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.     

大长细比反射镜侧面支撑结构设计与分析

随着近几年离轴三反(Three-Mirror Anastigmat,TMA)相机在大视场高分辨率成像领域的应用,大长细比反射镜的支撑技术成为离轴TMA相机研制的关键技术之一。文章研究的反射镜尺寸达到986mm×246mm,为了使大长细比反射镜的支撑结构同时满足高刚度和高面形稳定的要求,采用理论研究和有限元分析相结合的方法设计了一种侧面柔性支撑结构。分析结果表明,反射镜组件一阶频率达到114.9Hz,在重力和2℃温变耦合下综合面形变化均方根值只有4.9nm,工艺件的力学振动试验结果和仿真分析基本吻合,反射镜支撑结构设计合理,满足空间应用要求。     

雷达射频掩护信号分析及对抗方法研究

为提高抗干扰能力,雷达采用射频掩护信号对抗有源干扰机.分析射频掩护信号的产生机理和工作波形,以及射频掩护信号对雷达有源干扰机中测频接收机、信号处理机、数字射频存储器及脉冲行波管发射机的影响,从而给出雷达有源干扰机对抗射频掩护信号的方法.     

浅谈奥米加导航系统的位置误差

奥米加导航系统是一种全球性导航系统.在一般天气条件下,该系统具有良好的导航性能,但是在复杂天气条件下,也暴露出了一些缺点或不足。本文针对使用中出现的问题,根据其工作特性、信号格式、信息处理、定位计算,误差处理方式进行一些理论分析,并对改进系统操作进行一些探索。     

诱饵诱偏无人机截获系统的仿真分析

诱偏技术是电子对抗中自我保护的有效方法.在分析电扫恒差比幅测向原理的基础上,讨论了设置诱饵情况下无人机截获系统测向的误差;在射频仿真系统中,对诱饵、雷达与无人机的相对位置关系进行了研究,给出了算法,最后通过仿真对其进行了验证.这对电子对抗中武器系统诱偏技术的应用、射频仿真系统功能完善以及武器系统作战效能评估等研究都具有一定的参考价值.     

TD-SCDMA中外环功率控制的研究

CDMA系统是干扰受限的系统,降低干扰可以提高系统的容量.TD-SCDMA系统的功率控制就是在保证用户的QoS前提下,降低发射功率,减少系统干扰从而增大系统的容量.本文介绍了TD-SCDMA中外环空率控制的算法,并且分析了功率控制参数对系统性能的影响.     

基于软件无线电的机会信号实时盲分离系统

在复杂的电磁环境中,往往存在多种频率交叠的机会信号,为利用机会信号进行定位增加了难度。针对这个问题,提出了一种基于软件无线电的机会信号实时盲分离系统。系统的硬件部分是在FPGA中实现等变自适应盲分离算法的,实现了AD采集后的复数域混合信号的分离。分离后的信号通过USB3.0数据线上传到上位机中进行存储、识别和实时显示。算法的FPGA实现采用流水线架构和浮点运算设计来提高信号的实时处理能力和数据计算精度。实测结果表明,该系统能够实时分离多路复数域混合机会信号。     

超短波电台自动检测与故障诊断系统设计

介绍了超短波电台自动检测系统与故障诊断系统的功能,并根据功能要求进行了硬件电路的设计,采取面向信号的ATLAS语言进行软件设计和建立在专家知识输入故障推理模型.该系统经使用证明,检测结果精确,检测效率较高.     

复合材料大展弦比机翼动力学建模与颤振分析

新一代航空结构广泛采用复合材料，对复合材料机翼的气动弹性工程化建模和分析是飞机设计的重要任务。应用气动弹性分析理论和方法，对复合材料大展弦比机翼进行了结构有限元建模、模型修正、固有振动特性计算、部件发散与颤振工程分析。本文使用MSC／NASTRAN软件，在复合材料大展弦比机翼的初步静力分析模型基础上，依据结构图纸、相关试验结果反复修改得到合理的机翼结构动力学有限元模型，固有振动计算中采用动力减缩方法消除局部模态并提高计算精度，采用亚音速偶极子格网法求解非定常气动力，并对单独机翼进行了发散和颤振计算分析。     

Measurements of the 12C/13C Ratio in Planetary Nebulae and Implications for Stellar Evolution

We present the results of a study aimed at determining the 12C/13C ratio in two samples of planetary nebulae (PNe) by means of mm-wave observations of 12CO and 13CO. The first group includes six PNe which have been observed in the 3He+ hyperfine transition; the other group consists of 23 nebulae with rich molecular envelopes. We have determined the isotopic ratio in 14 objects and the results indicate a range of values between 9 and 23. In particular, three PNe have ratios well below the value predicted by standard evolutionary models ( 20), indicating that some extra-mixing process has occurred in these stars. We briefly discuss the implications of our results for standard and nonstandard stellar nucleosynthesis.