Solar wind origins in coronal holes and in the quiet Sun

Coronal hole (CH) and the quiet Sun (QS) are considered to account for sources of fast and slow solar wind streams, respectively. The differences between the solar wind streams flowing out from the CH and the QS are thought to be related with different plasma generation and acceleration mechanisms in the respective source regions. Here we review recent studies on the solar wind origin in the CH and the QS, compare the possible flow geometries and magnetic structures in these two kinds of solar regions, and summarize the physics associated with two different origin scenarios.     

Testing the no-hair theorem with observations of black holes in the electromagnetic spectrum

According to the no-hair theorem, astrophysical black holes are uniquely described by their mass and spin. In this paper, we review a new framework for testing the no-hair hypothesis with observations in the electromagnetic spectrum. The approach is formulated in terms of a Kerr-like spacetime containing a quadrupole moment that is independent of both mass and spin. If the no-hair theorem is correct, then any deviation from the Kerr metric quadrupole has to be zero. We show how upcoming VLBI imaging observations of Sgr A∗ as well as spectroscopic observations of iron lines from accreting black holes with IXO may lead to the first astrophysical test of the no-hair theorem.     

运载火箭推力故障下在线计算轻量化任务重构方法

为了避免运载火箭推力下降故障引起发射任务失败,基于径向基神经网络,提出了一种在线计算轻量化的任务重构方法,可快速在线计算最优救援轨道对应飞行轨迹(最优轨迹)的近似解.在离线部分,结合凸优化与自适应配点法产生"故障状态-最优轨迹"数据集.数据集被用来训练径向基神经网络,建立轨迹决策模型来构建故障状态到最优轨迹的动力学关系...     

Short term topological changes of coronal holes associated with prominence eruptions and subsequent CMEs

We study the short-term topological changes of equatorial and polar coronal hole (CH) boundaries, such as a variation of their area and disintegration, associated to reconnection with nearby (within 15° distance) quiescent prominence magnetic fields leading to eruptions and subsequent Coronal Mass Ejections (CMEs). The examples presented here correspond to the recent solar minimum years 2008 and 2009. We consider a temporal window of one day between the CH topological changes and the start and end times of prominence eruptions and onset of CMEs. To establish this association we took into account observational conditions related to the instability of prominence/filaments, the occurrence of a CME, as well as the subsequent evolution after the CME. We found an association between short-term local topological changes in CH boundaries and the formation/disappearance of bright points near them, as well as, between short-term topological changes within the whole CH and eruptions of nearby quiescent prominences followed by the appearance of one or more CMEs.     

Evolution of solar wind structures from 0.72 to 1 AU

Understanding the evolution of solar wind structures in the inner heliosphere as they approach the Earth is important to space weather prediction. From the in situ solar wind plasma and magnetic field measurements of Pioneer Venus Orbiter (PVO) at 0.72 AU (1979–1988), and of Wind/Advanced Composition Explorer (ACE) missions at 1 AU (1995–2004), we identify and characterize two major solar wind structures, stream interaction regions (SIRs) and interplanetary coronal mass ejections (ICMEs). The average percentage of SIRs occurring with shocks increases significantly from 3% to 24% as they evolve from 0.72 to 1 AU. The average occurrence rate, radial extent, and bulk velocity variation of SIRs do not change from 0.72 to 1 AU, while peak pressure and magnetic field strength both decrease with the radial evolution of SIRs. Within the 0.28 AU distance from the orbit of Venus to that of Earth, the average fraction of ICMEs with shocks increases from 49% to 66%, and the typical radial extent of ICMEs expands by about a fraction of 1.4, with peak pressure and magnetic field strength decreasing significantly. The mean occurrence rate and expansion velocity of ICMEs do not change from 0.72 to 1 AU.     

АЛ-31Ф发动机滑油泵故障分析与排故措施

对АЛ - 31Ф发动机滑油泵故障进行了分析 ,并提出了排故措施。     

输油管道的水击仿真

为了对输油管道的水击过程进行仿真，给出了描述水击过程的阿列维水击基本微分方程和常见的边界条件，使用特征线法进行求解。对于顺序输送管道，每个系统时间都要根据混油界面的瞬态流速计算混油界面的位置，并以此重新划分网格插值计算。     

循油冷却航空交流发电机三维温度场的网络拓扑法求解

 本文讨论求解循油冷却航空交流同步发电机的三维温度场的方法,用网络拓扑法求解的基本分块原则以及单元热导的计算,总体热导矩阵的形成方法,损耗和边界条件的处理方法,给出了计算循油冷却电机中油路及气隙部份的对流换热系数计算公式。为减少计算时间,将定、转子分别计算后组合求解,文章最后给出某循油冷却航空交流发电机的定、转子温度分布,并画出了定、转子最热部份的平面温度分布图以及转子绕组沿槽高的温度分布图。     

层板椭圆孔自由边缘效应

 复合材料层板的直边和圆孔自由边缘效应的三维应力分析,国内外已有不少的数值解和近似解析解。Rybicki等提出了各向异性板椭圆孔2维问题变换为圆孔问题的方法,本文论证了这种变换方法的3维情形,从而可根据圆孔自由边缘效应结果来估计椭圆孔自由边缘效应。     

降低含多孔带板应力集中的有限元研究

在飞机和船体结构设计中,由于管路穿行、电缆布置等总体布局要求,在机翼梁的腹板上的指定位置开有多个孔,引发多个孔应力互相干扰。利用ANSYS有限元软件分别对圆孔间距、圆孔数和方形孔圆角半径对含孔带板应力集中系数的影响进行了分析,并与特定情况的试验值进行了对比,两者基本一致。研究结果表明:在孔数一定时,对于不同的孔间距,存在不同的最佳值,使应力集中系数得到最有利的缓和,且板宽对该最佳值的影响不大;对于方形孔, 当圆角半径为1/14方形孔边长时,对缓和应力集中系数最有利。文中并给出了特定情况下最有利于降低应力集中系数的孔的个数。