Specific features of the high-speed plasma stream cycles

The high-speed plasma streams in the solar wind are investigated during the solar cycles nos. 20–22 (1964–1996), separately on the two types of streams according to their solar origin: the HSPS produced by coronal holes (co-rotating) and the flare-generated, in keeping with the classification made in different catalogues. The analysis is performed taking into account the following high-speed stream parameters: the durations (in days), the maximum velocities, the velocity gradients and, the importance of the streams. The time variation of these parameters and the high-speed plasma streams occurrence rate show an 11-year periodicity with some differences between the solar cycles considered. A detailed analysis of the high-speed stream 11-year cycles is made by comparison with the “standard” cycles of the sunspot relative number (Wolf number). The different behaviour of the high-speed stream parameters between even and odd solar cycles could be due to the 22-year solar magnetic cycle. The increased activity of the high-speed plasma streams on the descendant phases of the cycles, regardless of their solar sources, proves the existence of some special local conditions of the solar plasma and the magnetic field on a large scale that allow the ejection of the high energy plasma streams. This fact has led us to the analysis the stream parameters during the different phases of the solar cycles (minimum, ascendant, maximum and, descendant) as well as during the polar magnetic field reversal intervals. The differences between the phases considered are pointed out. The solar cycles 20 and 22 reveal very similar dynamics of the flare-generated and also co-rotating stream parameters during the maximum, descendant and reversal intervals. This fact could be due to their position in a Hale Cycle (the first component of the 22-year solar magnetic cycle). The 21st solar cycle dominance of all co-rotating stream parameters against the 20th and 22nd solar cycle ones, during almost all phases, could be due to the same structure of a Hale Cycle – solar cycle 21 is the second component in a 22-year SC. During the reversal intervals, all high-speed stream parameters have comparable values with the ones of the maximum phases of the cycles even if this interval contains a small part of the descendant branch (solar cycles 20 and 22).     

从动态飞行获得极曲线及相关性研究

本文研究飞机极曲线试飞及其与风洞的相关性问题.主要通过动态飞行获得飞机极曲线(C_y≤0.3)的飞行数据.飞行条件:高度为3～12 km;M数为0.8,0.9,1.2,1.8.结果表明:动态飞行技术是可行的,飞行极曲线与风洞极曲线的相关性较好.     

天/地基多平台空间目标光电观测时效性分析

针对如何部署光学探测设备才能更好实现对空间目标的高精度高频度监视问题,考虑光照条件、相对关系及探测性能,构建了天/地基空间目标探测与成像仿真模型;按照轨道特征选取了94颗LEO（Low Earth Orbit,低地球轨道）卫星、63颗GEO（Geosynchronous Earth Orbit,地球同步轨道）卫星和18颗大椭圆轨道卫星,选用春夏秋冬典型季节的特定时间长度,仿真分析了国内地基、南北极科考站、LEO卫星、准GEO卫星等多平台光电手段的位置探测和成像观测能力;比对分析地基平台纬度和季节、天基平台轨道高度和倾角对探测能力的影响得出：南北极科考站相比于国内站点可提高重点季节的探测时效性,98°倾角LEO平台对低轨目标成像时效性方面更具优势,等.在此基础上,提出了我国空间目标光电观测设备天地一体的布局构想.     

基于联合滤波器的高精度卫星定姿系统设计

设计了由陀螺、GPS姿态敏感器、红外地平仪和太阳敏感器构成的太阳同步极轨卫星姿态确定系统。提出联邦滤波器结构和算法,推导了各子系统的量测方程和姿态确定系统的误差状态方程。为规避对量测值进行非相关处理,采用减小GPS姿态敏感器输出的姿态滤波值作为系统滤波器量测值的频率的方法。仿真结果表明,采用联邦滤波器对多敏感器卫星姿态确定系统进行信息融合,具有计算量小、精度高、可靠性好等优点。     

轴流压气机失速特征识别

为了能够准确识别压气机旋转失速过程中失速团的数目,将压气机旋转失速过程中脉动压力波动的相位和幅值特征绘制在极坐标中,然后根据其在极坐标图中表现出来的特征来确定失速团的数目.经过与传统方法对比说明该分析方法对于失速团数目的确定优于原有的方法,具有抗噪性和一定的精度.另外,使用该方法可以可视化周向失速分布区域,并能可视化压气机失速先兆的发生和发展.      

正交各向异性材料拉伸圆棒的颈缩研究

本文对正交各向异性材料的圆棒拉伸试样的颈缩问题进行了有限元模拟计算，得到了不同各向异性参数与颈缩截面椭圆度的定量关系。进一步的研究表明，在相同宏观拉伸下，不同各向异性参数的拉伸试件的载荷与拉伸方向的各向异性参数相关，椭圆度(长短轴半径之比)与径向各向异性参数之比呈线性关系。在拉伸方向各向异性参数相同、其它两个方向参数不同的情况下，载荷区别不大。因此可以利用对颈缩问题的研究来确定材料正交各向异性度系数。     

极坐标算法对飞机CCIP弹道解算的优化

采用极坐标算法对某型飞机CCIP攻击模式进行弹道解算优化,该算法进行坐标变换和积分变量转换后,使弹道的积分变为一个具有确定积分上限的定积分,有效地简化了计算过程,节省了计算时间,提高了计算精度,能较好满足火控系统的精度和实时性要求。     

固体发动机复合材料壳体变形分析

用正交异性薄壳理论分析了复合材料壳体的变形,得到了内压作用下圆筒和封头的应变和位移表达式。结果表明,最大工作压强下圆筒的环向应变只与壳体的安全系数及材料的弹性常数有关,与最大工作压强无关。算例表明,计算值与测试结果吻合良好。     

极大似然法在飞机极曲线辨识中的应用

介绍了利用极大似然法辨识飞机极曲线的基本原理。通过仿真研究及对实测飞行试验数据的处理，表明该方法能够辨识出光滑的非线性飞机极曲线，算法具有良好的收敛性及结果的唯一性，并且可方便地推广应用于工程中其它类型的非线性曲线辨识问题。     

Solar Wind Control of the Magnetospheric and Auroral Dynamics

A dependence of the polar cap magnetic flux on the interplanetary magnetic field and on the solar wind dynamic pressure is studied. The model calculations of the polar cap and auroral oval magnetic fluxes at the ionospheric level are presented. The obtained functions are based on the paraboloid magnetospheric model calculations. The scaling law for the polar cap diameter changing for different subsolar distances is demonstrated. Quiet conditions are used to compare theoretical results with the UV images of the Earth’s polar region obtained onboard the Polar and IMAGE spacecrafts. The model calculations enable finding not only the average polar cap magnetic flux but also the extreme values of the polar cap and auroral oval magnetic fluxes. These values can be attained in the course of the severe magnetic storm. Spectacular aurora often can be seen at midlatitude during severe magnetic storm. In particularly, the Bastille Day storm of July 15–16, 2000, was a severe magnetic storm when auroral displays were reported at midlatitudes. Enhancement of global magnetospheric current systems (ring current and tail current) and corresponding reconstruction of the magnetospheric structure is a reason for the equatorward displacement of the auroral zone. But at the start of the studied event the contracted polar cap and auroral oval were observed. In this case, the sudden solar wind pressure pulse was associated with a simultaneous northward IMF turning. Such IMF and solar wind pressure behavior is a cause of the observed aurora dynamics.