转台中心轴线标定误差分析与修正

提出一种标定球和几何变换相结合的方法修正三维激光数字化系统中转台中心轴线的标定误差.该方法首先用8个不同旋转位置的标定球球心计算转台中心轴线,然后利用几何变换将不同位置的球心绕转台中心轴线旋转到零度位置,并计算与初始位置球心的偏差,依据不同位置球心旋转复位的偏差采用几何逆变换推导出转轴偏心的修正公式.在自行设计的三维激光线扫描测量平台上数据旋转拼合精度提高到0.07?mm,实现了多视旋转测量的数据点云在线自动拼合.与以前的方法相比,设计的转轴标定误差修正方法简单、高效,在其它安装转台的测量系统中同样适用.     

The Rotation and Interior Structure Experiment on the InSight Mission to Mars

The Rotation and Interior Structure Experiment (RISE) on-board the InSight mission will use the lander’s X-band (8 GHz) radio system in combination with tracking stations of the NASA Deep Space Network (DSN) to determine the rotation of Mars. RISE will measure the nutation of the Martian spin axis, detecting for the first time the effect of the liquid core of Mars and providing in turn new constraints on the core radius and density. RISE will also measure changes in the rotation rate of Mars on seasonal time-scales thereby constraining the atmospheric angular momentum budget. Finally, RISE will provide a superb tie between the cartographic and inertial reference frames. This paper describes the RISE scientific objectives and measurements, and provides the expected results of the experiment.     

Presolar Isotopic Signatures in Meteorites and Comets: New Insights from the Rosetta Mission to Comet 67P/Churyumov–Gerasimenko

Comets are considered the most primitive planetary bodies in our Solar System, i.e., they should have best preserved the solid components of the matter from which our Solar System formed. ESA’s recent Rosetta mission to Jupiter family comet 67P/Churyumov–Gerasimenko (67P/CG) has provided a wealth of isotope data which expanded the existing data sets on isotopic compositions of comets considerably. In this paper we review our current knowledge on the isotopic compositions of H, C, N, O, Si, S, Ar, and Xe in primitive Solar System materials studied in terrestrial laboratories and how the Rosetta data acquired with the ROSINA (Rosetta Orbiter Sensor for Ion and Neutral Analysis) and COSIMA (COmetary Secondary Ion Mass Analyzer) mass spectrometer fit into this picture. The H, Si, S, and Xe isotope data of comet 67P/CG suggest that this comet might be particularly primitive and might have preserved large amounts of unprocessed presolar matter. We address the question whether the refractory Si component of 67P/CG contains a presolar isotopic fingerprint from a nearby Type II supernova (SN) and discuss to which extent C and O isotope anomalies originating from presolar grains should be observable in dust from 67P/CG. Finally, we explore whether the isotopic fingerprint of a potential late SN contribution to the formation site of 67P/CG in the solar nebula can be seen in the volatile component of 67P/CG.     

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

After 25 years of laboratory research on protoplanetary dust agglomeration, a consistent picture of the various processes that involve colliding dust aggregates has emerged. Besides sticking, bouncing and fragmentation, other effects, like, e.g., erosion or mass transfer, have now been extensively studied. Coagulation simulations consistently show that \(\upmu\mbox{m}\)-sized dust grains can grow to mm- to cm-sized aggregates before they encounter the bouncing barrier, whereas sub-\(\upmu\mbox{m}\)-sized water-ice particles can directly grow to planetesimal sizes. For siliceous materials, other processes have to be responsible for turning the dust aggregates into planetesimals. In this article, these processes are discussed, the physical properties of the emerging dusty or icy planetesimals are presented and compared to empirical evidence from within and without the Solar System. In conclusion, the formation of planetesimals by a gravitational collapse of dust “pebbles” seems the most likely.     

Nucleosynthesis in Supernovae

We present the status and open problems of nucleosynthesis in supernova explosions of both types, responsible for the production of the intermediate mass, Fe-group and heavier elements (with the exception of the main s-process). Constraints from observations can be provided through individual supernovae (SNe) or their remnants (e.g. via spectra and gamma-rays of decaying unstable isotopes) and through surface abundances of stars which witness the composition of the interstellar gas at their formation. With a changing fraction of elements heavier than He in these stars (known as metallicity) the evolution of the nucleosynthesis in galaxies over time can be determined. A complementary way, related to gamma-rays from radioactive decays, is the observation of positrons released in \(\beta^{+}\)-decays, as e.g. from \(^{26}\mbox{Al}\), \(^{44}\mbox{Ti}\), \(^{56,57}\mbox{Ni}\) and possibly further isotopes of their decay chains (in competition with the production of \(e^{+}e^{-}\) pairs in acceleration shocks from SN remnants, pulsars, magnetars or even of particle physics origin). We discuss (a) the role of the core-collapse supernova explosion mechanism for the composition of intermediate mass, Fe-group (and heavier?) ejecta, (b) the transition from neutron stars to black holes as the final result of the collapse of massive stars, and the relation of the latter to supernovae, faint supernovae, and gamma-ray bursts/hypernovae, (c) Type Ia supernovae and their nucleosynthesis (e.g. addressing the \(^{55}\mbox{Mn}\) puzzle), plus (d) further constraints from galactic evolution, \(\gamma\)-ray and positron observations. This is complemented by the role of rare magneto-rotational supernovae (related to magnetars) in comparison with the nucleosynthesis of compact binary mergers, especially with respect to forming the heaviest r-process elements in galactic evolution.     

翼型波浪水面巡航地面效应数值模拟

数值求解非定常不可压缩流动的雷诺平均N-S(Navier-Stokes)方程和标准k-ε湍流模型,用VOR(Volume Of Fluid)方法模拟波浪水面,模拟了NACA2410翼型在波浪水面上方飞行的流场.研究了余弦波浪水面的生成方法,选取合适的计算网格和时间步长,避免了在生成规则余弦波浪水面时由于数值耗散使波面形状衰减.比较了固壁波浪与水面波浪计算结果的差异,发现固壁波浪的结果更接近余弦曲线分布.研究了波浪等级对翼型气动性能的影响,分析计算结果发现:在规则的余弦水面波浪上方飞行,翼型气动力呈现周期性,给出了一个周期内气动力的变化过程,以及波长和波幅对气动力平均值和波动幅度的影响规律.      

小卫星太阳电池阵结构声振响应分析研究

针对高频段太阳电池阵结构声振问题求解中的结构模态参数不确定性,文章从统计模态和能量平衡的角度出发,深入研究了复合材料面板太阳电池阵夹层结构的统计能量分析参数确定及功率流模型创建方法,并快速得到了太阳电池夹层结构的声振响应。对比分析与试验结果,发现二者吻合很好,因而验证了该声振响应分析方法用于小卫星太阳电池阵结构的有效性,并可作为小卫星工程研制中太阳电池阵结构动力学分析的有益补充。     

基于增量式路标表观学习的移动机器人定位

在全景图像中,机器人参考定位的路标表观受到畸变、观察视角、路标尺度变化以及环境亮度的影响,致使基于全景视觉的机器人自主定位存在着许多难点有待解决.提出增量式的路标表观学习方法,准确估计路标的表观变化,并为基于粒子滤波的机器人定位过程提供准确的观测信息.增量式路标学习过程利用增量式概率主元分析为理论工具,将不同视角的路标表观的主元特征表示成不断自主更新的特征基底,为计算观测量与路标真实表观的相似度提供了实现途径和理论依据.该学习算法能够被集成到带有重采样的贯序权值采样粒子滤波算法过程中,实现了全景视觉机器人的精确自主定位.实验结果表明:该算法的定位误差小,计算量小,执行效率高,对全景图像中的各类干扰均不敏感.     

干涉型光纤安防系统偏振误差机理分析

对应用于安全防范、石油管道监测的双马赫-曾德型光纤安防系统的结构及工作原理进行分析.针对现场测试结果,分析了影响系统精度的误差因素,提出影响系统精度和增加误报率主要是由于偏振态变化不一致导致的两路干涉信号幅值波动以及附加相位噪声引入的距离定位误差.并展开对系统偏振衰落形成机理及其主要影响因素的定量定性分析,同时建立数学模型,进行仿真计算.最后通过对双马赫-曾德型光纤安防系统样机进行实验,验证了分析结果的正确性.