用于飞行器隐身的闭式等离子体厚度选择分析

为分析闭式等离子体用于飞行器隐身的可行性,引入了可观隐身效果的概念及对应的闭式等离子体厚度。采用WKB方法,详细研究了X波段下的闭式等离子体吸波效果,得到了对应频段下产生可观隐身效果需要的等离子体厚度;研究了不同电子密度分布的吸波特性,数值算例说明,对不同电子密度分布的等离子体,吸波效果与厚度均成线性关系,同时,采用理论推导验证了该现象的正确性。结果表明,对于给定的电磁波,采用一定厚度的闭式等离子体可以达到可观隐身效果。     

直升机动力学中参数振动问题的数值解法

 参数振动问题是直升机的基本动力学问题之一,旋翼桨叶的挥舞弯曲微分方程和摆振弯曲微分方程都是复杂的参数振动问题,在许多计论直升机旋翼动力学的论著中~[1-4],有的虽然推导了复尽杂的参数振动方程,却没有提到求解的方法,有的对此根本没有论及.本文旨在讨论参数问题的数值解法.     

高超飞行器表面热效应地面模拟实验研究

文章深入分析高超飞行器与临近空间大气相互作用的基本物理过程,激波加热及粒子碰撞产生等离子体的物理机制,并利用磁热屏蔽效应在高超飞行器模拟器与高速定向流间建立磁化等离子体鞘层,大幅降低中性激波气体向飞行器的能流传递,从而为高超飞行器提供有效的热防护作用。通过两次比对实验验证了磁热屏蔽效应的有效性及工程实施的可行性,为今后研制高韧性、超轻质、可重复使用热防护复合材料提供了实验数据,奠定了技术基础。实验中利用层流等离子体源作为高能流密度热源是热防护实验装备上的创新,层流等离子体源能流截面大、能流密度高,可以针对高超飞行器表面热效应进行全尺寸的模拟实验。     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.     

Modeling Multifractality of the Solar Wind

The question of multifractality is of great importance because it allows us to investigate interplanetary hydromagnetic turbulence. The multifractal spectrum has been investigated with Voyager (magnetic field) data in the outer heliosphere and with Helios (plasma) data in the inner heliosphere. We use the Grassberger and Procaccia method that allows calculation of the generalized dimensions of the solar wind attractor in the phase space directly from the cleaned experimental signal. We analyze time series of plasma parameters of the low-speed streams of the solar wind measured in situ by Helios in the inner heliosphere. The resulting spectrum of dimensions shows a multifractal structure of the solar wind attractor. In order to quantify that multifractality, we use a simple analytical model of the dynamical system. Namely, we consider the generalized self-similar baker’s map with two parameters describing uniform compression and natural invariant measure on the attractor of the system. The action of this map exhibits stretching and folding properties leading to sensitive dependence on initial conditions. The obtained solar wind singularity spectrum is consistent with that for the multifractal measure on the weighted baker’s map.     

Complexity,Forced and/or Self-Organized Criticality,and Topological Phase Transitions in Space Plasmas

The first definitive observation that provided convincing evidence indicating certain turbulent space plasma processes are in states of ‘complexity’ was the discovery of the apparent power-law probability distribution of solar flare intensities. Recent statistical studies of complexity in space plasmas came from the AE index, UVI auroral imagery, and in-situ measurements related to the dynamics of the plasma sheet in the Earth's magnetotail and the auroral zone. In this review, we describe a theory of dynamical ‘complexity’ for space plasma systems far from equilibrium. We demonstrate that the sporadic and localized interactions of magnetic coherent structures are the origin of ‘complexity’ in space plasmas. Such interactions generate the anomalous diffusion, transport, acceleration, and evolution of the macroscopic states of the overall dynamical systems. Several illustrative examples are considered. These include: the dynamical multi- and cross-scale interactions of the macro-and kinetic coherent structures in a sheared magnetic field geometry, the preferential acceleration of the bursty bulk flows in the plasma sheet, and the onset of ‘fluctuation induced nonlinear instabilities’ that can lead to magnetic reconfigurations. The technique of dynamical renormalization group is introduced and applied to the study of two-dimensional intermittent MHD fluctuations and an analogous modified forest-fire model exhibiting forced and/or self-organized criticality [FSOC] and other types of topological phase transitions. This revised version was published online in August 2006 with corrections to the Cover Date.     

Effect of q-nonextensive hot electrons on bifurcations of nonlinear and supernonlinear ion-acoustic periodic waves

Nonlinear and supernonlinear ion-acoustic periodic waves are investigated in a three-component unmagnetized plasma which consists of mobile fluid cold ions, Maxwellian cold electrons and q-nonextensive hot electrons employing phase plane analysis. Using the traveling wave transformation, the plasma system is reduced to a planar autonomous dynamical system. Utilizing phase plane analysis of planar dynamical systems, all possible phase portraits including nonlinear homoclinic orbit, nonlinear periodic orbit, supernonlinear homoclinic orbit and supernonlinear periodic orbit are presented depending on physical parameters $q,\alpha ,\sigma$ and V. Using numerical simulations, nonlinear and supernonlinear ion-acoustic periodic waves are shown for different conditions. It is found that the nonextensive parameter q plays a crucial role in the bifurcations of nonlinear and supernonlinear ion-acoustic periodic waves. Our study may be applicable to understand the nonlinear and supernonlinear periodic features in auroral plasma.     

颈动脉内血流动力学特征受向前加速度影响的数值模拟

人们在日常或某些特殊条件下常会面临方向和大小发生迅速变化的加速度环境,已有研究发现加速度环境会影响心血管系统生理、病理特征。利用计算机模拟方法详细研究了向前加速度环境下人体颈动脉内的血流动力学参数变化规律。结果表明:加速度会对颈动脉内压力、压力梯度、壁面剪切应力等与血管生理、病理现象密切相关的血流动力学参数产生显著影响。研究结果为加速度环境下颈动脉生理、病理研究提供了一定的理论依据,也为航空航天领域加速度环境下人员防护提供参考。      

面向深空探测的电磁帆推进技术研究进展

电磁帆是一类利用太阳风驱动的无工质或少工质新型推进技术,在需要推力器长时间工作的深空探测任务中具有非常广阔的应用前景。首先介绍了电磁帆的基本概念和主要分类,其次分别介绍了电帆、纯磁帆和磁等离子体帆三类推进方式的系统组成和工作原理,重点介绍了各自的研究现状,并梳理出了相关关键技术,同时介绍了等离子体磁罩技术。最后对电磁帆推进技术研究进展进行了总结,为国内开展此方面研究提供了研究方向和发展思路。     

大功率无电极高密度等离子体电磁推进概述

无电极高密度等离子体电磁推进技术已成为未来深空探测、载人航天和货运、太阳能电站以及航天器在轨服务与维护等空间任务中极具竞争力的核心推进技术之一。在梳理不同无电极等离子体电磁加速机制基础上,开展大功率无电极高密度等离子体电磁推进技术性能对比,给出新概念无电极场反构型电磁推进技术向未来超大功率拓展的优势和发展潜力,同步分析了该技术亟需解决的关键基础问题,旨在为中国新概念场反构型电磁推进技术的研发提供理论基础。