考虑作动器速率饱和的人机闭环系统稳定域

针对作动器速率饱和引起的Ⅱ型驾驶员诱发振荡(PIO,Pilot Induced Oscillations)严重威胁先进战机飞行安全的问题,研究了计及作动器速率饱和的人机闭环系统稳定域.建立了考虑作动器速率饱和的人机闭环系统非线性模型,引入增广状态变量以及饱和度函数处理速率饱和环节,应用椭球体不变集估计人机闭环系统的稳定域,得到了稳定域估计的一般算法.通过时域仿真研究了所估计的稳定域的保守性,研究了驾驶员操纵增益以及作动器速率饱和值对稳定域的影响.结果表明:稳定域法物理意义清晰、结果直观,可用于人机闭环系统稳定性的评估.研究结果可为先进战机飞行控制系统的设计提供理论依据.     

液体火箭发动机背压振荡环境下的雾化特性研究进展

为加深对背压振荡环境下雾化特性的认识,针对在液体火箭发动机中广泛应用的气液同轴直流式喷嘴、撞击式喷嘴与离心式喷嘴,综述了背压振荡环境下单束液体射流、气液同轴射流、射流撞击以及旋流雾化特性的研究进展,总结了背压振荡影响雾场的主要作用机制,阐述了以往研究中存在的一些问题以及需要突破的若干关键技术难题。通过综述可知,背压振荡主要通过两个方面影响雾场：一是通过改变喷注压降影响喷射,继而影响雾化过程;二是通过振荡的气相流场直接作用于雾场。背压振荡环境下的雾化研究仍需要开展大量工作,且需要突破以下几个技术难点：在试验方面,需要设计可以产生高频率、高幅值压力振荡的反压舱装置,同时对雾场的干扰要降到最小;发展先进的光学诊断方法,可以用于反压舱内雾场信息的提取;在数值模拟方面,需要开展雾化过程的高精度数值模拟,同时研究压力波的产生、发展及演化过程,在这两点基础上研究背压振荡与雾场的相互作用。     

三维等离子体MHD气动热环境数值模拟

电磁流动控制技术是一个多学科交叉融合的重要研究方向,在高超声速飞行器气动特性优化、气动热环境减缓、边界层转捩和等离子体分布等流动控制方面显示出广阔的应用前景。考虑高超声速飞行器绕流流场中发生的离解、复合、电离和置换等化学反应,气体分子振动能激发以及化学非平衡效应,耦合电磁场作用并基于低磁雷诺数假设,通过数值模拟求解三维非平衡Navier-Stokes流场控制方程和Maxwell电磁场控制方程,建立磁场与三维等离子体流场耦合数值模拟方法及程序,采用典型算例进行考核。在此基础上,开展不同条件下磁场对再入三维等离子体流场以及气动热环境影响分析。研究表明:建立的高超声速飞行器的等离子体流场与磁场耦合计算方法及程序,其数值模拟结果与文献符合,外加磁场使飞行器头部弓形激波外推,磁场强度越强,激波面外推距离越大;不同磁场强度环境下,流场中温度峰值大小略有变化,变化幅度较小;磁场对绝大部分区域的热流有减缓作用,作用的大小与飞行高度、马赫数以及磁场的配置紧密相关;当前的计算条件下,飞行的高度越高,磁场的作用越明显。     

The Solar Wind - Inner Heliosphere

The solar wind in the inner heliosphere, inside ~ 5 AU, has been almost fully characterized by the addition of the high heliographic latitude Ulysses mission to the many low latitude inner heliosphere missions that preceded it. The two major omissions are the high latitude solar wind at solar maximum, which will be measured during the second Ulysses polar passages, and the solar wind near the Sun, which could be analyzed by a Solar Probe mission. Here, existing knowledge of the global solar wind in the inner heliosphere is summarized in the context of the new results from Ulysses.     

Alfvén wave heating

This review discusses Alfvén wave heating in non-uniform plasmas as a possible means for explaining the heating of the solar corona. It focusses on recent analytical results that enable us to understand the basic physics of Alfvén wave heating and help us with the interpretation of results of numerical simulations. First we consider the singular wave solutions that are found in linear ideal MHD at the resonant magnetic surface where the frequency of the wave equals the local Alfvén frequency. Next, we use linear resistive MHD for describing the waves in the dissipative region and explain how dissipation modifies the singular solutions found in linear ideal MHD.     

脉冲等离子体推力器推进剂烧蚀传热计算

运用磁流体动力学的方法,建立脉冲等离子体推力器工作过程模型,展开三维仿真研究,对推进剂的烧蚀传热过程进行分析。通过该模型计算得到的推进剂烧蚀质量和元冲量能够反映出实验结果的大体趋势,同时针对不同电容以及两种不同推力室构型的情况进行了评估。结果显示,推进剂的温度变化波形反映着放电波形的变化波形,影响着推力室等离子体的流动,良好的推进剂表面温度分布更有助于推进剂的喷射过程。     

Modelling of Solar Wind, CME Initiation and CME Propagation

Simulations of coronal mass ejections (CMEs) evolving in the interplanetary (IP) space from the Sun up to 1 AU are performed in the framework of ideal magnetohydrodynamics (MHD) by the means of a finite-volume, explicit solver. The aim is to quantify the effect of the background solar wind and of the CME initiation parameters, such as the initial magnetic polarity, on the evolution and on the geo-effectiveness of CMEs. First, three different solar wind models are reconstructed using the same numerical grid and the same numerical scheme. Then, different CME initiation models are considered: Magnetic foot point shearing and magnetic flux emergence. For the fast CME evolution studies, a very simple CME model is considered: A high-density and high-pressure magnetized plasma blob is superposed on a background steady state solar wind model with an initial velocity and launch direction. The simulations show that the initial magnetic polarity substantially affects the IP evolution of the CMEs influencing the propagation velocity, the shape, the trajectory (and thus, the geo-effectiveness).     

磁层顶剪切磁流体非线性性态的谱截断法研究Ⅰ.流场扰动对磁场的作用

本文用谱截断方法研究了磁层顶剪切磁流体的非线性性态。结果表明:流场扰动会使系统出现剪切不稳定(K-H不稳定)性;系统具有对初值的敏感性,这是导致湍动而使磁层顶动力学性态难以预测的根本原因;流场粘性及流场与磁场的相互作用使能量与动量在流场与磁场中转化和传输;外界能流通过粘性与耦合作用可周而复始地在系统中传递。      

1998年5月2日日冕亮度观测图的数值研究

采用数值手段模拟了1998年5月2日日冕亮度观测图，计算模式改进为球坐标下系下特殊的二维理想磁流体（MHD）模型，即把（r,φ）坐标建立在SOHO观测日冕亮度的子午面上，消除了子午面极区的几何奇异性，根据SOHD日冕观测布置磁极子得到初始磁场位形，内边界条件采用自治的投影特征边界条件，计算迭代出稳态的多 磁场结构，得得到了与观测基本一致的亮度图，计算结果表明在太阳表面附近磁场位形对太阳凤等离子参数分布起控制作用。     

Three Dimensional Simulation of the Steady Solar Wind in Carrington Rotation 1935

A three-dimensional MHD simulation is conducted to study the steady solar wind in Carrington Rotation (CR) 1935 by using the three-dimensional numerical magnetohydrodynamic (MHD) model introduced by Feng et al. The numerical results demonstrate that the neutral current sheet has two peaks and two valleys, which is consistent with the result of PFSS model at Wilcox Solar Observatory (WSO). The obtained proton number density at 2.5 Rs is of the same order of magnitude as the result estimated from K-coronal brightness during the CRs 1733-1742 in 1983made by Wei et al. The radial velocity profile along heliocentric distance is consistent with that of low solar wind speed deduced by Sheeley and Wang et al. However, it is not able to reproduce the fast-speed flow in coronal holes and slow solar wind in streamers because of oversimplified energy equation adopted in our model. Future efforts must be made to remedy this deficiency.