系统组分数的确定

分析了组分数表达式中各个量的意义,并举例说明组分数的计算。讨论了化学平衡和反应进行到底2种情形对系统组分数的影响:化学平衡中生成物只有1相的,化学平衡考虑与否不会影响组分数;可进行到底的反应,在特定条件下可按照化学平衡来处理。最后总结了快速确定系统组分数的步骤。     

自适应同步参数未知的异结构分数阶超混沌系统

基于分数阶系统稳定理论,实现了分数阶超混沌CYQY系统与参数未知的分数阶超混沌Lorenz系统间的异结构自适应同步.不仅设计了控制器,还设计了参数自适应规则并保留了非线性项.数值仿真证实了自适应控制器的有效性. 关键词： 分数阶 超混沌 同步 自适应     

求分段函数在分段点处导数的一种有效方法

为了求解分段函数在分段点处的导数,利用微分学中的相关知识推证定理,并举例说明了如何利用该定理求分段函数在分段点处的导数。     

1维线阵离轴高斯光束的分数傅里叶变换

 为研究非相干的1维线阵离轴高斯光束通过分数傅里叶变换(FRFT)系统的传输特性,利用Collins积分公式,导出了其在FRFT面上的光强分布解析式,并利用此解析式作数值计算和分析。研究表明：非相干的1维线阵离轴高斯光束在FRFT面上的光强分布由FRFT的阶数和子光束数目共同决定,其归一化的光强分布随FRFT的阶数周期性变化,周期为2;子光束数目的大小及其奇偶性对归一化光强分布的影响取决于FRFT的阶数;轴上归一化光强分布也随FRFT的阶数周期性变化,变化周期也为2。     

含介质的单透镜和双透镜分数傅里叶变换光学系统

根据菲涅耳衍射公式,导出了含介质的单透镜与双透镜系统输出面的光场复振幅分布,并与分数傅里叶变换定义式比较,得到了实现分数傅里叶变换的系统结构参量.运用矩阵光学方法,导出上述系统的ABCD矩阵,并与分数傅里叶变换矩阵比较,研究发现两种方法所得结果一致.     

超短脉冲圆极化激光场的一阶修正描述及加速效应

研究了超短脉冲圆极化激光场的一阶修正场,通过数值计算,探讨了入射电子的动力学特性,发现了超短脉冲圆极化激光场中的加速现象.通过研究电子的动力学特性与脉宽的关系发现,近轴近似方程在利用1/ω归一化后,脉宽τ0≤30时(ω为激光频率),仍然适用;而在脉宽τ0>30时,近轴近似方程与一阶修正方程的计算结果出现偏离.在事例τ0=100和τ0=300中,采用一阶修正场方程,研究了电子束团的能量分布与空间分布的特征,发现在脉宽τ0=300的情况下,加速电子数目增多,而且电子束能够发生汇集.     

Probing Quark Loop Effects on Dressed Gluon Propagator

We study the quark loop effects on the dressed gluon propagator and also on the quark propagator itself. We find that the gluon propagators are different in two phases. The quark mass effects on the gluon propagator are small but not negligible. We also study the current quark mass dependence on the bag constant.     

Mass Fraction of 13C-Pocket in Metal-Poor AGB Stars and the Primary Nature of Neutron Source

Chemical abundances of very metal-poor s-rich stars contain excellent information to set new constraints on models of neutron-capture processes at low metallicity. Using the parametric approach based on the radiative s-process nucleosynthesis model, we obtain the mass fraction q of 13 C-pocket, the overlap factor r, the neutron exposure per interpulse △τ, and the component coefficients of the s-process and the r-process for 25 s-rich stars, respectively. We find that q deduced for the lead stars is comparable to the overlap factor r, which is larger than the standard case （hereafter ST case） of the AGB model （q - 0.05） about 10 times, and AT are about 10 times smaller than the ST case （AT = 7.0 mbarn^-1）. Although the two parameters obtained for the lead stars are very different from the ST case of the AGB stellar model, it is worth noting that the total amounts of 13 C in metal-poor condition are close to the ST case. The above relation is a significant evidence for the primary nature of the neutron source and the lead stars could be polluted by low-mass AGB stars. Because interpulse period declines with increasing stellar mass, for high-mass AGB star, the neutron irradiation may be terminated due to their shorter interpulse period. Thus the neutron exposure per interpulse of the larger AGB stars should be about 10 times smaller than the ST case. In this ease, the primary nature of the neutron source also exists.     

Homotopy Analysis Approach to Periodic Solutions of a Nonlinear Jerk Equation

The homotopy analysis method is applied to seek periodic solutions of a nonlinear jerk equation involving the third-order time-derivative. The periodic solutions can be approximated via an analytical series. An auxiliary parameter is introduced to control the convergence region of the solution series. Two numerical examples are presented to demonstrate the effectiveness of the homotopy analysis approach. The examples indicate that, by choosing a proper value of the auxiliary parameter, the first few terms in the solution series yield excellent results.