector appears to be a coherent entity with internal structure such that its preceding portion is more active than its following portion. Cosmic rays corotate with the interplanetary field, and there are differential flows associated with the sector pattern. Profound effects on geomagnetic activity and the radiation belts are produced as the sector pattern rotates past the earth. The solar origin of the sector pattern is discussed. The solar source may be associated with the large-scale weak background photospheric fields observed with the solar magnetograph. It is suggested that there may be a rather continual relation between this solar structure and terrestrial responses, of which the recurring M-Region geomagnetic storms are just the most prominent example.     

倾斜微槽道热管中纳米流体的应用

为了研究热管倾斜角度和压力对热管蒸发段、冷凝段传热系数以及最大换热功率的影响,对使用水基CuO纳米流体为工质的倾斜微槽道热管强化换热特性进行实验研究.实验装置主要由带角度调节功能的微槽道热管和加热、冷却系统组成.实验结果发现,用水基纳米流体替代去离子水为工质时,热管整体换热特性得到明显增强,蒸发段、冷凝段传热系数以及最大功率都能大幅度提高,总热阻明显降低.倾斜水热管的蒸发段和冷凝段传热系数比水平水热管的有大幅提高,但最大功率变化不大.而倾斜纳米流体热管不但蒸发段和冷凝段传热系数比水平纳米流体热管有大幅提高,而且最大功率更有接近一倍的增加.对水和纳米流体两种工质,对应于最佳换热特性的倾斜角都是75°.因此,纳米流体对倾斜热管有良好的应用前景.      

一种基于雷达波束驻留模式的空间碎片轨道参数估计方法

利用窄波束的单脉冲精密跟踪雷达波束驻留模式进行碎片探测是空间碎片环境统计特征描述的一种重要途径。由于该模式观测弧段极短,且无法获取同一目标的多个弧段,因而利用常规定轨方法难以达到理想的效果。在圆轨道假设下,提出了一种利用波束驻留模式获取的单个极短弧计算碎片轨道高度和倾角的方法。首先利用碎片的距离确定其轨道高度;在此基础上,根据推导出的不同波束指向时碎片的距离变化率与轨道倾角的关系,得出其轨道倾角。该方法对于正南、正东指向的雷达波束驻留模式均适用,其中正南指向时还需利用方位角和仰角数据来区分轨道倾角与补角;但不适用于波束指向天顶的情况。仿真结果验证了方法的有效性。     

Flight trajectory optimization of sun-tracking solar aircraft under the constraint of mission region

The optimal yawing angle of sun-tracking solar aircraft is tightly related to the solar azimuth angle, which results in a large arc flight path to dynamically track the sun position. However, the limited detection range of payload usually requires solar aircraft to loiter over areas of interest for persistent surveillance missions. The large arc sun-tracking flight may cause the target area on the ground to be outside the maximum coverage area of payload. The present study therefore develops an optimal flight control approach for planning the flight path of sun-tracking solar aircraft within a mission region. The proposed method enables sun-tracking solar aircraft to maintain the optimal yawing angle most of the time during daylight flight, except when the aircraft reverses its direction by turning flight. For a circular region with a mission radius of 50 km, the optimal flight trajectory and controls of an example Λ-shaped sun-tracking solar aircraft are investigated theoretically. Results demonstrate the effectiveness of the proposed approach to optimize the flight path of the sun-tracking aircraft under the given circular region while maximizing the battery input power. Furthermore, the effects of varying the mission radius on energy performance are explored numerically. It has been proved that both net energy and energy balance remain nearly constant as the radius constraint varies, which enables the solar aircraft to achieve perpetual flight at almost the same latitude as the large arc flight. The method and results presented in this paper can provide reference for the persistent operation of sun-tracking solar aircraft within specific mission areas.     

基于局部大气偏振特性的仿生导航方法

目前主流的偏振导航算法中，思路通常为通过对全天域偏振图像的获取拟合出太阳子午线或中性点的位置，进而判断导航方向。现提出一种新的导航方向获取算法，可在小视场条件下，通过对太阳方向矢量的拟合判断导航方向。在此基础上进行了计算机仿真和室外实验，利用偏振相机获取了天顶区域大气偏振分布模式；利用斯托克斯矢量分析法解算出了大气偏振模式的分布情况，包括其中偏振度和偏振角的信息，初步证实了解算算法在实际情况下的可行性和精度，导航精度可达到0.2°左右。     

Observations of Vertical Reflections from the Topside Martian Ionosphere

The Martian ionosphere has for the first time been probed by a low frequency topside radio wave sounder experiment (MARSIS) (Gurnett et al., 2005). The density profiles in the Martian ionosphere have for the first time been observed for solar zenith angles less than 48 degrees. The sounder spectrograms typically have a single trace of echoes, which are controlled by reflections from the ionosphere in the direction of nadir. With the local density at the spacecraft derived from the sounder measurements and using the lamination technique the spectrograms are inverted to electron density profiles. The measurements yield electron density profiles from the sub-solar region to past the terminator. The maximum density varies in time with the solar rotation period, indicating control of the densities by solar ionizing radiation. Electron density increases associated with solar flares were observed. The maximum electron density varies with solar zenith angle as predicted by theory. The altitude profile of electron densities between the maximum density and about 170m altitude is well approximated by a classic Chapman layer. The neutral scale height is close to 10 to 13 km. At altitudes above 180 km the densities deviate from and are larger than inferred by the Chapman layer. At altitudes above the exobase the density decrease was approximated by an exponential function with scale heights between 24 and 65 km. The densities in the top side ionosphere above the exobase tends to be larger than the densities extrapolated from the Chapman layer fitted to the measurements at lower altitudes, implying more efficient upward diffusion above the collision dominated photo equilibrium region.