故障容错光交叉通道数据链路的可靠性

光交叉通道数据链路(OCCDL)是光传飞行控制系统余度计算机之间进行数据交换的重要途径.为了提高OCCDL系统的可靠性,提出一种新的具有多链路故障容错能力的OCCDL系统.给出了该OCCDL系统的结构配置,分析了系统正常工作和故障工作情况下的工作流程,设计了系统光开关故障、光链路等关键部分的故障容错逻辑,建立了基于马尔...     

Influence of the Interplanetary Magnetic Field on the Solar Wind Flow about Planetary Obstacles

The main effects caused by the interplanetary magnetic field (IMF) are analyzed in cases of supersonic solar wind flow around magnetized planets (like Earth) and nonmagnetized (like Venus) planets. The IMF has a relatively weak strength in the solar wind but it is enhanced considerably in the so-called plasma depletion layer or magnetic barrier in the vicinity of the streamlined obstacle (magnetopause of a magnetized planet, or ionopause of a nonmagnetized planet). For magnetized planets, the magnetic barrier is a source of free magnetic energy for magnetic reconnection in cases of large magnetic shear at the magnetopause. For nonmagnetized planets, mass loading of the ionospheric particles is very important. The new created ions are accelerated by the electric field related to the IMF, and thus they gain energy from the solar wind plasma. These ions form the boundary layer within the magnetic barrier. This mass loading process affects considerably the profiles of the magnetic field and plasma parameters in the flow region.     

基于F代表点的高斯过程矩匹配滤波

提出了一种基于F偏差代表点的高斯过程矩匹配滤波方法。该方法通过高斯过程学习系统的过程函数和观测函数,在高斯矩匹配滤波的框架下利用F偏差代表点进行数值计算。在单变量非线性模型及静基座初始对准中进行的仿真实验表明,该方法的精度不低于解析计算的高斯过程假设密度滤波（GP-ADF）,远高于高斯过程无迹卡尔曼滤波（GP-UKF）。     

基于结构随机跳变系统的制导交班边界设计

为了减小最终脱靶量,研究了系统存在随机扰动时交班切换边界定位问题。首先建立了具有中制导和末制导的结构随机跳变系统模型,然后根据结构随机跳变系统理论进行系统概率分析,并在此基础上结合优化算法,得到最优的交班切换边界,使得当前脱靶量的数学期望和方差最小。最后,进行了某型导弹纵向俯仰通道仿真,验证了该方法的有效性。     

Origin and stability of lunar polar volatiles

Temperature regime at the LCROSS impact site is studied. All detected species in the Cabeus crater as well as CH₄ and CO clathrate hydrates except H₂, CO, and CH₄ are stable against evaporation at the LCROSS impact site. CO and CH₄ can be chemisorbed at the surface of the regolith particles and exist in the form of clathrate hydrates in the lunar cold traps. Flux rates of delivery of volatile species by asteroids, micrometeoroids, O-rich, C-rich, and low-speed comets into the permanently shadowed regions are estimated. Significant amounts of H₂O, CO, H₂, H₂S, SO₂, and CO₂ can be impact-produced during collisions between asteroids and O-rich comets with the Moon while CH₃OH, NH₃ and complex organic species survive during low-speed comet impacts as products of disequilibrium processes. C-rich comets are main sources of CH₄, and C₂H₄.     

三能级原子和两个压缩态光场多光子相互作用中的量子效应

本文研究了具有A型跃迁结构的三能级原子与两个压缩态光场多光子相互作用过程中的一些量子效应。通过数值计算得到不同参数条件下原子能级布居数反转的时间特性,光场平均光子数及其统计性质的时间演化,并讨论了多光子过程对加深光场压缩状态的影响。计算结果表明,多光子相互作用使系统的基本Rabi振荡频率增大,崩坍—复原持续期缩短,Mandel参数的改变加剧,光场的压缩增强。     

Effects of the position of the solar wind termination shock and the heliopause on the heliospheric modulation of cosmic rays

The effects of changing the position of the solar wind termination shock and the position of the heliopause, and therefore the extent of the heliosheath, on the modulation of cosmic ray protons are illustrated. An improved numerical model with diffusive termination shock acceleration, a heliosheath and drifts is used. The modulation is computed in the equatorial plane and at 35 heliolatitude using recently derived diffusion coefficients applicable to a number of cosmic ray species during both magnetic polarity cycles of the Sun. It was found that qualitatively the modulation results for the different heliopause positions are similar although they differ quantitatively, e.g., clearly different radial gradients are predicted for the regions beyond the termination shock compared to inside the shock. The difference between the modulation for the two solar polarity cycles are less significant at a heliolatitude of 35° than in the equatorial plane. We found that moving the termination shock from 90 to 100 AU, with the heliopause fixed at 120 AU, caused only quantitative differences so that the exact position of the TS in the outer heliosphere seems not crucially important to global modulation. Moving the heliopause outwards, to represent the modulation in the tail region of the heliosphere, causes overall decreases in the cosmic ray intensities but not linearly as a function of energy, e.g., at 1 GeV the effect is insignificant. We conclude from this modelling that the modulation of protons in the heliospheric nose and tail regions are qualitatively similar although, clear quantitative and interesting differences occur.     

能量包线随机平均法在双线性迟滞系统随机响应分析中的应用

 本文将能量包线随机平均法应用于分析单自由度双线性迟滞系统对白噪声激励的随机响应,详细分析了位移、速度及总能量的平稳响应各统计量随系统粘性阻尼、次斜率及激励强度的变化。解析结果与数字模拟结果比较表明,该方法优于迄今为止用于双线性迟滞系统随机响应分析的其他近似方法。     

New results on planetary lightning

We present the latest observations from spacecraft and ground-based instruments in search for lightning activity in the atmospheres of planets in the solar system, and put them in context of previous research. Since the comprehensive book on planetary atmospheric electricity compiled by Leblanc et al. (2008), advances in remote sensing technology and telescopic optics enable detection of additional and new electromagnetic and optical emissions, respectively. Orbiting spacecraft such as Mars Express, Venus Express and Cassini yield new results, and we highlight the giant storm on Saturn of 2010/2011 that was probably the single most powerful thunderstorm ever observed in the solar system. We also describe theoretical models, laboratory spark experiments simulating conditions in planetary mixtures and map open issues.     

The Iapetus’s ridge: Possible explanations of its origin

Images from the Cassini mission show the existence of a long ridge on Iapetus. It extends at least 1400 km along the great circle defined by the equator. We discuss the possibility that the ridge is a result of extensional forces acting above an ascending current of solid-state convection. A two-cell pattern of convection is a reasonable explanation of the observed feature. Three scenarios of the ridge formation are proposed: spin–orbit resonance scenario, convection in low viscosity-interior scenario, and impact generating flow scenario.