高精度航天器微振动力学环境分析

高精度航天器由于其指向精度和分辨率水平极高,需要考虑微振动的影响。文章给出了微振动的定义,分析了微振动特性、国外研究现状、建模特点及方法,总结归纳了高精度航天器星体内部的主要扰动源。给出了反作用轮、斯特林低温制冷器、星载敏感器以及太阳翼等典型扰动源扰动的时域或频域模型及微振动隔离模型,并进行了相应的仿真,从系统层面评估了微振动对高精度航天器性能的影响,可供高精度航天器设计时参考。     

激光辐照充压壳体的破坏评价(Ⅱ)——局部热载作用下断裂参数的分布特性

在激光辐照充压壳体的破坏评价中,需确定断裂参数的分布类型及相关的分布参数.壳体材料的断裂韧性KIC是评估模型中对破坏结果有重要影响的断裂参量.因此,以壳体材料30CrMnSiNi2A的KIC为主要研究对象,利用数理统计的方法,对其相关分布特性进行了研究.首先,根据提供的样本,对于断裂参数的分布类型,利用Shapiro-Wilk W检验和正态概率纸检验,表明断裂参数的分布服从正态分布.其次,对于分布类型的数字特征,利用参数估计的方法给出了点估计结果,同时对估计精度及相关的最小样本容量进行了分析.这些问题为了解评估数据的可信程度提供了基础,同时也可为实验室数据处理提供了参考.     

航天器太阳电池阵分流技术研究

对航天器太阳电池阵分流技术进行了归纳总结,对PWM,S3R和S4R三种开关分流调节技术进行了详细的原理分析,比较总结各自的技术特点。并对S3R和S4R技术进行了深入研究,对S3R技术进行了详细的设计与计算,对S4R技术典型工况进行了详细分析与实验验证。同时对三种开关分流技术做出了评价。     

Photoelectron flux variations observed from the FAST satellite

This paper examines high resolution (ΔE/E = 0.15) photoelectron energy spectra from 10 eV to 1 keV, created by solar irradiances between 1.2 and 120 nm. The observations were made from the FAST satellite at ∼3000 km, equatorward of the auroral oval for the July–August, 2002 solar rotation. These data are compared with the solar irradiance observed by the Solar EUV Experiment (SEE) on the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite and fluxes calculated using the Field Line Interhemispheric Plasma (FLIP) code. The 41 eV photoelectron flux, which corresponds to solar EUV fluxes near 20 nm, shows a clear solar rotation variation in very good agreement with the EUV flux measurements. This offers the possibility that the 41 eV photoelectron flux could be used as a check on measured solar EUV fluxes near 20 nm. Because of unexpected noise, the solar rotation signal is not evident in the integral photoelectron flux between 156 and 1000 eV corresponding to EUV wavelengths between 0.1 and 7 nm measured by the SEE instrument. Examination of daily averaged photoelectron fluxes at energies between 25 and 500 eV show significant changes in the photoelectron spectra in response X and M class flares. The intensity of photoelectrons produced in this energy region is primarily due to two very narrow EUV wavelength regions at 2.3 and 3 nm driving Auger photoionization in O at 500 eV and N₂ at ∼360 eV. Comparison of calculated and daily averaged electron fluxes shows that the HEUVAC model solar spectrum used in the FLIP code does not reproduce the observed variations in photoelectron intensity. In principle, the 21 discrete photoelectron energy channels could be used to improve the reliability of the solar EUV fluxes at 2.3 and 3 nm inferred from broad band observations. In practice, orbital biases in the way the data were accumulated and/or noise signals arising from natural and anthropogenic longitudinally restricted sources of ionization complicate the application of this technique.     

被动式太阳房在河北农村推广的探讨

本文在介绍太阳房概念的基础上,通过调查和分析河北农村住房情况、家庭规模、收入水平和能接受的新房造价,设计了符合河北农村现状的单层被动式太阳房,并进行了相应的热工计算和造价分析。结果表明,在不显著增加造价的前提下,节能率均达到了70%以上,从技术和经济的角度论证了被动式太阳房在河北农村推广的可行性。     

零重力试验装置对太阳翼展开影响分析

文章建立了太阳翼与展开试验装置的联合分析模型,与试验结果进行了对比,通过仿真得出摩擦、横导轨质量、横导轨变形是影响展开时间和展开末角速度的主要因素,为此提出了试验装置的改进建议,即采用空气轴承减小摩擦,横导轨使用密度小、模量高的碳纤维复合材料。     

一种基于太阳震荡时间延迟量测的自主天文导航方法

太阳震荡可以在短时间内引起太阳光强度和光谱线心波长的剧烈变化,通过探测太阳光强度和光谱线心波长并记录时间,可以获得直接接收的太阳光到达时间和经天体反射的太阳光到达时间之间的时间延迟,可以利用时间延迟作为量测量提供航天器的位置信息。提出了一种基于太阳震荡时间延迟量测的自主天文导航方法;建立了基于时间延迟的隐式量测模型,并应用了IUKF方法。仿真结果表明：本文所提出的导航方法,应用在转移轨道上的位置误差和速度误差分别约为3.55 km和0.077 m/s,环绕轨道分别为1.76 km和1.57 m/s。同时也研究了3种因素对导航性能的影响。     

太阳辐射对ER3BP拉格朗日点的影响

为了研究Halo轨道中继通信以及行星际轨道转移等问题,需要首先对拉格朗日点(平动点)的理论进行分析。使用考虑太阳辐射的椭圆型限制性三体建模,代替原有的圆型限制性三体建模,提高了建模的精度。提出了在L1,L2,L3点的更为精确的新解析解,经过Matlab仿真,其相对于精确数值解的误差,分别为Ammar的解析解的13.13%,29.51%,0.46%。     

On the early phase of relativistic solar particle events: Are there signatures of acceleration mechanism?

Many physical processes precede and accompany the solar energetic particles (SEP) occurrence on the Earth’s orbit. Explosive energy release on the Sun gives rise to a flare and a coronal mass ejection (CME). X-ray and gamma emissions are believed to be connected with flares. Radio emission is signature of disturbances traveling through the corona and interplanetary space. Particles can gain energy both in the flare and the accompanying wave processes. The beginning of the SEP events has the advantage of being the phase most close to the time of acceleration. Influence of interplanetary transport is minimal in the case of first arriving relativistic solar protons recorded by ground based neutron monitors in so called ground-level enhancements (GLE). The early phase of the SEP events attracts attention of many scientists searching for the understanding of particle acceleration. However, they come to the opposite conclusions. While some authors find arguments for coronal mass ejections as a sole accelerator of SEPs, others prove a flare to be the SEP origin. Here, the circumstances of SEP generation for several GLEs of the 23rd solar cycle are considered. Timing of X-ray, CME, and radio emissions shows a great variety from event to event. However, the time of particle ejection from the Sun is closer to maximum of X-ray emission than to any other phenomena considered. No correlation is found between the particle fluxes and the CME characteristics.     

推进剂通道结构对太阳热发动机影响数值研究

运用数值模拟方法,通过改变推力室螺旋通道结构参数,对太阳热发动机(STP)能进行了详细的研究,深入分析了STP的推力,比冲、质量流量变化情况,得出了一般情况下螺旋通道的长度,宽度参数范围,同时比较了单、双通道的优缺点,所得的结论对STP推力室/热吸收室推进剂加热通道结构设计具有指导意义.