等离子体彗尾流线断裂现象的讨论

等离子体Ⅰ型彗尾流线的断裂,已多次被人们见到.本文用MHD的理论,讨论和分析了这种现象,认为这是一种空间等离子体扰动所产生的结果.本文作了定性的分析,及定量的计算,比较满意地解释了这种彗尾中的观测现象.      

1991年太阳L260°活动概况及其射电的特征

本文介绍了太阳L260°活动概况,并计算了黑子群的位置漂移及对应的射电缓变源.北京天文台2.84GHz射电望远镜在该活动区观测到8次特大的射电爆发(流量超过1000s.f.u.),其中4次(1991年5月16日,6月9日,6月11日,8月25日)射电爆发时变曲线十分相似而且这些微波爆发都与Ⅱ型Ⅲ型Ⅳ型米波爆发有良好的对应.可能说明该活动区所对应的日冕在长时间内存在一种磁场位形结构,这种磁场位形结构容易产生日冕物质抛射.      

吹吸扰动控制猝发过程中雷诺应力的实验

采用热线测速技术和双丝边界层热线探针,在风洞中以高于对应最小湍流时间尺度的分辨率,精细测量了平板湍流边界层施加不同频率周期性质量引射前后,不同流向和法向位置的瞬时流向、法向和展向速度分量的时间序列信号.采用流向脉动速度局部平均结构函数模极大值法检测了壁湍流猝发过程中拟序结构不同速度分量和雷诺应力分量的条件相位平均波形.发现在扰动源下游一定范围内,摩擦因数和雷诺应力幅值有所减小,扰动改变了法向或展向脉动速度与流向脉动速度的条件相位平均波形的相位差,使其保持在π/2的奇数倍左右,此时雷诺应力几乎为0,改变了湍流边界层原有雷诺应力的产生和扩散输运机制,抑制了湍流雷诺应力的产生和输运.      

Height of shock formation in the solar corona inferred from observations of type II radio bursts and coronal mass ejections

Employing coronagraphic and EUV observations close to the solar surface made by the Solar Terrestrial Relations Observatory (STEREO) mission, we determined the heliocentric distance of coronal mass ejections (CMEs) at the starting time of associated metric type II bursts. We used the wave diameter and leading edge methods and measured the CME heights for a set of 32 metric type II bursts from solar cycle 24. We minimized the projection effects by making the measurements from a view that is roughly orthogonal to the direction of the ejection. We also chose image frames close to the onset times of the type II bursts, so no extrapolation was necessary. We found that the CMEs were located in the heliocentric distance range from 1.20 to 1.93 solar radii (Rs), with mean and median values of 1.43 and 1.38 Rs, respectively. We conclusively find that the shock formation can occur at heights substantially below 1.5 Rs. In a few cases, the CME height at type II onset was close to 2 Rs. In these cases, the starting frequency of the type II bursts was very low, in the range 25–40 MHz, which confirms that the shock can also form at larger heights. The starting frequencies of metric type II bursts have a weak correlation with the measured CME/shock heights and are consistent with the rapid decline of density with height in the inner corona.     

旋转弹导引头红外角跟踪回路研究

分析了导引头红外末制导角跟踪回路的稳态性能对旋转弹跟踪性能的影响,以及起伏噪声对制导精度的影响,提出了采用二阶无静差角跟踪回路的改进办法.针对改进后的角跟踪回路,计算出了失调角和目标视线角之间的关系,并采用卡尔曼滤波将目标视线角速度准确地估计出来.试验结果表明:二阶无静差系统可以提高旋转弹的跟踪性能,且能够输出满意的制导信号,具有很好的实用价值.     

圆柱绕流尾迹对壁湍流相干结构影响的实验研究

对边界层外区的圆柱尾迹流动结构对边界层近壁区相干结构的影响进行了实验研究.实验在低湍流度风洞中进行,将圆柱放置于yc≈1.1δ(δ为边界层厚度)处,利用热线风速仪分别测量了沿流向不同位置边界层内的瞬时脉动速度信号,并分别比较了位于x/d=1、2、3、4、5、10、15、20、30,y+=10~1000范围内的壁湍流相干结构条件相位平均波形及其统计特性.发现圆柱绕流尾迹对平板边界层内相干结构有明显的影响,圆柱绕流尾迹虽然使壁湍流相干结构从喷射向扫掠转变阶段的强度减弱,但壁湍流相干结构的发生概率增加,总体上促进湍流产生,使湍流边界层增厚,壁面摩擦切应力和壁面摩擦速度均增加,从而肯定了湍流边界层外层流动中产生的扰动与近壁区相干结构猝发的生成和发展有直接联系,壁湍流相干结构猝发是外区流动中产生的扰动与湍流边界层内区共同作用产生的这一结论.     

低能量冲击对碳/环氧复合材料缠绕压力容器的结构损伤及强度影响分析

碳/环氧复合材料缠绕压力容器对外界冲击非常敏感,较低能量的冲击就有可能造成容器结构的严重损伤,进而导致爆破强度的显著降低。国外在碳/环氧复合材料缠绕压力容器低能量冲击研究方面取得了一些试验结果,在对这些试验结果进行综合分析,提炼出了影响冲击损伤效果的相关因素,并分析了这些因素对损伤效果的影响趋势进行了。另外对我国今后开展这方面的相关研究工作提出了一些建议。     

Bi系超导体主要特征量的计算及分析

应用巡游载流子与负U中心局域化载流子混杂相互作用的高T_c氧化物超导体理论模型,对Bi系超导体2212相和2223相的主要特征量——超导转变温度、穿透深度、相干长度、热力学临界场和T_c处比热跳跃进行了数值计算,并将计算结果与实验值比较。根据计算结果,对高T_c氧化物超导体的一些特性进行了分析讨论。     

基于信息管理与融合技术在目标类型识别上的研究

在系统模型的基础上结合实战提出影响目标飞机类型识别的证据,并按照影响程度进行优先权排序;结合数据库,提出证据概率计算的数学表达式;采用深度优先搜索的融合模式,按照D-S证据理论进行融合计算;在传感器管理模块的作用下,对融合结果进行反馈控制;结合实例,对系统进行仿真验证,证明其可靠有效。     

Relationships between energetic storm particle events and interplanetary shocks driven by full and partial halo coronal mass ejections

We have analysed energetic storm particle (ESP) events in 116 interplanetary (IP) shocks driven by front-side full and partial halo coronal mass ejections (CMEs) with speeds $>$400 km s^?1during the years 1996–2015. We investigated the occurrence and relationships of ESP events with several parameters describing the IP shocks, and the associated CMEs, type II radio bursts, and solar energetic particle (SEP) events. Most of the shocks (57 %) were associated with an ESP event at proton energies $>$1 MeV.The shock transit speeds from the Sun to 1 AU of the shocks associated with an ESP event were significantly greater than those of the shocks without an ESP event, and best distinguished these two groups of shocks from each other. The occurrence and maximum intensity of the ESP events also had the strongest dependence on the shock transit speed compared to the other parameters investigated. The correlation coefficient between ESP peak intensities and shock transit speeds was highest (0.73 $\pm$ 0.04) at 6.2 MeV. Weaker dependences were found on the shock speed at 1 AU, Alfvénic and magnetosonic Mach numbers, shock compression ratio, and CME speed. On average all these parameters were significantly different for shocks capable to accelerate ESPs compared to shocks not associated with ESPs, while the differences in the shock normal angle and in the width and longitude of the CMEs were insignificant.The CME-driven shocks producing energetic decametric–hectometric (DH) type II radio bursts and high-intensity SEP events proved to produce also more frequently ESP events with larger particle flux enhancements than other shocks. Together with the shock transit speed, the characteristics of solar DH type II radio bursts and SEP events play an important role in the occurrence and maximum intensity of ESP events at 1 AU.