低速通用飞机机翼低成本精细化设计

针对低速通用飞机升阻特性的低成本精细化设计,通过合理地简化模型,建立了一种将翼型升阻比曲线斜率作为附加设计约束的机翼工程优化设计方法。基于该优化设计方法,利用低成本快速设计分析工具开展了优化设计,并对设计方法及结果进行了风洞试验验证。试验结果表明,所提方法能够有效提高机翼最大升阻比,同时使最大升阻比对应的升力系数逼近巡航工况,进一步挖掘了低速通用飞机的经济性潜力。     

Improvement of the GRACE star camera data based on the revision of the combination method

The new release of the sensor and instrument data (Level-1B release 02) of the Gravity Recovery and Climate Experiment (GRACE) had a substantial impact on the improvement of the overall accuracy of the gravity field models. This has implied that improvements on the sensor data level can still significantly contribute to arriving closer to the GRACE baseline accuracy. The recent analysis of the GRACE star camera data (SCA1B RL02) revealed their unexpectedly higher noise. As the star camera (SCA) data are essential for the processing of the K-band ranging data and the accelerometer data, thorough investigation of the data set was needed. We fully reexamined the SCA data processing from Level-1A to Level-1B with focus on the combination method of the data delivered by the two SCA heads. In the first step, we produced and compared our own combined attitude solution by applying two different combination methods on the SCA Level-1A data. The first method introduces the information about the anisotropic accuracy of the star camera measurement in terms of a weighing matrix. This method was applied in the official processing as well. The alternative method merges only the well determined SCA boresight directions. This method was implemented on the GRACE SCA data for the first time. Both methods were expected to provide optimal solution characteristic by the full accuracy about all three axes, which was confirmed. In the second step, we analyzed the differences between the official SCA1B RL02 data generated by the Jet Propulsion Laboratory (JPL) and our solution. SCA1B RL02 contains systematically higher noise of about a factor 3–4. The data analysis revealed that the reason is the incorrect implementation of algorithms in the JPL processing routines. After correct implementation of the combination method, significant improvement within the whole spectrum was achieved. Based on these results, the official reprocessing of the SCA data is suggested, as the SCA attitude data are one of the key observations needed for the gravity field recovery.     

梯形翼高升力构型的数值模拟技术

基于雷诺平均Navier-Stokes(RANS)方程和结构网格技术,采用亚跨超声速平台(TRIP3.0),数值模拟了美国国家航空航天局(NASA)梯形翼构型。研究了控制方程、网格密度、流动转捩和初始条件等不同影响因素对气动特性的影响。风洞试验是2002年在NASA Langley 14ft×22ft亚声速风洞中完成的,试验结果包括了基本气动力和力矩、表面压力系数和边界层速度型分布。计算结果与试验数据的比较表明:求解完全的RANS方程,提高了翼梢涡的模拟精度;网格密度主要影响翼梢涡的强度;转捩模型提高了边界层的模拟精度,进而提高了升力系数、俯仰力矩系数的模拟精度;最大升力系数及失速迎角对初始条件具有依赖性。     

多任务使命平台上电子设备发展趋势研究

通过对侦察、对抗和打击一体化系统在现代战争中的地位与作用的介绍,分析了多任务使命平台上各种电子设备之间的冲突,提出了在多任务使命平台上综合电子设备的发展趋势,在此基础上得出几点启示.     

γ-Re_θ转捩模型的标定研究

介绍了γ-Reθ转捩模型,补充了相应的关联函数。基于平板的试验数据在中国空气动力研究与发展中心(CARDC)的trip软件平台上对该关联函数进行了标定,并研究了关联函数的变化对转捩结果的影响规律。通过修正与SST湍流模型的结合,改进了转捩位置后壁面摩擦阻力系数偏低的状况。     

地月系低能转移轨道设计

分析了不同转移轨道间的性能指标,以黄道面与白道面交线作为庞加莱截面实现不同系统轨道的拼接,利用其中耗能最小的日地系稳定流形和地月系的不稳定流形设计了一条低能耗转移轨道.最后对不同轨 道进行了能量分析和对比,优化了国内提出的低能探月轨道.仿真结果表明,文中方法比直接通过霍曼转移节约21.1%的能量,对探月工程的轨道设计具...     

基于FPGA的IP over CCSDS设计与实现

首先介绍了TCP/IP(传输控制协议/网际协议)技术和CCSDS(空间数据系统咨询委员会)建议的应用背景,从天地网络一体化和未来空间站与地面交互式通信系统需求的角度出发,提出了一种基于FPGA(现场可编程门阵列)的IP over CCSDS处理方法。详细描述了IP over CCSDS软件的实现方案和技术特点,并对其进行了测试和结果分析。     

Turbo码块同步参数优化设计

在信道码码块同步技术研究的基础上,针对CCSDS(空间数据系统咨询委员会)建议规定的Turbo码,为不同码块长度、不同编码效率的Turbo码设计一组最佳同步参数,以最优化平均入锁时间和数据有效率。利用理论推导出的解析公式,计算不同参数下的平均入锁时间和数据有效率,从而优选出最佳同步参数,并归纳总结最佳同步参数的特点。本文得到的同步参数可为实际工程提供参考。     

Numerical simulations of the regional characteristics of dust transport on Mars

Using a Martian general circulation model (GCM), regions favorable for expansion of dust storms on Mars are identified. Dust transport simulations for the northern fall provide global maps of dust expansibility. These global maps show that dust injected from certain areas in the northern mid-latitudes tends to spread widely within a few days. The high expansibility of dust in such areas results from thermal tides, baroclinic waves, and quasi-stationary disturbances. Dust injected into the vast regions around Tharsis and the Sirenum–Aonia regions also tends to spread extensively. However, dust expansion around these two regions largely depends on the local time of dust injection. On the other hand, dust injected at high latitudes in either hemisphere does not spread extensively. Such global maps indicating regions favorable for dust storm expansion are a clue to understanding the expansion processes and climatology of great dust storms on Mars.     

X-Rays From Mars

X-rays from Mars were first detected in July 2001 with the satellite Chandra. The main source of this radiation was fluorescent scattering of solar X-rays in its upper atmosphere. In addition, the presence of an extended X-ray halo was indicated, probably resulting from charge exchange interactions between highly charged heavy ions in the solar wind and neutrals in the Martian exosphere. The statistical significance of the X-ray halo, however, was very low. In November 2003, Mars was observed again in X-rays, this time with the satellite XMM-Newton. This observation, characterized by a considerably higher sensitivity, confirmed the presence of the X-ray halo and proved that charge exchange is indeed the origin of the emission. This was the first definite detection of charge exchange induced X-ray emission from the exosphere of another planet. Previously, this kind of emission had been detected from comets (which are largely exospheres) and from the terrestrial exosphere. Because charge exchange interactions between atmospheric constituents and solar wind ions are considered as an important nonthermal escape mechanism, probably responsible for a significant loss of the Martian atmosphere, X-ray observations may lead to a better understanding of the present state of the Martian atmosphere and its evolution. X-ray images of the Martian exosphere in specific emission lines exhibited a highly anisotropic morphology, varying with individual ions and ionization states. With its capability to trace the X-ray emission out to at least 8 Mars radii, XMM-Newton can explore exospheric regions far beyond those that have been observationally explored to date. Thus, X-ray observations provide a novel method for studying processes in the Martian exosphere on a global scale.