磁流体管流准一维模型的数值验证与性能分析

为了快速分析磁流体管流,采用涡轮喷气发动机模型对磁流体管流进行类比分析,引入变截面管流理论和修改过的多变效率表达式,推导了磁流体发电器和加速器的准一维模型,采用二维数值方法验证了准一维模型的可行性,利用该准一维模型对磁流体管流进行了性能分析,结果表明,多变效率的引入使准一维模型更加完整,当负载系数不变时,磁流体装置中的平均马赫数越低,其等熵效率越高。     

一类TVD型组合差分方法及其在磁流体数值计算中的应用

根据太阳风数值模拟的特点，考虑到算法的质量（收敛速度、稳定性、精度等），结合磁流体数值计算的特性，对三维球坐标磁流体动力学（MHD）方程组中的流体部分采用一种修正Lax-Friedrichs差分法而对磁场部分采用MacComack格式，发展了一类快捷的具有TVD特性的组合数值新方法，作为格式的检验，在一维情况下，将其与PPM格式进行了比较，对一维快慢磁流体激波问题得到了与PPM格式精度相同的结果，然后将其诮到定态太阳风的数值模拟上，在不同等离子体β情形下，可得到理想的太阳风定态结构，为今后将此数值模式应用到具有复杂磁场位型或三维直实太阳风暴的数值模拟研究奠定了基础。     

Splitting Based Scheme for Three-dimensional MHD with Dual Time Stepping

A new hybrid numerical scheme of combining an E-CUSP (Energy-Convective Upwind and Split Pressure) method for the fluid part and the Constrained Transport (CT) for the magnetic induction part is proposed. In order to avoid the occurrence of negative pressure in the reconstructed profiles and its updated value, a positivity preserving method is provided. Furthermore, the MHD equations are solved at each physical time step by advancing in pseudo time. The use of dual time stepping is beneficial in the computation since the use of dual time stepping allows the physical time step not to be limited by the corresponding values in the smallest cell and to be selected based on the numerical accuracy criterion. This newly established hybrid scheme combined with positivity preserving method and dual time technique has demonstrated the accurateness and robustness through numerical experiments of benchmark problems such as the 2D Orszag-Tang vortex problem and the 3D shock-cloud interaction problem.      

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.     

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.     

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.     

MKDVB and CKB Shock Waves

This review presents results from MKDVB and CKB systems to illustrate the properties of magnetohydrodynamics intermediate shock waves. The intermediate shocks can have a family of shock structures; the shock structure and the evolution are related. Furthermore, there exists a class of time-dependent intermediate shocks. This revised version was published online in August 2006 with corrections to the Cover Date.     

基于加速栅溅射腐蚀失效的离子推力器寿命预测

离子推力器加速栅溅射腐蚀失效是制约离子推力器寿命的关键失效模式之一.针对离子推力器长寿命、多功率条件下运行的特点,基于坑和凹槽的溅射腐蚀数据,建立模型对其进行寿命预测.通过研究离子推力器加速栅中心凹槽腐蚀深度在不同功率段下随工作时间的变化规律发现:运行功率顺序对加速栅凹槽腐蚀率影响较小,进而采用累积损伤理论建立离子推力器多功率段下运行的寿命预测模型.最后, 对美国的NASA's Evolutionary Xenon Thruster(NEXT)进行了寿命预测,预测结果寿命为46041h,与试验结果符合较好.      

冲压加速器的冷发射试验

冲压加速器是一种利用化学能将弹丸加速到7km／s的新装置，在航天工程和常规兵器领域具有极大的潜在应用前景，美、法、德、日、韩等发达国家纷纷开展此项研究，并取得了令人鼓舞的初步成果。本文首先描述冲压加速器的原理，然后介绍了我国第一座冲压加速器─—气动中心超高速所的37mm口径冲压加速器，以及已成功完成的冷发射试验。     

磁流体斜激波的汇合

本文讨论磁流体快、慢激波的汇合作用规律,主要结论如下:(1)两个前向快激波汇合之后,形成一更强的前向快激波,尾随一前向慢稀疏波、一正接触间断(后侧密度大于前侧)、一后向慢激波和一后向快稀疏浚。(2)两个前向慢激波汇合之后,形成一更强的前向慢激波,尾随一正接触间断、一后向慢稀疏波和一后向快激波2在前向慢激波前方出现一前向快波,它或为稀疏浚(中、小激波角情况),或为激波(大激波角情况).(3)前向快激波会追上前向慢激波而发生汇合,之后互换位置且强度减弱,尾随一正接触间断和一后向稀疏波对。