RP-3航空煤油的亚/超临界密度实测和计算方法研究

为了逐步改善高性能空天动力装置研究中液态碳氢燃料物性数据缺乏的现状,设计了一种气动活塞式的密度测量装置,对压力和温度范围分别为1.2~4.0MPa和293~673K的常用液态碳氢燃料——RP-3航空煤油的密度进行了实验测量,并分析了其密度随温度和压力的变化规律。此外,基于PR状态方程进行了真实流体的密度计算,并结合已有的正癸烷(C10H22)密度实验数据对计算过程进行了修正。通过将采用修正后的方法计算出的RP-3航空煤油的密度值与实验测量值进行对比,发现计算值比实验值稍低,尤其在低温阶段和临界点附近。分析认为,这主要是由于此计算方法用于混合物计算时的局限性造成的。     

Coherent matter wave inertial sensors for precision measurements in space

We analyze the advantages of using ultra-cold coherent sources of atoms for matter-wave interferometry in space. We present a proof-of-principle experiment that is based on an analysis of the results previously published in Richard et al. (2003) from which we extract the ratio h/m for ⁸⁷Rb. This measurement shows that a limitation in accuracy arises due to atomic interactions within the Bose–Einstein condensate. Finally we discuss the promising role of coherent-matter-wave sensors, in particular inertial sensors, in future fundamental physics missions in space.     

空间目标可见光相机的成像算法研究与分析

可见光相机可被应用于空间目标监测,其拍摄的图像具有高分辨率、高清晰度和高质量等优点。基于可见光探测器CMV4000获取Bayer格式数据的特点,采用了颜色插值和白平衡等方法,实现了彩色图像的重建。通过对比和分析多种插值方法,选取基于梯度的插值算法和灰度世界法用于工程实现色彩数据的重建。用彩色板等目标在实验室、暗室等场景下对算法进行仿真测试。结果表明：基于梯度的插值方法和白平衡法可以有效地恢复彩色图像,可以在空间环境中获取高质量的彩色图像。     

一种改进的模糊度子集选取方法及其性能评估

模糊度固定(ambiguity resolution, AR)能在一定程度上加快精密单点定位收敛并提高定位精度。但是模糊度固定率和计算效率会随模糊度数量的增加而降低,因此部分模糊度固定(partial ambiguity resolution, PAR)备受关注。PAR技术的关键在于模糊度子集选取,提出了一种改进的模糊度子集选取法,将高度角、信噪比以及模糊度方差联合作为模糊度子集选取的指标。实验结果表明：静态模式下,相比于全模糊度固定(full ambiguity resolution, FAR)和基于高度角的PAR方法,该方法的固定率分别提升9.65%和2.56%,首次固定时间分别缩短6.86%和3.43%,收敛时间分别缩短15.57%和5.13%,当三种方法固定率大致相同时,定位精度分别提升4.74%和5.39%;动态模式下,该方法的固定率分别提升22.75%和0.92%,首次固定时间分别缩短12.44%和0.44%,当三种方法固定率大致相同时,定位精度分别提升3.50%和4.89%。总体而言,无论是在静态还是动态模式下,该方法相比于FAR和基于高度角的PAR方法,性能均有所提升。     

RSSI测距在蓝牙室内定位抗差算法中的应用

蓝牙信号强度在室内环境下易受人员扰动等环境因素影响,从而影响定位精度。基于RSSI测距的蓝牙室内定位原理,将人员等扰动视为异常误差,采用胡贝尔、汉佩尔、IGG和LEGE四种抗差算法,比较分析了不同抗差算法的定位提升效果。试验结果表明,不管有无人员扰动,四种抗差算法均可改善定位精度,其中IGG法定位精度最高,约为3m,且有较好的稳定性。     

Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles,Cosmic Rays,and Magnetic Fields

This paper summarizes the results obtained by the team “Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields” supported by the International Space Science Institute (ISSI) in Bern, Switzerland. We focus on the physical processes occurring in the outer heliosphere, especially at its boundary called the heliopause, and in the local interstellar medium. The importance of magnetic field, charge exchange between neutral atoms and ions, and solar cycle on the heliopause topology and observed heliocentric distances to different heliospheric discontinuities are discussed. It is shown that time-dependent, data-driven boundary conditions are necessary to describe the heliospheric asymmetries detected by the Voyager spacecraft. We also discuss the structure of the heliopause, especially due to its instability and magnetic reconnection. It is demonstrated that the Rayleigh–Taylor instability of the nose of the heliopause creates consecutive layers of the interstellar and heliospheric plasma which are magnetically connected to different sources. This may be a possible explanation of abrupt changes in the galactic and anomalous cosmic ray fluxes observed by Voyager 1 when it was crossing the heliopause structure for a period of about one month in the summer of 2012. This paper also discusses the plausibility of fitting simulation results to a number of observational data sets obtained by in situ and remote measurements. The distribution of magnetic field in the vicinity of the heliopause is discussed in the context of Voyager measurements. It is argued that a classical heliospheric current sheet formed due to the Sun’s rotation is not observed by in situ measurements and should not be expected to exist in numerical simulations extending to the boundary of the heliosphere. Furthermore, we discuss the transport of energetic particles in the inner and outer heliosheath, concentrating on the anisotropic spatial diffusion diffusion tensor and the pitch-angle dependence of perpendicular diffusion and demonstrate that the latter can explain the observed pitch-angle anisotropies of both the anomalous and galactic cosmic rays in the outer heliosheath.     

有无边界层吸入对S弯进气道流动特性的影响

为了深入认识一种吸入大量来流边界层的S弯进气道,在完成其设计的基础上,采用仿真方法对其流动特性展开了研究,并与无边界层吸入的S弯进气道进行了对比。结果表明:由于吸入大量来流边界层,该进气道进口段流场主要受钝体绕流与平板边界层相互干扰作用;在内通道第二弯段后半段,二次流逐渐发展成为对涡,并将堆积在下壁面的低能流卷向截面中间,最终在出口截面的中下半部形成了低总压恢复区。另外,边界层的吸入使得进气道总压恢复系数下降约0.04,且随出口马赫数的升高,总压恢复系数先升高后降低,而在无边界层吸入的S弯进气道中总压恢复系数随之单调降低。     

A high-order SPH method by introducing inverse kernels

The smoothed particle hydrodynamics (SPH) method is usually expected to be an effi-cient numerical tool for calculating the fluid-structure interactions in compressors; however, an endogenetic restriction is the problem of low-order consistency. A high-order SPH method by intro-ducing inverse kernels, which is quite easy to be implemented but efficient, is proposed for solving this restriction. The basic inverse method and the special treatment near boundary are introduced with also the discussion of the combination of the Least-Square (LS) and Moving-Least-Square (MLS) methods. Then detailed analysis in spectral space is presented for people to better under-stand this method. Finally we show three test examples to verify the method behavior.     

旋流器关键参数对双旋流冷态流场特性的影响

为了探究中心分级双旋流燃烧室内冷态流场特性,采用粒子成像测速法PIV(Particle im?age velocimetry)方法进行研究,揭示了值班级与主燃级旋流的相互作用及其对双旋流燃烧室内流场的影响机制,获得了值班级旋流强度、主燃级旋流强度和两级旋流之间的空气比例等旋流器关键参数对燃烧室内流场的影响规律.结果表明...     

THE WAVE EXPERIMENT CONSORTIUM (WEC)

In order to get the maximum scientific return from available resources, the wave experimenters on Cluster established the Wave Experiment Consortium (WEC). The WEC's scientific objectives are described, together with its capability to achieve them in the course of the mission. The five experiments and the interfaces between them are shown in a general block diagram (Figure 1). WEC has organised technical coordination for experiment pre-delivery tests and spacecraft integration, and has also established associated working groups for data analysis and operations in orbit. All science operations aspects of WEC have been worked out in meetings with wide participation of investigators from the five WEC teams.