大气信道对沿海激光通信的影响分析

为利于沿海靶场激光通信系统的设计与应用,研究分析了晴天、轻霾天、雾天、湍流等常见天气中大气信道对激光通信的影响。针对短距离近地面传输特点,利用经验数学模型仿真分析了激光透过率与能见度以及误码率与折射率结构常量的定量关系。结果表明：激光波长越长,衰减和湍流效应影响越小;晴天大气衰减对通信影响最小,轻霾天次之,雾衰减影响最严重;强湍流闪烁效应对误码率影响较大,但增加链路高度和选择长波长激光可减小影响。     

横流中喷雾掺混流场结构研究

为了获得有限空间内喷雾在横流影响下的掺混发展及机理,应用PIV系统测量了单个旋流雾化喷嘴产生的喷雾在横流中的掺混流场,实验在矩形通道内实施。获得了3种喷嘴入射角度和3种液气动量比下的掺混截面流场结构。结果表明,由于射流撞击、剪切和壁面约束作用,流场中形成前缘涡和反旋涡对,反旋涡对对掺混起了主要作用。比较不同喷嘴入射角度和液气动量比下的流场结构发现,随喷雾入射角度减小,两相作用提前发生,且反旋涡对尺度小,更利于掺混均匀;随液气动量比减小,气相作用增强,旋涡强度和尺度变小,更小的涡尺度更利于液滴均匀分布。     

某带分流叶片的亚声速离心压气机叶轮CFD结果确认及分析

为了研究数值模拟结果的准确性,使用计算流体动力学(CFD)软件Numeca,采用Spalart-Allmaras(S-A)模型和shear stress transport(SST)模型对某压比为1.5的亚声速离心压气机叶轮的性能进行了计算,并将4个不同截面上的速度分布等计算结果和实验数据进行了对比.结果表明:S-A模型和SST模型的计算结果几乎完全相同,误差小于1%;整体性能的模拟计算结果和实验值吻合较好,在设计工况点,误差在2%以内,在非设计工况点,误差也小于6%;不同截面上速度分布的计算结果和实验值相差较大,在轮毂附近,最大误差在20%左右,在轮缘附近,部分截面最大误差高于100%,不能真实反映轮缘附近的流动情况.      

四轴陀螺稳定平台分区离散变结构控制策略及优化方法

为了有效提高四轴陀螺稳定平台伺服系统全姿态控制精度,针对变结构分区控制过程中台体大角度晃动问题,提出一种优化的四轴陀螺稳定平台控制回路分区离散变结构控制策略。在分析四轴平台框架系统运动学方程的基础上,给出了随动式分区离散变结构控制策略,通过分析执行机构与被控角速度之间的相关程度,对随动式分区离散变结构控制策略进行优化。为了进一步减小变换区域时的切换扰动,在随动式分区离散变结构控制基础上提出一种稳定式分区离散变结构控制方法,对变结构区域进行了整合和优化,有效避免了运动状态在不同区域之间切换造成的台体晃动。仿真结果表明,随动式分区离散变结构控制策略优化前后相比,X 方向台体晃动角速度减小63.5%,Y 方向台体晃动角速度减小84.5%;稳定式分区离散变结构控制策略优化前后相比,X 方向台体晃动角速度减小29.0%,Y 方向台体晃动角速度减小57.3%,有效减小了平台台体在变结构控制切换过程中的晃动,提高了控制精度。     

Inferring plasma flow velocities from photospheric vector magnetic field observations for the investigation of flare onsets

The amount of emergence and submergence of magnetized plasma and the horizontal motion of the footpoints of flux tubes might be crucial for the dynamics of the solar atmosphere. Although the rate of flux emergence and submergence can be observationally determined near the polarity inversion line (Chae et al., 2004), the same is not true for regions away from the PIL. Also, the horizontal motions cannot be directly measured in the solar photosphere. In this sense, the evolution of the photospheric magnetic field provides valuable information which can be used to estimate photospheric plasma flows since magnetic field and plasma are closely associated (frozen-in-condition). We used three methods to estimate the photospheric plasma motion from magnetic field observations. The methods were applied to photospheric vector magnetic field data of active region NOAA 9077, observed by the Huairou Solar Observing Station (HSOS) of the National Astronomical Observatories of China before and after the ‘Bastille Day’ flare on July 13th and 14th, 2000.     

交叉航路碰撞风险研究

航路上航班的碰撞风险问题是目前空域规划的主要研究问题之一,就交叉航线的碰撞风险问题进行了研究.首先推导出交叉航路碰撞概率计算公式,然后结合概率论和划设保护区的方法对交叉航线的碰撞风险问题进行了研究,最后用自主开发的"空域安全评估方法的研究与应用"软件对上海区域内的某交叉航线的碰撞风险进行了仿真计算.为交叉航路的碰撞风险计算提供了简单易行的方法.     

The dynamic chromosphere: Pushing the boundaries of observations and models

The interface between the bright solar surface and the million-degree corona continues to hold the key to many unsolved problems in solar physics. Advances in instrumentation now allow us to observe the dynamic structures of the solar chromosphere down to less than $0_{.}^{″}1$ with cadences of just a few seconds and in multiple polarisation states. Such observational progress has been matched by the ever-increasing sophistication of numerical models, which have become necessary to interpret the complex observations. With an emphasis on the quiet Sun, I will review recent progress in the observation and modelling of the chromosphere. Models have come a long way from 1D static atmospheres, but their predictions still fail to reproduce several key observed features. Nevertheless, they have given us invaluable insight into the physical processes that energise the atmosphere. With more physics being added to models, the gap between predictions and observations is narrowing. With the next generation of solar observatories just around the corner, the big question is: will they close the gap?     

利用多卫星观测CIR事件演变的统计分析

根据2007-2009年STEREO-BEHIND (STB)和ACE卫星的行星际磁场和太阳风数据, 基于冕洞高速流从太阳向外匀速径向传输假设, 讨论了随着STB和ACE卫星与太阳之间的夹角从0°增大至70°时, 冕洞发出的高速太阳风形成的相互作用区(CIR)依次扫过STB和ACE卫星的时间差特性, 并统计分析了两颗卫星观测到的CIR参数的变化特征. 结果显示, 可以利用STB对CIR事件的观测来预测这个CIR事件到达ACE的理论时间, 时间误差均值和最大值分别为0.217d和0.952d, 时间误差的产生与STB和ACE卫星观测到的CIR速度大小的不同有关, 用速度差异矫正后, 时间误差的平均值和最大值可分别减小为0.194d 和0.489d; STB和ACE卫星观测的CIR事件太阳风速度最大值的线性相关系数达到了0.84, STB和ACE卫星观测到的CIR事件对特征物理量中速度、质子温度的变化最小, 而质子密度及总压力的变化最大. 分析结果表明, STB和ACE卫星观测到的CIR事件有很强的相似性, STB卫星的CIR观测可以作为ACE卫星观测CIR事件特征的参考, 从而为地球空间环境扰动预报提供依据.      

舰空导弹发射时间窗解算模型仿真

介绍了舰空导弹发射时间窗的概念和舰空导弹杀伤区、发射区的形状和参数,在舰空导弹发射区解算的基础上,对时间窗的解算进行了数学建模,其目的是将结果作为目标威胁评估的一个指标和确定舰空导弹的发射时机。为了使时间窗解算具有实时性和合理性,在解算中考虑了来袭目标机动的影响,采用MATLAB对所建模型进行了仿真计算。仿真结果表明,所得数据可作为舰空导弹对来袭目标的威胁评估和目标分配的依据,指导防空作战指挥决策。     

What are the physical mechanisms of eruptions and CMEs?

CMEs are due to physical phenomena that drive both, eruptions and flares in active regions. Eruptions/CMEs must be driven from initially force-free current-carrying magnetic field. Twisted flux ropes, sigmoids, current lanes and pattern in photospheric current maps show a clear evidence of currents parallel to the magnetic field. Eruptions occur starting from equilibria which have reached some instability threshold. Revisiting several data sets of CME observations we identified different mechanisms leading to this unstable state from a force free field. Boundary motions related to magnetic flux emergence and shearing favor the increase of coronal currents leading to the large flares of November 2003. On the other hand, we demonstrated by numerical simulations that magnetic flux emergence is not a sufficient condition for eruptions. Filament eruptions are interpreted either by a torus instability for an event occurring during the minimum of solar activity either by the diffusion of the magnetic flux reducing the tension of the restraining arcade. We concluded that CME models (tether cutting, break out, loss of equilibrium models) are based on these basic mechanisms for the onset of CMEs.