ESF的Transition区谱分布特性

本文提出了研究Transition区谱分布的静电模型,并按等离子体弱耦强湍理论对其重正化得到了谱方程.对谱方程作适当近似后,证明了该近似谱方程存在扰动密度谱为k~(-5),扰动电场谱为k~(-3)分布的解,从而定量解释了Transition区的实验谱分布结果.     

多冲量近圆轨道交会的快速打靶法

交会对接是空间站工程中一项非常重要的技术.对于给定的交会对接任务,设计可行的变轨策略,找出简单的计算变轨参数的算法是十分必要的.将高斯变分方程在参考轨道附近线性化得到一组线性化的轨道根数偏差方程,将该偏差方程的解作为二体模型解的初值进行轨道根数打靶,然后将所得到的二体模型的解作为摄动模型解的初始进行打靶.结果表明该迭代算法能很快收敛到摄动模型下的交会对接解.     

Cahn-Hilliard方程的行波解

主要利用奇异摄动方法,得到一维Cahn-Hilliard方程行波解形式的内、外解.两者匹配得到整体行波解.这个结果的特点是,它不仅将高阶偏微分方程的解用内外解匹配好,而且完全满足方程的边界条件和初始条件.当长时间变化时, Cahn-Hilliard方程的解以行波结构为极限状态.此结果很好地解释Cahn-Hilliard方程的现有理论及数值结果,实际模型和方程的性质也完全符合.     

结构方程模型的预测建模方法

提出一种结构方程模型的动态预测建模方法,从而可以在无须未来样本数据的情况下,预测系统要素之间未来的因果关系。采用矩阵谱分解,将协方差矩阵唯一分解为特征值矩阵和特征向量矩阵乘积的形式.分别应用经典的线性回归方法和高维群点主轴旋转预测方法对特征值矩阵和特征向量矩阵建立预测模型,提出一种协方差矩阵的后推预测算法.采用极大似然法,迭代估计未来结构方程模型的各种参数.仿真实验例示了该方法的主要计算步骤.计算结果显示,利用本模型得到的拟合值精度较高,预测模型真实可信,表明这种方法可以用于分析和预测结构方程模型.      

麦克斯韦分子碰撞下的离子分布函数及其非相干散射谱的计算

采用麦克斯韦分子碰撞模型描述玻耳兹曼方程的碰撞项, 基于双麦克斯韦分布函数得到的输运方程包含了粘滞和热流的影响, 通过求解输运方程得到了离子漂移速度, 平行和垂直磁场的离子温度, 应力张量以及平行和垂直能量的热流矢量的表达式. 进而得到了麦克斯韦分子碰撞模型下离子分布函数的16矩近似. 利用非相干散射理论, 计算得到了非相干散射谱. 相对于简单的驰豫碰撞模型, 麦克斯韦分子碰撞模型能更准确地描述非麦克斯韦分布的电离层E 层的碰撞过程.      

太阳宇宙线的传播效应(Ⅱ)——峰值谱的传播改正

根据太阳宇宙线传播方程的量纲分析解, 讨论了传播对宇宙线事件峰值谱的影响, 着重指出对其进行传播改正的重要性。太阳风对流是低能谱变坦的可能原因之一, 在一定条件下, 幂律型发射谱可以变成指数型观测谱, 动能幂律谱也可以变成刚度幂律谱。能谱的幂指数随源耀斑的磁方位角而增加, 分布有明显的东西不对称性。进一步对第20周的相对论性太阳质子事件进行传播改正, 求出发射谱, 其中有些可表达成统一指数的幂律谱, 有些仍有低能段趋坦现象。      

ESF大尺度湍谱分布特性

本文从考虑磁剪切效应的电子连续性方程出发,直接进行两点重正化,建立并解析求解了电子密度涨落关联函数<δn(1)δn(2)>的演化方程.得到的谱<(δn)2>k在谱形,强度变化和最小方差拟合的谱指数等方面均与赤道扩展F大尺度湍谱分布实验结果符合较好.统一解释了通常分为Medium,Intermediate两区的实验结果,同时说明了F峰上、下的谱形相似和垂直与平行于地面的两个方向上的谱形相似问题.     

基于像素间孤波的图像处理模型分析

通过对数字图像像素栅格之间非线性影响的研究,建立了像素间非线性影响的一维和二维时间演化方程模型,通过对方程模型的分析可知图像在空间上是离散的,图像像素之间的作用关系是非线性连续的,且方程具有解析性的孤波解.模型重点研究像素孤波的两个孤波之间的相互作用,给出了像素孤波的二孤波解,利用像素孤波的相互作用来研究模型的性能,发现像素孤波相互作用后仍能保持自身性质不变,因此可用像素孤波代替像素本身.同时发现像素孤波在相互作用时其幅值是两者的非线性叠加,可以作为影响的结果;并且像素孤波相互作用时其相位会发生特定的改变,可以将其映射为像素之间相互影响的方向信息.通过实验表明,模型可以用在图像滤波中,平滑度并不最优但是图像细节得到更多保留.      

卫星姿控发动机高空羽流场工程分析

发展卫星姿控小推力发动机高空羽流场的工程估算方法,计算分析其主要燃气组分的分布特征.采用网格技术将发动机喷管出口截面剖分形成多独立点源,建立了非均匀出口流动条件下的分析模型.与自由分子单一点源模型相比,该模型的计算结果更接近实验值.对MBB 10 N双组元发动机多组分羽流场的研究表明,压强场和内能场的变化较剧烈;不同于轻分子组分,重分子组分主要集中于轴线附近,其密度场呈较强方向性.      

导弹摆动式突防策略的有效性

以突防概率作为评价标准,研究了突防导弹作正弦摆动突防机动时的突防效果.拦截-突防问题的模型为线化平面相对运动方程.用共轭系统分析法,得到了该模型在突防导弹摆动式突防策略的作用下,拦截导弹的脱靶量解析解,它由暂态分量和稳态分量组成.研究了突防持续时间按正态分布时导弹的突防概率以及这两部分对突防概率的贡献.     

FEM code simulation of the magnetospheric proton fluxes

We report a study of the numeric solution to the diffusive transport equation for energetic protons magnetically trapped in the Earth's equatorial magnetosphere. The analysis takes into account the pertinent physical processes in this region, including deceleration of protons by Coulomb collisional interactions with free and bound electrons, the charge exchange process, cosmic ray albedo neutron decay source, and electric and magnetic radial diffusion. These results were obtained using the Finite Element Method with magnetic moment and geomagnetic L-shell as free variables. Steady state boundary conditions were imposed at L=1 as zero distribution function and at L=7 with proton distribution function extracted from ATS 6 satellite observations. The FEM-code yields unidirectional proton flux in the energy range of 0.1–1000 MeV at the equatorial top of the geomagnetic lines, and the results are found to be in satisfactorily agreement with the empirical NASA AP-8 model proton flux within the energy range of 0.5–100 MeV. Below 500 keV, the empirical AP-8 model proton fluxes are several orders of magnitude greater than those computed with the FEM-code at L<3. This discrepancy is difficult to explain by uncertainties of boundary spectrum parameters or transport coefficients.     

由地面宇宙线中子强度反演空间质子和重离子的分布

采用线性回归的方法研究了太阳活动平静时期空间高能质子和重离子微分通量与地面OULU宇宙线台站中子强度之间的相关性,利用地面中子强度数据来反演空间高能质子和重离子通量.从质子和重离子的能谱出发,结合OULU台站中子强度的数据,提出了由地面中子强度数据反演空间高能质子和重离子微分通量的新方法.文中以GOES卫星上350～420 MeV,420～510 MeV,510～700 MeV,＞700 MeV(P8～P11)四能道的高能质子和ACE卫星上的元素C为例,并将反演的数据与测量结果比较,二者符合较好.为了探索这种反演方法在空间辐射环境描述中的应用,同时利用2006年11月和12月质子通量的反演结果对反演方法进行了验证,证明利用这一反演方法可以从地面中子强度的数据很好地反演出空间质子和重离子的微分通量.      

Preliminary validation of computational procedures for a new atmospheric ionizing radiation (AIR) model.

A new computational procedure to determine particle fluxes in the Earth's atmosphere is presented. The primary cosmic ray spectrum has been modeled through an analysis of simultaneous proton and helium measurements made on high altitude balloon flights and spacecraft. An improved global fit to the data was achieved through applying a unique technique utilizing the Fokker-Plank equation with a non-linear rigidity-dependent diffusion coefficient. The propagation of primary particles through the Earth's atmosphere is calculated with a three-dimensional Monte Carlo transport program called FLUKA. Primary protons and helium nuclei (alphas) are generated within the rigidity range of 0.5 GV-20 TV uniform in cos2 theta. For a given location, primaries above the effective cutoff rigidity are transported through the atmosphere. Alpha particles are initially transported with a separate package called HEAVY to simulate fragmentation. This package interfaces with FLUKA to provide interaction starting points for each nucleon originating from a helium nucleus. Results from this calculation are presented and compared to measurements.     

Theoretical model of steady-state magnetic reconnection in collisionless incompressible plasma based on the Grad–Shafranov equation solution

The problem of steady-state magnetic reconnection in an infinite current layer in collisionless, incompressible, nonresistive plasma, except of the electron diffusion region, is examined analytically using the electron Hall magnetohydrodynamics approach. It is found that this approach allows reducing the problem to the magnetic field potential finding, while last one has to satisfy the Grad–Shafranov equation. The obtained solution demonstrates all essential Hall reconnection features, namely proton acceleration up to Alfvén velocities, the forming of Hall current systems and the magnetic field structure expected. It turns out that the necessary condition of steady-state reconnection to exist is an electric field potential jump across the electron diffusion region and the separatrices. Besides, the powerful mechanism of electron acceleration in X-line direction is required. It must accelerate electrons up to the electron Alfvén velocity inside the diffusion region and on the separatrixes. This is a necessary condition for steady-state reconnection as well.     

Non-linear diffusion of cosmic rays

The propagation of cosmic rays in the interstellar medium after their release from the sources – supernova remnants – can be attended by the development of streaming instability. The instability creates MHD turbulence that changes the conditions of particle transport and leads to a non-linear diffusion of cosmic rays. We present a self-similar solution of the equation of non-linear diffusion for particles ejected from a SNR and discuss how obtained results may change the physical picture of cosmic ray propagation in the Galaxy.     

利用质子强度变化对太阳质子事件进行短期预报方法初步研究

采用GOSE-10卫星4～9 MeV(P2),9～15 MeV(P3),15～40 MeV(P4),40～80 MeV(P5)能段上的质子通量数据,结合质子能谱,对太阳质子事件发生前各能谱参数的变化特征进行分析,详细介绍利用能谱参数的变化特征及能量E>10 MeV的质子通量数据对太阳质子事件进行预报的新方法,并运用这种方法对2002-2006年期间太阳质子事件进行了预报.预报结果显示,预报提前量最多达到100 h以上,对质子事件的报准率达97.5%,预报方法具备一定的有效性和实用性.      

太阳风质子束流的演化

太阳神飞船观测表明，太阳风高速流中质子束分量相对于核分量的密度随日心距离增加而增加．提出解释这一观测现象的机理并给出二维数值模拟结果．由于阿尔芬波速随日心距离增加而减少，第二支左旋波将与更多的质子共振，把部分原来属于核分布的质子拉到束分布中来．用数值模拟方程方法求解回旋波共振导致的准线性扩散方程，数值结果与观测结果相符合．     

On the effects of dynamical turbulence on the perpendicular diffusion of low-energy cosmic ray electrons

Diffusion perpendicular to the heliospheric magnetic field plays an integral role in the transport of charged particles in the heliosphere. In this study the perpendicular diffusion coefficient of low-energy cosmic ray electrons is calculated, using an equation derived from the random ballistic decorrelation interpretation of nonlinear guiding centre theory. An observationally motivated 2D turbulence power spectrum is assumed and the effects of various turbulence inputs on the resulting perpendicular diffusion coefficient are investigated. The perpendicular diffusion coefficients are first determined at 1 AU, for both magnetostatic and dynamical turbulence conditions. These solutions are also evaluated for radial distances of 0.1 AU to 10 AU to further investigate the values of the perpendicular diffusion coefficients in the very inner heliosphere. The results of this study show that the dissipation range of the turbulence power spectrum provides a negligible contribution towards the perpendicular diffusion coefficient, and that solutions derived using only the energy containing range serve as good approximations for solutions derived assuming the full 2D turbulence power spectrum. Finally, it is shown that the effects of dynamical turbulence, as considered in the present study, do not affect the perpendicular diffusion coefficients derived from the scattering theory considered here.     

Quiet time distribution of plasma pressure in the inner earth's magnetosphere

Trapped particles of the radiation belts provide a considerable part of plasma pressure at low L-shells. The evaluations of this part during quiet times can be made on the basis of existing trapped radiation models. The radial profiles of plasma pressure at 1.2 < L < 7 were obtained by using the empirical AP8MAX model of trapped radiation (L < 6.6) and the theoretical model of the distribution of the proton fluxes in the Earth's radiation belts (L < 7) developed on the basis of the numerical solution of the radial diffusion equation with dissipation processes. The calculations were compared with AMPTE/CCE data. The contribution of quiet-time plasma pressure profile producing the quiet-time ring current to D_st-variation was obtained about 15 nT which is comparative with the magnetic field disturbances during weak and moderate magnetic storms (D_st = −40 ≈ −100 nT).