一种新的求解脑磁逆问题的搜索方法

给出一种新的求解真实头模型下脑磁逆问题的搜索方法.通过不同位置的源的相互关系，由上一个搜索源的计算结果通过简单计算，直接得到下一个搜索源的结果，避免了繁琐耗时的边界元积分方法，简化了求解过程，提高了求解速度. 关键词： 脑磁图 逆问题 搜索方法     

地球外核热对流运动的区域分解多重网格并行数值模拟

旋转球层中热对流运动的数值模拟是地球发电机模型的重要组成部分,对研究地球发电机作用机理具有重要意义.本文设计一个基于国产超级计算平台并行性能良好的地球外核热对流运动并行数值模型.时间积分方案采用与Crank-Nicolson格式和二阶Adams-Bashford公式相结合的近似分解分步法,空间离散基于立方球网格的二阶精度有限体积格式.所得到的两个大规模稀疏线性代数方程组采用带预处理的Krylov子空间迭代法进行求解.为加速迭代求解过程及提高并行性能,迭代过程采用区域分解多重网格的多层限制型加法Schwarz预处理子,减少了求解程序的计算时间,提高了数值模型的并行性能,模型被很好地扩展到上万处理器核数.数值模拟结果与基准模型算例0的参考值吻合得很好.     

分步傅里叶法求解广义非线性薛定谔方程的改进及精度分析

利用分步傅里叶算法求解广义非线性薛定谔方程时对非线性项的处理往往采取了较多的数值近似,而且需要特别小心选择空间和时间的步长以及窗口尺寸,以保证精度要求.以描述光子晶体光纤中超连续谱产生的广义非线性薛定谔方程为例,利用分步傅里叶方法求解时对非线性项直接采用积分处理,而不采取任何数学近似,数值计算时又将积分变成卷积利用傅里叶变换求解,从而方便而又精确地完成了非线性项的计算.整个过程没有任何人为的近似,从而保证了计算模型的精确度.同时,还对因步长选择引起的计算精度进行了分析,提出了从频谱图上判断空间、时间步长选 关键词： 非线性光学 广义非线性薛定谔方程 分步傅里叶方法 超连续谱产生     

表面电荷法平面元电荷系数的半解析解法

针对在线性及高次电荷估计下,表面电荷法中全解析法对平面元电荷系数求解和实现较复杂的问题,提出一种半解析法.将系数积分由局部坐标系变换到整体坐标系下分离参数的二重积分,利用内层积分存在解析解的特点,将二维问题降为一维,方便数值积分计算.对于对数奇异积分问题采用辅助函数法消除.通过算例与全解析法计算精度进行比较,结果表明,在一定的单元划分下,可达到很高精度,具有一定可行性.     

磁偶极子阵列模型的适用性研究与优化分析

随着我国水下探测、通信技术的发展,传统的磁性测量模型已无法满足高精度、高效率建模的需要.本文从舰船磁场积分模型出发,综合分析模型离散化为磁偶极子阵列模型产生的复化中矩形,以及Gauss-Legendre积分余项分析过程引起的离散误差、算法误差,模型简化产生的拟合误差、模型误差等,对模型适用性条件进行分析;同时,以建模精度和计算复杂度为目标构造多目标优化函数,通过NSGA-Ⅱ算法对多目标函数进行求解,得到使精度、复杂度较为均衡的最优解集,提出了不同精度、复杂度需求下的选择规则.为了保证结果的有效性,在舰船磁场混合模型的基础上利用数值实验对模型进行验证,充分考虑模型拟合误差,通过对磁性均匀、磁性不均匀潜艇的仿真分析得到模型达到适用范围时距离与磁偶极子数目的相关关系;在保证模型适用的条件下,基于NSGA-Ⅱ算法的多目标优化过程所得结果运算效率、精度高,具有很好的工程应用价值.     

基于Zernike系数优化模型的光学反射镜支撑结构拓扑优化设计方法

使用Zernike多项式表征镜面的变形,应用伴随变量法推导Zernike系数对拓扑优化设计变量的敏度,克服了差分法求解敏度时计算量大的问题,实现了基于Zernike系数直接建构具有成千上万设计变量的优化模型的目标函数以及设计约束.同时,在有限元数值离散的理论框架下,采用有限单元基函数以及单元数值积分的程序实现了结构变形以及Zernike系数的求解,简化了计算流程的同时还能保证计算精度.本文算法可以对目标函数或约束为线性组合的Zernike系数的一般结构拓扑优化模型进行优化,具有一定的泛用性.     

重夸克偶素的高阶变分-积分微扰修正

利用基于积分方程的改进的变分微扰方法(变分-积分微扰法)求解重夸克偶素激发态.设置含有变分参数的母哈密顿量作为零级哈密顿量,选择该母哈密顿系统的精确解作为试探波函数,得到了只有几项的高阶修正波函数和高阶能量修正.该计算结果更接近精确能量值,修正波函数的有界性和收敛性也得到了证明.结果表明,这种方法不仅可提高计算结果的精度,而且可确保微扰级数解的收敛性. 关键词： 重夸克偶素 变分-积分微扰法 高阶能量修正     

高频电磁波多次散射的数值求解

结合等效射线管模型和物理光学法实现了复杂目标高频电磁波多次散射高效且精确的数值求解.在求解射线管的电磁场积分中，选取物体表面为积分区域，详细推导了在物体表面完成的远场积分公式，数值计算结果比前人沿射线管波前积分更精确.计算了几种由平板构成的导体和涂覆介质目标，数值求解结果与已有的实验数据相当符合.该结果可为复杂目标的雷达探测和识别提供理论参考. 关键词： 电磁散射 电磁场积分方程 物理光学法     

甲烷气体在泡沫陶瓷中预混燃烧的数值模拟和实验研究

本文对甲烷气体在泡沫陶瓷内燃烧进行了数值模拟和实验研究.根据预混燃烧理论,建立了基于气固两相局部非热平衡模型,采用 26 种组分,77 步详细化学反应机理来模拟反应过程.边界上的辐射换热采用双通量法求解,为减少计算时间,计算区域内部利用扩散近似法求解.为减少边界条件对模拟结果精度的影响,提出了采用能量平衡方法,建立边界上的对流,导热和辐射的整个换热过程,模拟表明这种边界条件具有二阶离散精度.     

矩形单元声场波函数构造及其应用*

在波叠加法中,结构外部声场是在离散边界上对Green函数进行积分并叠加得到,但数值积分的计算效率较低。而等效源法虽然提高了计算效率,但其面源简化为点源的过程中存在较大的积分近似误差。针对上述两种方法的缺陷,构造了一种波函数以替代离散单元关于Green函数积分的声场。首先,利用球坐标系下Helmholtz方程的解,推导了替代矩形单元积分的一般形式波函数及效率更高的内推波函数。其次,当离散单元为正方形时,将其近似成圆形域,进一步简化了内推波函数的表达式。最后,将所构造的波函数应用于声场计算。数值结果表明,在计算单个矩形单元外部辐射声场时,构造的波函数不仅保证了计算精度,而且相比于直接积分大幅度提高了计算效率。其中,矩形域一般形式和内推形式的波函数计算效率是直接积分的5～6倍,圆形域内推波函数计算效率达到了直接积分的12～13倍。在简支板声源和立方箱体辐射声源数值算例中,圆形域内推波函数在整个计算频段的声场计算精度均高于等效源法。     

封闭式扬声器系统空气劲度的非线性研究

从理想气体多变过程的状态方程出发,推导了封闭式扬声器系统的非线性空气劲度的理论公式。研究发现,封闭式扬声器系统的非线性空气劲度与音圈运动位移、有效辐射面积、箱体有效容积和多变系数等主要因素有关。通过实验,分别测量了封闭式扬声器系统与扬声器单元的非线性劲度,二者相减获得封闭式扬声器系统的非线性空气劲度。实测数据与理论计算得到很好的吻合。     

广义相对论中负指数多层球的结构及稳定性

本文运用广义相对论讨论了满足负指数多方状态方程的流体多层球。经典引力理论与相对论性理论的差别由σ标志。σ是球体中心处的压力与密度之比。通过数值积分得到了n<0的相对论性Emden函数。在-1ed^*也增大。 关键词：     

Reissner–Nordström and Charged Gas Spheres

This paper studies polytropic gas spheres with some innovations. The main idea, already advanced in the context of neutral, homogeneous, polytropic stellar models, is to base the theory firmly on a variational principle. Another essential novelty is that the mass distribution extends to infinity, the boundary between bulk and atmosphere being defined by an abrupt change in the polytropic index, triggered by the density. The logical next step is to include the effect of radiation, which is a very significant complication since a full treatment would have to include an account of ionization, thus fields representing electrons, ions, photons, gravitons and neutral atoms as well. In way of preparation, we consider models that are charged but homogeneous, involving only gravity, electromagnetism and a single scalar field that represents both the mass and the electric charge; in short, a non-neutral plasma. While this work only represents a stage in the development of a theory of stars, without direct application to physical systems, it does shed some light on the meaning of the Reissner–Nordström solution of the modified Einstein–Maxwell equations. But the main point of the paper is a suggestion about the proper place of the photon gas in a theory of stellar structure and other plasmas, with an application to a simple system; it is proposed to treat the photon gas as part of the dynamics.     

Notes on radial oscillations of gas bubbles in liquids: thermal effects

For oscillations of gas bubbles in liquids, the polytropic exponent and thermal damping constant for the high frequency region have been re-evaluated based on the framework by Prosperetti [J. Acoust. Soc. Am. 61, 17-27 (2007)]. It is seen that the approximation of G(1)? 1 in Prosperetti (1977) should be dropped for G(1)≥ 10(-2). The ratios of bubble radii to wavelengths are the paramount parameters categorizing the behavior into three different regions.     

Rational Legendre pseudospectral approach for solving nonlinear differential equations of Lane–Emden type

Lane–Emden equation is a nonlinear singular equation in the astrophysics that corresponds to the polytropic models. In this paper, a pseudospectral technique is proposed to solve the Lane–Emden type equations on a semi-infinite domain. The method is based on rational Legendre functions and Gauss–Radau integration. The method reduces solving the nonlinear ordinary differential equation to solve a system of nonlinear algebraic equations. The comparison of the results with the other numerical methods shows the efficiency and accuracy of this method.     

Cosmological Implications of Interacting Polytropic Gas Dark Energy Model in Non-flat Universe

The polytropic gas model is investigated as an interacting dark energy scenario. The cosmological implications of the model including the evolution of EoS parameter w _Λ, energy density Ω_Λ and deceleration parameter q are investigated. We show that, depending on the parameter of model, the interacting polytropic gas can behave as a quintessence or phantom dark energy. In this model, the phantom divide is crossed from below to up. The evolution of q in the context of polytropic gas dark energy model represents the decelerated phase at the early time and accelerated phase later. The singularity of this model is also discussed. Eventually, we establish the correspondence between interacting polytropic gas model with tachyon, K-essence and dilaton scalar fields. The potential and the dynamics of these scalar field models are reconstructed according to the evolution of interacting polytropic gas.     

Natures of Statefinder Parameters and Om Diagnostic for Cardassian Universe in Ho?ava-Lifshitz Gravity

In this work, we have considered Cardassian Universe in Ho?ava-Lifshitz gravity. Four types of Cardassian Universe models i.e., polytropic/power law, modified polytropic, exponential and modified exponential models have been considered for accelerating models. The natures of statefinder parameters, deceleration parameter, Om diagnostic and EoS parameters have been investigated for all types of Cardassian models in Ho?ava-Lifshitz gravity.     

Exact anisotropic sphere with polytropic equation of state

We study static spherically symmetric spacetime to describe compact objects with anisotropic matter distribution. We express the system of Einstein field equations as a new system of differential equations using a coordinate transformation, and then write the system in another form with polytropic equation of state and obtain two classes of exact models. The models satisfy all major physical features expected in a realistic star. For polytropic index n?=?2, we obtain expressions for mass and density which are comparable with the reported experimental observations.     

Polytropic Gas Scalar Field Models of Dark Energy

In this work we investigate the polytropic gas dark energy model in the non flat universe. We first calculate the evolution of EoS parameter of the model as well as the cosmological evolution of Hubble parameter in the context of polytropic gas dark energy model. Then we reconstruct the dynamics and the potential of the tachyon and K-essence scalar field models according to the evolutionary behavior of polytropic gas model.