Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

基于EFFD方法的自然层流短舱优化设计

采用extended free-form deformation(EFFD)方法研究了自然层流(natural laminar flow,NLF)短舱的气动外形优化设计方法.使用基于Bernstein基函数的EFFD方法完成了NLF短舱剖面的参数化,利用基于k-εSST(shear stress transport)两方程湍流模型的γ-θ转捩模型进行自然转捩预测,结合EFFD、一种混合动网格方法、Kriging代理模型和改进的粒子群算法(particle swarm optimization,PSO)建立了针对NLF短舱气动外形的优化设计框架.采用该框架分别对通气NLF短舱和带动力NLF短舱进行优化设计.单独通气NLF短舱优化结果的外表面实现48%的层流,阻力系数比初始通气NLF短舱减小了0.0003.带动力NLF短舱的优化结果外表面保持了41%的层流.这些结果表明采用相关技术建立的优化设计框架在NLF短舱设计中具有一定应用价值.     

表面介质阻挡放电等离子体体积力实验

采用粒子图像测速(PIV)技术,在2200,4800,7300,14600Pa空气压力条件下,测量了高频高压表面介质阻挡放电(surface dielectric barrier discharge,SDBD)等离子体诱导流场.根据速度场和N-S方程求解了等离子体体积力分布,分析了空气压力和激励器电压对等离子体体积力影响.实验结果表明:相同空气压力时,激励器电压越高体积力越大.相同激励器电压时,体积力随空气压力升高减小.在体积力分布区域,体积力方向一致,较大体积力区域分布于体积力方向线上游,流场高速流动区域紧挨较大体积力分布区域,位于体积力方向线下游.     

基于自适应粒子滤波的涡扇发动机故障诊断

针对涡扇发动机非线性、非高斯的特点,提出了一种自适应的粒子滤波算法用于涡扇发动机气路部件突变故障的诊断.为了减小算法的计算量并且保证滤波精度,分析了滤波精度和样本数目的关系,提出根据滤波过程中状态的方差自适应地调整粒子数,在保证一定的滤波精度下可以有效地减少滤波过程中使用的粒子数,提高了算法的实时性.同时,引入扩展卡尔曼滤波(EKF)用于更新粒子,产生重要概率密度函数,在一定程度上避免了粒子的退化.通过某型涡扇发动机的仿真分析表明:改进的算法相比标准粒子滤波算法用于涡扇发动机气路部件故障诊断时,参数估计的方均根误差减小了50%左右,且算法的计算量减小了30%.     

基于PIV的凝胶模拟液撞击雾化速度场实验研究

为了更好研究凝胶推进剂的雾化,采用时间分辨粒子图像测速(TR-PIV),研究了不同撞击角度(45°,60°,75°,90°和120°)和射流压差(0.4MPa~0.8MPa)对凝胶推进剂雾化速度的影响。实验结果表明:雾化液滴速度对于撞击轴线呈单峰对称分布,距离撞击点越远,雾化液滴速度越小且分布越均匀;增大撞击角和增大射流压差都可提高凝胶推进剂有效撞击速度,即增加撞击后液体动能转换液体破碎所需的能量,雾化质量提高;当有效撞击速度大于27.9m/s时,实验室配置的凝胶推进剂可充分雾化。     

转子-支承耦合结构的模型修正研究

在转子-支承耦合结构的动力学分析过程中,结构模态参数计算结果与实验测试结果往往存在较大差异。针对此问题,应用优化算法对结构动力学模型进行修正,使计算模型能更准确地反映结构特性。建立由梁单元、盘单元、弹性支承单元组成的结构动力学有限元模型;选择优化目标函数、设计参数,并对各参数进行灵敏度分析。应用粒子群算法对选取的设计参数进行优化,得到最优模型。利用转子-滚动轴承实验器进行验证,结果表明,方法能够有效地实现转子-支承耦合结构的动力学模型修正,修正后模型更接近实际结构。     

应用三维粒子动态分析仪测量三分支联接流场

应用三维粒子动态分析仪 (3D PDA)测得了矩形截面三分支联接的三维速度分布。在测量中 ,经过理论分析与对比试验 ,选择了蚊香烟雾作为散射粒子。实验结果表明 ,在只有支管进气的情况下 ,在总管的封闭端和支管下游总管壁面处产生了回流 ;以及气流从支管进入总管后由于截面扩张在总管横截面上所诱发的二次流 ,并且二次流现象只发生在支管下游附近的总管横截面上。     

介质涂覆位置对球面收敛喷管电磁散射特性影响

外形设计和隐身材料使用是缩减目标雷达散射截面积(RCS)的两种常用方法。为了研究雷达吸波材料(RAM)对于球面收敛矢量喷管(SCFN)的RCS减缩效果,采用引入阻抗边界条件后的迭代物理光学(IPO)法,研究了球面收敛二元喷管及8种吸波材料涂覆方案的电磁散射特性,并获得了X波段下9种模型的后向RCS随探测角度的变化规律。研究结果表明:吸波材料涂覆可以有效地缩减球面收敛喷管的RCS;合理的涂覆方案可以在保证RCS缩减效果的基础上,降低吸波材料的使用量;相比全涂覆方案,仅在喷管出口和球面段进行涂覆,可以在吸波材料减少30%使用量的情况下,达到全涂覆方案80%的缩减效果。     

Are small-scale field-aligned currents and magnetosheath-like particle precipitation signatures of the same low-altitude cusp?

We examined some 75 observations from the low-altitude Earth orbiting DMSP, Ørsted and CHAMP satellites which were taken in the region of the nominal cusp. Our objective was to determine whether the actually observed cusp locations as inferred from magnetosheath-like particle precipitation (“particle cusp”) and intense small-scale magnetic field variations (“current cusp”), respectively, were identical and were consistent with the statistically expected latitude of the cusp derived from a huge number of charged particle spectrograms (“statistical cusp”).