1998年5月日冕三维结构的数值模拟

采用三维理想磙流体力学（MHD）模式，内边界条件把二维投影特征线边界方法推广应用到三维计算，有效地稳定了数值计算并保证稳态解的自洽性；初始猜解磁场由1935卡林顿周光球磁场观测数据得到，这样计算得到的1998年5月份期间日冕三维结构比较符合实际，计算结果表明：（1）计算得到的源表面非径向磁场量值在磁中性线附近不超过2μT，表明源表面磁场基本径向。（2）模拟得到的源表面径向磁场量值除了在磁中性线附近的区域外变化不大，这和观测一致。（3）由源表面磁场按平方反比的规律计算出1AU处磁场量值更接近观测值。（4）计算得到的日冕结构和观测定性一致，三维数值模拟结果表明，日冕的三维大尺度背景结构主要是由磁场决定的，在闭磁场处或者电流片附近，太阳风的密度高，速度低；在开场区，太阳风的密度低，速度高。     

激波／边界层干扰脉动压力测量技术

建立了激波／边界层干扰脉动压力测试系统。对一组后掠压缩角产生的激波／边界层干扰脉动压力流场进行测量,结果表明,脉动压力时均值及其分布与静态测量得到的结果一致。测量还发现在实验的锥形干扰范围内,未出现类似于二维干扰中由非定常低频振荡激波引起的间歇现象。     

磁流体斜激波的碰撞

讨论了磁流体斜激波之间的碰撞及其与接触间断的相互作用规律,主要结论如下:(1)两个快激波碰撞后交换位置,同时出现一接触间断和一慢稀疏波对。(2)两个慢激波碰撞后交换位置且强度减弱,同时出现一接触间断和一块激波对。(3)一前向快激波与一后向慢激波碰撞后交换位置,快激波强度增加,慢激波强度减弱,同时出现一后向快激波、一负接触间断和一前向慢稀疏波。(4)一前向快激波与一正(负)接触间断相互作用后交换位置,快激波减弱,同时出现一后向快稀疏波(快激波)、一后向慢激波和一前向慢激波(慢稀疏波).(5)一前向慢激波与一正(负)接触间断相互作用后交换位置,慢激波减弱,同时出现一后向慢稀疏波(慢激波)和一快稀疏波(快激波)对。      

行星际磁场北向时磁层顶区磁场重联的全球模式

在对背阳面磁层顶区局域磁场重联模拟的基础上提出了一个行星际磁场北向时磁层顶磁场重联的全球模式。行星际磁场北向时碰层顶磁场重联导致近地尾瓣的能量被输送到远磁尾,太阳风能量不在磁尾储存,向阳面磁层顶变厚,磁层受到一系列扰动。      

双楔面诱导的斜爆轰波阵面的磁流体控制

基于高超声速飞行器爆轰推进发展需要,数值研究了由双楔面诱导的斜爆轰波类型及其磁流体(MHD)控制的可行性,探讨了后楔倾角变化对双楔斜爆轰流场与MHD控制的影响.结果表明:对于前、后楔倾角分别为15°与20°的双楔面诱导的斜爆轰,Lorentz力可以将不同来流马赫数条件下的稳定斜爆轰波阵面恢复到设计位置,并可以使不稳定斜爆轰波趋于稳定,但是,无法将不稳定斜爆轰波恢复到设计位置.而当后楔倾角稍微增加时,若爆轰流场稳定,同样可对斜爆轰波阵面进行有效控制.但当后楔倾角大于25°时,稳定斜爆轰波流场失稳,此时MHD无法控制流场稳定性.但若增加气体反应速率,虽然斜爆轰波不稳定,MHD控制却可使其趋于稳定,但无法将爆轰波阵面恢复到设计位置.      

MHD waves in coronal flux tubes

The basic MHD waves of a coronal flux loop are investigated for the rectangular box model of a plasma with oblique magnetic field and line-tied at the ends. The waves found are completely different from those in a periodic box, representative for tokamaks. They consist of a mixture of Alfvén components with a ballooning factor, favouring minimal field line bending, and fast components without such a factor. Pure Alfvén modes are only found as singular limiting cases of cluster spectra of Alfvén-fast waves, where the fast components are localised in a photospheric boundary layer which is dictated by the requirements of line-tying. This justifies the assumption of continuous spectra in coronal loops, required for the mechanism of resonant Alfvén wave heating. The waves consist of large amplitude Alfvén components in the corona and fast components with a small but rapidly varying amplitude in the boundary layer, so that they appear to have the right signature for effective transfer of energy from the photosphere to the corona.     

Observing the Sun at 20–650 MHz at Thermopylae with Artemis

Fine structure of type IV radio solar bursts with a great variety and complexity often give much information in different ways and enable estimation of various coronal characteristics. In this work, we expose our new method for fine structure revealing and separation of two basic kinds of type IV fine structure, as fibers and pulsations. We also estimate frequency drift of fibers from dynamic spectra, clean from continuous background, with a prototype method using 2-D Fourier transform and we estimate periodicities of fibers as well as pulsations with continuous wavelet transform. Working with the last method we found periodicities close to 3 min umbral oscillations and 5 min global solar oscillations.     

具有操纵面间隙非线性二维翼段的气动弹性分析

 基于Theodorsen 理论和Wagner 函数,提出了不可压缩流作用下三自由度二维翼段任意运动非定常气动力表达式。对操纵面自由度具有的间隙非线性,建立了二维翼段气动弹性系统无量纲分段线性运动方程。数值仿真预示了系统极限环振动的相轨迹、无量纲振动幅值和频率,表明操纵面铰链处存在的间隙非线性将导致整个系统的极限环振动;随着来流速度的增加,系统极限环振动的幅值和频率都存在跳跃现象。     

磁控进气道二维性能计算

超燃冲压发动机进气道通常都是针对某一特定的马赫数进行设计的,当飞行马赫数不在设计马赫数时发动机性能急剧降低,磁控进气道的应用很有可能解决这一技术难题.对磁控进气道内的流动情况进行了二维数值模拟.飞行马赫数大于设计马赫数时采用磁控进气道可以调整激波位置使激波回到设计点,并减小燃烧室入口处的马赫数.分析了霍尔效应对磁控进气道性能的影响,结果表明分段电极可以有效减小霍尔效应的不利影响.      

Superlow-Frequency MHD-Eigenoscillations With a Discrete Spectrum in Parabolic Model of Magnetosphere

A new concept of the global magnetospheric resonator is suggested for fast magnetosonic waves in which the role of the resonator is played by the near part of the plasma sheet. It is shown that the magnetosonic wave is confined in this region of the magnetosphere throughout its boundaries. The representative value of the resonator's eigenfrequency estimated at f ≈ 1 mHz is in good agreement with observational data on ultraThe theory explains the ground-based localization of the oscillations observed in the midnight-morning sector of the high-latitude magnetosphere.