Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere

We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to solar gravity. Incorporating specific forms of current density and gas pressure in the Grad–Shafranov equation, we solve the magnetic flux function, and find it to be separable with a Coulomb wave function in radial direction while the vertical part of the solution decreases exponentially. We employ improved fluxtube boundary conditions and take a realistic ambient external pressure for the photosphere to transition region, to derive a family of solutions for reasonable values of the fluxtube radius and magnetic field strength at the base of the axis that are the free parameters in our model. We find that our model estimates are consistent with the magnetic field strength and the radii of Magnetic bright points (MBPs) as estimated from observations. We also derive thermodynamic quantities inside the fluxtube.     

An analytical model of prominence dynamics

Solar prominences are magnetic structures incarcerating cool and dense gas in an otherwise hot solar corona. Prominences can be categorized as quiescent and active. Their origin and the presence of cool gas ($～{10}^4$?K) within the hot ($～{10}^6\text{K}$) solar corona remains poorly understood. The structure and dynamics of solar prominences was investigated in a large number of observational and theoretical (both analytical and numerical) studies. In this paper, an analytic model of quiescent solar prominence is developed and used to demonstrate that the prominence velocity increases exponentially, which means that some gas falls downward towards the solar surface, and that Alfvén waves are naturally present in the solar prominences. These theoretical predictions are consistent with the current observational data of solar quiescent prominences.     

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.     

超临界正癸烷同轴剪切喷注热声振荡数值模拟

以液体火箭发动机同轴剪切喷嘴燃烧室作为研究对象,对超临界压力下低温正癸烷向高温正癸烷喷注过程中,由于高温正癸烷被快速冷却导致密度剧烈变化进而引发的热声振荡现象进行数值模拟。研究了出口压力、高温正癸烷流动速度与温度、低温正癸烷喷注速度与温度对热声波振幅与频率的影响。结果表明：当高温正癸烷被快速冷却时,其自身体积快速收缩,同时由于附近高温正癸烷的惯性导致压力先增大后减小,快速交替变化,从而产生热声波在高温正癸烷中传播。热声波振幅与频率的大小主要由高温正癸烷在不同压力与温度下的热物性决定。热声波的频率随着高温正癸烷声速增大而增大;热声波的振幅由高温正癸烷的相对压力系数与温度变化率共同决定。     

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。     

Absolute and Convective Instabilities of Circularly Polarized Alfvén Waves

We discuss the recent progress in studying the absolute and convective instabilities of circularly polarized Alfvén waves (pump waves) propagating along an ambient magnetic field in the approximation of ideal magnetohydrodynamics (MHD). We present analytical results obtained for pump waves with small dimensionless amplitude a, and compare them with numerical results valid for arbitrary a. The type of instability, absolute or convective, depends on the velocity U of the reference frame where the pump wave is observed with respect to the rest plasma. One of the main results of our analysis is that the instability is absolute when U _l < U < U _r and convective otherwise. We study the dependences of U _l and U _r on a and the ratio of the sound speed to the Alfvén speed b. We also present the results of calculation of the increment of the absolute instability on U for different values of a and b. When the instability is convective (U < U _l or U > U _r) we consider the signalling problem, and show that spatially amplifying waves exist only when the signalling frequency is in two symmetric frequency bands. Then, we write down the analytical expressions determining the boundaries of these frequency bands and discuss how they agree with numerically calculated values. We also present the dependences of the maximum spatial amplification rate on U calculated both analytically and numerically. The implication of the obtained results on the interpretation of observational data from space missions is discussed. In particular, it is shown that circularly polarized Alfvén waves propagating in the solar wind are convectively unstable in a reference frame of any realistic spacecraft.     

Synthesis of CME-Associated Moreton and EIT Wave Features from MHD Simulations

Soft X-ray (SXR) waves, EIT waves, and Hα Moreton waves are all associated with coronal mass ejections (CMEs). The knowledge of the characteristics about these waves is crucial for the understanding of CMEs, and hence for the space weather researches. MHD numerical simulation is performed, with the consideration of the quiet Sun atmosphere, to investigate the CME/flare processes. On the basis of the numerical results, SXR, EUV, and Hα images of the eruption are synthesized, where SXR waves, EIT waves, and Hα Moreton waves are identified. It confirms that the EIT waves, which border the expanding dimmming region, are produced by the successive opening (or stretching) of the closed magnetic field lines. Hα Moreton waves are found to propagate outward synchronously with the SXR waves, lagging behind the latter spatially by ～27 Mm in the simulated scenario. However, the EIT wave velocity is only a third of the Moreton wave velocity. The synthesized results also suggest that Hα± 0.45Å would be the best off-band for the detection of Hα Moreton waves.     

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.     

磁流体中间激波的相互作用

本文讨论磁流体中间激波的相互作用规律．主要结论：中间激波汇合的产物为后向快简单波、后向慢简单波或慢激波、接触间断、前向慢激波和前向快激波，其中后向波成份和接触间断很弱．当左（右）激波较强时，中国激波碰撞产物为后（前）向快激波、后（前）向慢简单波或慢激波、负（正）切向间断、前（后）向慢简单波和前（后）向快激波．     

Bifurcation in a 3-DOF Airfoil with Cubic Structural Nonlinearity

Limit cycle oscillations (LCOs) as well as nonlinear aeroelastic analysis of a 3-DOF aeroelastic airfoil motion with cubic restoring moments in the pitch degree of freedom are investigated.Aeroelastic equations of an airfoil with control surface in an incompressible potential flow are presented in the time domain.The harmonic balance (HB) method is utilized to calculate the LCO frequency and amplitude for the airfoil.Also the semi-analytical method has revealed the presence of stable and unstable limit cycles,along with stability reversal in the neighborhood of a Hopf bifurcation.The system response is determined by numerically integrating the governing equations using a standard Runge-Kutta algorithm and the obtained results are compared with the HB method.Also the results by the third order HB (HB3) method for control surface are consistent with the other numerical solution.Finally,by combining the numerical and the HB methods,types of bifurcation,be it supercritical,subcritical,or divergent flutter area are identified.