A new structural reliability analysis method in presence of mixed uncertainty variables

For structures with both random and fuzzy uncertainty, this paper presents a novel method for determining the membership function in fuzzy reliability with the Automatic Updating Extreme Response Surface (AUERS) method. In the proposed method, fuzzy variables are initially converted into a value domain under the given cut level and the extreme point in the domain where the reliability reaches its extreme value is considered. Second, the Particle Swarm Optimization (PSO) algorithm is used to determine the extreme point according to the extreme responses for different sets of random sample inputs. A kriging response surface is subsequently constructed between the random variables and the corresponding extreme points. An automatic updating strategy is then introduced based on the Relative Mean Square Predicted Error (RMSPE) before performing every iteration of reliability analysis. By adding new sample points, the approximate quality of the kriging response surface is improved. Finally, reliability analysis is used to determine the reliability bound under the given cut level. The proposed method assures the accuracy and computation efficiency of the mixed uncertainty reliability analysis results while it prevents the solution from becoming trapped in a local optimum, which occurs in classical optimization methods. Two example analyses are used to demonstrate the validity and advantages of the proposed method.     

Investigation of diurnal variations of cosmic ray fluxes measured with using ASEC and NMDB monitors

A study of daily variations of secondary Cosmic Rays (CR) is performed using data on charged and neutral CR fluxes. Particle detectors of Aragats Space-Environmental Center (ASEC), Space Environmental Viewing and Analysis Network (SEVAN) and neutron monitors of the Neutron Monitor Database (NMDB) are used. ASEC detectors continuously register various species of secondary CR with different threshold energies and incident angles. NMDB joins data of 12 Eurasian neutron monitors. Data at the beginning of the 24th solar activity cycle are used to avoid biases due to solar transient events and to establish a benchmark for the monitoring of solar activity in the new started solar cycle.     

飞行器滑模变结构姿态控制器参数优化设计

研究了大气层外飞行器姿态控制器设计。基于误差四元数建立飞行器姿态运动学与动力学方程,用滑模变结构控制方法设计控制器,通过构造Lyapunov函数验证了控制器具全局稳定性和鲁棒性。以控制器参数为优化变量,机动时间为优化指标,飞行器发动机输出力矩为约束条件,用粒子群算法实现对滑模控制器参数的优化设计。仿真结果表明：控制器设计可行且有效,并能对参数进行优化。     

驻涡燃烧室凹腔流场结构实验

驻涡燃烧室采用凹腔结构稳定火焰,研究凹腔内不同燃料与空气喷射情况下的流场结构非常重要。采用粒子成像测速仪(PIV)测量了驻涡燃烧室凹腔在不同主流速度下的流场,并对比分析了凹腔进气结构分别为不开冷却缝及油气渗混孔、开冷却缝不开油气渗混孔、开冷却缝和后体油气渗混孔、开冷却缝和前体油气渗混孔时的流场结构。研究结果表明,不同主流速度下所设计的不同凹腔进气结构均能在腔内形成稳定的涡,冷却缝对流场的影响较小,凹腔油气掺混孔在开孔截面上对流场及涡核中心位置的影响较大。     

固体火箭发动机Al_2O_3凝结及颗粒破碎的数值模拟

Al2O3凝结对固体火箭发动机Al颗粒的燃烧效率及燃气流动有很大影响。结合拉格朗日方法,建立Al2O3凝结模型,分析了在Al2O3烟雾凝结及颗粒自身破碎作用下,不同初始直径Al颗粒的燃烧效率及燃烧室流场的变化规律。计算结果与同条件下的测试数据有较好的吻合,颗粒分布符合相关实验现象。结果表明,小颗粒燃烧后,流场温度及Al2O3烟雾分布均匀;随颗粒初始直径的增加,径向出现明显分层现象;在发动机出口,小颗粒燃烧效率较高,颗粒中Al2O3质量分数较大,但破碎程度较小;随初始直径增加,颗粒燃烧效率逐渐降低,颗粒中仍含有大量未燃烧的Al,破碎程度提高,颗粒数目急剧增加。     

吸收剂颗粒尺寸对吸波材料性能的影响

对最佳的吸收剂颗粒粒度进行数值计算和分析。从趋肤效应和单个磁畴颗粒大小两个角度,以纯铁粉为例对最佳的粒度做了分析,结果表明,对于2~18 GHz的雷达波,铁粉颗粒在16 nm~1μm为好。还分析了利用纳米颗粒的量子尺寸效应来吸收电磁波时颗粒的尺寸范围,计算结果表明,此时颗粒尺寸至少应小于22 nm。     

基于PSO_LS-SVM的装备研制费用预测研究

在简要介绍了粒子群优化算法基本原理的基础上,建立了基于POS_LS-SVM的装备研制费用预测模型,并应用实例进行了验证。结果表明,采用PSO_LS-SVM方法进行装备研制费用预测,得到的预测结果精度更高、计算速度更快。     

Heating heavy ions in the polar corona by collisionless shocks: A one-dimensional simulation

Recently a new model for explaining the observations of preferential heating of heavy ions in the polar solar corona was proposed ( and ). In that model the ion energization mechanism is the ion reflection off supercritical quasi-perpendicular collisionless shocks in the corona and the subsequent acceleration by the motional electric field E = −V × B/c. The mechanism of heavy ion reflection is based on ion gyration in the magnetic overshoot of the shock. The acceleration due to the motional electric field is perpendicular to the magnetic field, giving rise to large temperature anisotropy with T_⊥ ? T_∥, in agreement with SoHO observations. Such a model is tested here by means of a one dimensional test particle simulation where ions are launched toward electric and magnetic profiles representing the shock transition. We study the dynamics of O⁵⁺, as representative of coronal heavy ions for Alfvénic Mach numbers of 2–4, as appropriate to solar corona. It is found that O⁵⁺ ions are easily reflected and gain more than mass proportional energy with respect to protons.     

Particle acceleration and gamma rays in solar flares: Recent observations and new modeling

Experiments on SMM, GAMMA, Yohkoh, GRANAT, Compton GRO, INTEGRAL, RHESSI and CORONAS-F satellites over the past three decades have provided copious data for fundamental research relating to particle acceleration, transport and energetics of flares and to the ambient abundance of the solar corona, chromosphere and photosphere. We summarize main results of solar gamma-astronomy (including some results of several joint Russian–Chinese projects) and try to appraise critically a real contribution of those results into modern understanding of solar flares, particle acceleration at the Sun and some properties of the solar atmosphere. Recent findings based on the RHESSI, INTEGRAL and CORONAS-F measurements (source locations, spectrum peculiarities, ³He abundance etc.) are especially discussed. Some unusual features of extreme solar events (e.g., 28 October 2003 and 20 January 2005) have been found in gamma-ray production and generation of relativistic particles (solar cosmic rays, or SCR). A number of different plausible assumptions are considered concerning the details of underlying physical processes during large flares: (1) existence of a steeper distribution of surrounding medium density as compared to a standard astrophysical model (HSRA) for the solar atmosphere; (2) enhanced content of the ³He isotope; (3) formation of magnetic trap with specific properties; (4) prevailing non-uniform (e.g., fan-like) velocity (angular) distributions of secondary neutrons, etc. It is emphasized that real progress in this field may be achieved only by combination of gamma-ray data in different energy ranges with multi-wave and energetic particle observations during the same event. We especially note several promising lines for the further studies: (1) resonant acceleration of the ³He ions in the corona; (2) timing of the flare evolution by gamma-ray fluxes in energy range above 90 MeV; (3) separation of gamma-ray fluxes from different sources at/near the Sun (e.g., different acceleration sources/episodes during the same flare, contribution of energetic particles accelerated by the CME-driven shocks etc.); (4) asymmetric magnetic geometry and new magnetic topology models of the near-limb flares; (5) modeling of self-consistent time scenario of the event.     

基于改进粒子群算法的航空发动机状态变量建模

为了克服现有航空发动机状态变量建模过程中的不足,采用了一种改进粒子群算法建立航空发动机状态变量模型。首先改进了粒子群算法,提出一种每个粒子根据自身适应值动态调整其惯性系数方法来平衡搜索性能;对群体最优位置进行实时的代内更新以提高搜索速度;为避免陷入局部最优,在最优个体附近进行随机搜索。其次利用该算法建立航空发动机状态变量模型,根据航空发动机在稳态点处的线性化模型应与在该同一稳态工作点处的非线性模型响应一致的原则构造适应值函数,仿真结果表明所建立的状态变量模型不论是稳态过程还是动态过程都与非线性模型响应基本一致,建模精度较高,建立过程简便。