双补燃室固冲凝聚相颗粒分布对比试验研究

针对固冲发动机燃烧效率较低以及凝相粒子分布规律不清楚的现状,本文建立了一套评价固冲发动机燃烧效率的双补燃室试验装置和研究凝相颗粒分布的取样装置。对比研究了结构相同的补燃室内的参数,其误差小于0.5%,说明该装置可以用于精确对比不同补燃室的燃烧效率。然后应用该装置完成了补燃室长度分别为600mm、800mm、1000mm,进气角度分别为30°、45°、60°的对比试验,分析了粒子的粒度分布规律和化学成分变化规律,该规律与数值分析的规律相同。试验结果表明：在进气角度不变情况下,补燃室长度增加有利于提高燃烧效率,燃烧室压强提高,凝相粒子直径明显减小,B粒子燃烧更充分;在补燃室长度为1000mm的情况下,进气角度增加有利于燃烧效率增加,燃烧室压强提高,粒子直径减小,B粒子燃烧更充分。双补燃室发动机是评价补燃室燃烧效率的有效装置,粒度分布和燃烧产物的化学成分有助于补燃室结构设计。     

In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections

The heliospheric counterparts of coronal mass ejections (CMEs) at the Sun, interplanetary coronal mass ejections (ICMEs), can be identified in situ based on a number of magnetic field, plasma, compositional and energetic particle signatures as well as combinations thereof. We summarize these signatures and their implications for understanding the nature of these structures and the physical properties of coronal mass ejections. We conclude that our understanding of ICMEs is far from complete and formulate several challenges that, if addressed, would substantially improve our knowledge of the relationship between CMEs at the Sun and in the heliosphere.     

Solar Wind Sources and Their Variations Over the Solar Cycle

In this paper I will briefly summarize the present status of our knowledge on the four different sorts of solar wind, their sources and their short- and long-term variations. First: the fast solar wind in high-speed streams that emerges from coronal hole regions. Second: the slow solar wind emerging from the non-active Sun near the global heliospheric current sheet above helmet streamers and underlying active regions. Third: the slow solar wind filling most of the heliosphere during high solar activity, emerging above active regions in a highly turbulent state, and fourth: the plasma expelled from the Sun during coronal mass ejections. The coronal sources of these different flows vary dramatically with the solar activity cycle.     

相变材料容器的瞬态热分析

空间太阳能热动力发电系统是很有前途的空间电源系统。基于微重力状态下的导热控制微分方程，采用焓法对相变材料容器进行了二维数值分析，改进了以往的模拟计算，对计算结果给予了讨论。     

GEO轨道兆瓦级空间太阳能电站接收整流技术研究

依据中国空间太阳能电站建设中远期规划和技术发展水平,预估兆瓦级电站发射天线口径为200 m左右,并根据收发天线口径尺寸的约束关系以与接收天线口径相关的波束收集效率和构建成本之间的矛盾为问题导向,通过研究不同口径的接收天线口面上功率密度分布,分析与之匹配的后端整流电路需求,给出了接收天线口径的优选过程。研究结果表明5 km为较合理的兆瓦级电站接收天线设计建设指标,且在整个接收整流阵列中仅需同一种整流器件,同样整流电路即可实现较高的整流效率,为实现兆瓦级空间太阳能电站（Space solar power satellite,SSPS）的演示验证系统论证提供了技术支撑。最后以此为基础研究了整流电路的设计实现,给出了适用于较低输入功率密度下提高整流效率的技术途径。     

模块化多旋转关节空间太阳能电站方案设计

文章基于多旋转关节空间太阳能电站(MR-SPS)方案,以降低远距离高压电力传输技术难度为核心,提出一种更新的模块化多旋转关节空间太阳能电站概念。该方案在分布式太阳电池分阵和多导电旋转关节基础上,对于微波发射天线阵也进行了模块化设计和分布式布局,实现了太阳电池分阵和微波发射天线分阵的一一对应,形成多个独立的太阳能发电与能量传输模块,通过模块的扩展实现整个空间太阳能电站。该方案大幅简化了空间电力传输与管理的复杂性和在轨组装的难度。同时各个模块完全独立,组装后即可单独工作,也提高了系统的可靠性。     

不同形貌Ni颗粒对向列相液晶电光性能的影响

将不同形貌的Ni颗粒(类碗状Ni颗粒、Ni花颗粒和Ni球颗粒)掺杂在液晶中制备了扭曲向列相(TN)液晶显示模式液晶盒,采用液晶综合参数测试仪对掺杂不同形貌Ni颗粒的向列相液晶(NLC)显示模式液晶盒的阈值电压、饱和电压、对比度及响应时间进行了研究。结果表明,掺杂Ni颗粒后,液晶的电光性能得到明显改善,阈值电压、饱和电压均有所降低,对比度明显增大,响应时间下降。其中类碗状Ni颗粒改善效果最为明显,驱动电压降幅达到13.77%,对比度增大35.55%,响应时间降低至9.390 ms。Ni颗粒的形貌及比表面积对液晶的电光性能有很大影响。比表面积及曲率大的Ni颗粒对液晶电光性能的改善效果好。      

太阳帆航天器的关键技术

将太阳帆航天器所涉及的关键技术划分为4个方面：总体设计、轨道和姿态动力学与控制、太阳帆材料及其性能、太阳帆折叠与展开。针对每项关键技术,基于对国外长期研究结果进行分析并阐述主要技术特征,梳理国内相关研究进展,包括笔者与合作者的研究成果,分析存在的主要问题。根据上述分析,指出我国发展太阳帆航天器应该重视的若干问题。     

Solar energetic particle events during the rise phases of solar cycles 23 and 24

We present a comparative study of the properties of coronal mass ejections (CMEs) and flares associated with the solar energetic particle (SEP) events in the rising phases of solar cycles (SC) 23 (1996–1998) (22 events) and 24 (2009–2011) (20 events), which are associated with type II radio bursts. Based on the SEP intensity, we divided the events into three categories, i.e. weak (intensity < 1 pfu), minor (1 pfu < intensity < 10 pfu) and major (intensity ? 10 pfu) events. We used the GOES data for the minor and major SEP events and SOHO/ERNE data for the weak SEP event. We examine the correlation of SEP intensity with flare size and CME properties. We find that most of the major SEP events are associated with halo or partial halo CMEs originating close to the sun center and western-hemisphere. The fraction of halo CMEs in SC 24 is larger than the SC 23. For the minor SEP events one event in SC23 and one event in SC24 have widths < 120° and all other events are associated with halo or partial halo CMEs as in the case of major SEP events. In case of weak SEP events, majority (more than 60%) of events are associated with CME width < 120°. For both the SC the average CMEs speeds are similar. For major SEP events, average CME speeds are higher in comparison to minor and weak events. The SEP event intensity and GOES X-ray flare size are poorly correlated. During the rise phase of solar cycle 23 and 24, we find north–south asymmetry in the SEP event source locations: in cycle 23 most sources are located in the south, whereas during cycle 24 most sources are located in the north. This result is consistent with the asymmetry found with sunspot area and intense flares.     

Simulation of ASTROD I test mass charging due to solar energetic particles and interplanetary electrons

As ASTROD I travels through space, its test mass will accrue charge due to exposure of the spacecraft to high-energy particles. This test mass charge will result in Coulomb forces between the test mass and the surrounding electrodes. In earlier work, we have used the GEANT 4 toolkit to simulate charging of the ASTROD test mass due to cosmic-ray protons of energies between 0.1 and 1000 GeV at solar maximum and at solar minimum. Here we use GEANT 4 to simulate the charging process due to solar energetic particle events and interplanetary electrons. We then estimate the test mass acceleration noise due to these fluxes. The predicted charging rates range from 2247 e⁺/s to 47,055 e⁺/s, at peak intensity, for the four largest SEP events in September and October 1989. Although the noise due to charging exceeds the ASTROD I budget for the two larger events, it can be suppressed through continuous discharging. The acceleration noise during the two small events is well below the design target. The charging rate of the ASTROD I test mass due to interplanetary electrons in this simulation is about −11% of the cosmic-ray protons at solar minimum, and over −37% at solar maximum. In addition to the Monte Carlo uncertainty, an error of ±30% in the net charging rates should be added to account for uncertainties in the spectra, physics models and geometry implementations.