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。     

基于SMC-CPHD的多目标跟踪算法研究

针对CPHD滤波算法在多目标跟踪中计算难处理和对于局部目标估计存在漏检的问题,提出了基于序贯蒙特卡罗方法的基数概率假设密度（SMC-CPHD）滤波算法。这种方法是将SMC和CPHD两种滤波算法的优点相结合,用一些离散的粒子去接近PHD函数,不仅解决了在滤波修正步没有闭式解的问题,而且避免了当某个目标发生漏检时,PHD权值的转移问题,在递推PHD函数的同时也递推基数分布。将此方法应用到有杂波存在复杂的多目标跟踪环境中,通过仿真实验,对CPHD滤波和SMC-CPHD滤波得出的结果进行比较,验证了本文所提出方法对多目标跟踪的可行性和精确性。     

燃烧供热热光伏系统实验研究

针对未来深空探测供电需求,设计了一套热光伏发电系统,采用丙烷燃烧器模拟同位素热源,并利用低禁带GaSb电池实现了系统的热电转换。研究了气体流量、过量空气系数、回热器性能、滤波器等对辐射器温度及电池输出功率、系统转换效率的影响。结果表明：电池输出功率随燃气量单调增加,而在一定燃气量下,存在一最优过量空气系数使其达到最大值;同时,回热器和滤波器对辐射器温度和电池输出特性有很大影响;本实验系统可以实现最大输出功率密度0.45W/cm 2,系统转换效率2.8%。     

考虑在轨运动可靠性的空间机械臂关节力矩优化方法

提出一种考虑在轨运动可靠性的冗余度空间机械臂关节力矩优化方法。首先将机械臂操作空间中点到点的转移任务从笛卡尔空间转换至关节空间,利用七次多项式插值法对各关节变量进行参数化处理,获得粒子群算法的优化控制参数;与传统路径规划方法不同,将机械臂各关节力矩的均值和最小作为粒子群算法优化求解的目标函数;依据该目标函数以及相应优化控制参数,利用粒子群算法对空间机械臂运行轨迹进行优化求解,得到机械臂关节力矩均值和最小的运行路径。仿真实验表明,相比传统路径规划方法及以关节力矩二范数为目标函数的关节力矩优化方法,在降低冗余度空间机械臂关节力矩均值方面,文中方法分别减小了33.57%和10.47%;在降低关节力矩最大值方面,分别减小了43.25%和6.19%。     

Experimental investigations of a full model with adaptive elasto-flexible membrane wings

The morphing wing concept aims to constantly adapt the aerodynamics to different flight stages. The wing is able to adapt to different flight conditions by an adjustable Aspect Ratio (AR) and sweep. A high AR configuration provides high aerodynamic efficiency, while a low AR configuration, with highly swept wings offers a good maneuverability. Additionally, the flexible membrane allows the wing surface to stretch and contract in-plane as well as the airfoil to adapt to different aerodynamic loads. In the context of this work, the aerodynamic characteristics of a full model with form-adaptive elasto-flexible membrane wings are investigated experimentally. The focus is on the high-lift regime and on the analysis of the aerodynamic coefficients as well as their sensitivities. Especially, the lateral aerodynamic derivatives at asymmetric wing positions are of interest.     

Study of the radiation fields in LEO with the Space Application of Timepix Radiation Monitor (SATRAM)

We present the analysis of data taken by the Space Application of Timepix Radiation Monitor (SATRAM). It is centred on a Timepix detector (300?$\mathrm{\mu }$m thick silicon sensor, pixel pitch 55?$\mathrm{\mu }$m, 256?×?256 pixels). It was flown on Proba-V, an Earth observing satellite of the European Space Agency (ESA) from an altitude of 820?km on a sun-synchronous orbit, launched on May 7, 2013. A Monte Carlo simulation was conducted to determine the detector response to electrons (0.5–7?MeV) and protons (10–400?MeV) in an omnidirectional field taking into account the shielding of the detector housing and the satellite. With the help of the simulation, a strategy was developed to separate electrons, protons and ions in the data. The measured dose rate and stopping power distribution are presented as well as SATRAM’s capability to measure some of the stronger events in Earth’s magnetosphere. The stopping power, the cluster height and the shape of the particle tracks in the sensor were used to separate electrons, protons and ions. The results are presented as well. Finally, the pitch angles for a short period of time were extracted from the data and corrected with the angular response determined by the simulation.