基于粒子系统的火灾特效仿真研究

阐述了粒子系统的基本原理,在对粒子系统的研究基础上,分析了通过预定义和自定义的方法创建和设置火灾模拟效果,论述了在VisualC＋＋6．0环境下Vega火灾模拟效果应用编程,实现了Vega中基于粒子系统的火灾效果的模拟,以及在VisualC＋＋6．0环境下调用Vega提供的API接口来进行基于粒子系统的火灾效果模拟,结果表明粒子系统是模拟火灾效果的有效方法,通过函数编程可以更高效地对虚拟场景中火灾模拟效果进行实时的交互控制。     

一种物联网的时钟服务器配置方法

为了进一步提高物联网时钟同步的准确性和有效性,文中提出了一种时钟服务器的配置方法.此方法是在建立一个时钟服务器配置优化模型的基础上,利用粒子群优化算法求解出时钟服务器的配置结果,并对此方法进行了仿真实验验证.实验结果表明,此时钟服务器配置方法能够满足物联网时钟同步的要求,并且降低了配置代价.     

基于粒子群优化算法的飞行成本最优轨迹优化

以某大型民用飞机为例,应用了以飞行成本最优为目标的性能指标,同时运用最优控制理论,推导出飞机纵向飞行过程（爬升-巡航-下降）的优化方程,使用粒子群算法进行全局寻优,并通过Matlab进行了仿真,实现了以最优成本为目标的轨迹优化。仿真结果表明：用粒子群算法进行全局寻优,寻优效率较高,考虑时间成本后的轨迹,与节油轨迹相比,空速有所增加,耗油量也有所增加,但飞行时间大大缩短,为航空公司降低运营成本提供帮助。     

Why should the latitude of the observer be considered when modeling gradual proton events? An insight using the concept of cobpoint

The shape of flux profiles of gradual solar energetic particle (SEP) events depends on several not well-understood factors, such as the strength of the associated shock, the relative position of the observer in space with respect to the traveling shock, the existence of a background seed particle population, the interplanetary conditions for particle transport, as well as the particle energy. Here, we focus on two of these factors: the influence of the shock strength and the relative position of the observer. We performed a 3D simulation of the propagation of a coronal/interplanetary CME-driven shock in the framework of ideal MHD modeling. We analyze the passage of this shock by nine spacecraft located at ∼0.4 AU (Mercury’s orbit) and at different longitudes and latitudes. We study the evolution of the plasma conditions in the shock front region magnetically connected to each spacecraft, that is the region of the shock front scanned by the “cobpoint” (Heras et al., 1995), as the shock propagates away from the Sun. Particularly, we discuss the influence of the latitude of the observer on the injection rate of shock-accelerated particles and, hence, on the resulting proton flux profiles to be detected by each spacecraft.     

基于离散单元法的二维颗粒阻尼研究

针对自由端带空腔的L型悬臂梁建立了二维颗粒阻尼物理模型,发展并利用离散单元法(DEM)对二维颗粒阻尼进行了数值仿真,重点考查了二维空腔尺寸对颗粒阻尼的影响规律:①高度非线性的颗粒阻尼能够显著地抑制结构振动,阻尼值至少比金属材料阻尼大一个数量级;②当无量纲加速度Γ<1时,颗粒阻尼很小;当Γ＞1时,随Γ增加,颗粒阻尼先增大...     

考虑夹杂间相互影响的颗粒增强两相复合材料等效热膨胀系数预测

基于热-机械载荷联合作用下两相颗粒复合材料的热力学响应特性,推导得到了材料的宏观等效热膨胀系数,给出的表达式中完全考虑了夹杂之间的相互影响,因此适用于大体积分数的复合材料体系.此外,还给出了在热-机械载荷联合作用下代表性体积单元(Representative volume element,RVE)、夹杂和基体中体积均匀化应力场和应变场的具体分布形式.本文的预测结果与已有的实验数据吻合很好,说明了该模型的有效性.     

Solar Energetic Particle Composition, Energy Spectra, and Space Weather

Recent progress in measuring the composition and energy spectra of solar energetic particles (SEPs) accelerated by CME-driven shocks is reviewed, including a comparison of the observed charge-to-mass dependence of breaks in SEP spectra with model predictions. Also discussed is a comparison of SEP and CME kinetic energies in seventeen large SEP events, and estimates of the SEP radiation dose that astronauts would be subject to once they venture outside the protective cover of Earth’s magnetosphere.     

Cosmic Rays at High Heliolatitudes

The Ulysses spacecraft has been the first to orbit the Sun over its poles and to explore the heliosphere at these high heliolatitudes. It has now completed two fast latitude scans, one at solar minimum and one at solar maximum. Since its launch in October 1990, this mission has led to several surprising discoveries concerning energetic particles, cosmic rays, Jovian electrons, the solar wind, the heliospheric magnetic field and the global features of the heliosphere. This review addresses mainly the propagation and modulation of cosmic rays and other charged particles, from both an observational and theoretical point of view, with emphasis on what has been learned from exploring the inner heliosphere to high heliolatitudes. This is done for solar minimum and maximum conditions. The review is concluded with a summary of the main scientific discoveries and insights gained so far from the Ulysses mission.     

On the Differences in Composition between Solar Energetic Particles and Solar Wind

Although the average composition of solar energetic particles (SEPs) and the bulk solar wind are similar in a number of ways, there are key differences which imply that solar wind is not the principal seed population for SEPs accelerated by coronal mass ejection (CME) driven shocks. This paper reviews these composition differences and considers the composition of other possible seed populations, including coronal material, impulsive flare material, and interplanetary CME material.     

通过e+e-→-ff过程探测BH

最小Higgs模型(LH)预言了重规范玻色子BH的存在。为此计算了它对e e-→f(f=l,b,c)过程的贡献,研究了在未来的高能线性e e-对撞(ILC)实验中发现该粒子的可能性,该实验的质心能量S=500GeV,￡int=340fb-1。结果表明在合理的参数空间内,完全可以探测到该新粒子的可能物理信号。