引导场对无碰撞电流片低频电磁不稳定性的影响

通过数值求解无碰撞电流片中可压缩磁流体力学模型下得到的一般形式的色散关系,讨论了无碰撞电流片中引导场对低频电磁波不稳定性的影响.结果表明,平衡态磁场中的引导场,对于三维扰动传播的波不稳定性有很强的影响.(1)在电流片中间平面上(z=0),无引导场时,没有不稳定性发生,但若存在引导场,不稳定性便发生,并随着引导场的增强,不稳定性明显增强,不稳定的波模可能是低混杂模.(2)在中间平面附近(z=0.2),电流片是不稳定的.随着引导场的增强,不稳定性增长率明显地增强,不稳定的波模从平行和反平行两个方向传播变为反平行方向一个方向传播,并且是斜传播的,具有低频哨声模或低混杂模的特征.(3)在电流片边缘附近(z=0.8),引导场对不稳定的波模和增长率没有明显影响,不稳定的波模都是准平行的哨声波.      

面内强磁场下铁磁板壳的自由振动

本文研究了面内强磁场环境下铁磁板壳的自由振动问题。基于Eringen-Maugin的关于磁弹性作用的理性力学模型,从理论上推导了一般壳体在磁场中的运动方程,进而求解了面内强磁场作用下的小磁化率悬臂铁磁薄板自由振动频率。数值计算结果表明,本文模型和已有的实验结果吻合很好。     

动网格在固体火箭发动机非稳态工作过程中的应用

利用Fluent流场计算软件、动网格技术、UDF文件,用DEFINE_GRID_MOTION定义燃面边界的移动,用DEFINE_PROFILE定义边界类型,考虑侵蚀燃烧、压强变化率对推进剂燃速的影响,对轴对称变截面固体火箭发动机的非稳态工作过程内流场进行了瞬态分析.得到了变截面轴对称固体发动机稳态工作过程中装药燃面推移图像,并得到了发动机内弹道参数分布云图及其随时间的变化规律.     

直升机附件舱温度场的数值模拟

为考查某型直升机附件舱的热控制能力,采用有限元软件分析了其在强制冷却和自然冷却情况下的温度场分布.应用非结构化网格和有限体积法进行计算区域和控制方程的离散,采用标准k-ε模型封闭湍流控制方程.针对3种冷却系统设计方案,分析了不同冷却气流进口尺寸、相对位置以及不同附件散热量对附件舱温度分布的影响,计算了自然冷却情况下附件舱密闭时的温度场.计算和试验结果均表明,所采用的冷却方案可以满足附件舱冷却的需要.      

单一压力容器镍氢电池组几何参数对其温度场的影响

 针对实际空间用单一压力容器(IPV)镍氢电池组的传热特点,建立其瞬态热分析的数学物理仿真模型。通过设计改变电池组几何参数,包括电池组底板厚度、套筒高度和厚度,采用有限差分法,对比模拟研究电池组在飞船实际运行条件下几何参数对其温度场的影响。结果表明：套筒厚度对电池组温度场的影响最为敏感,增大套筒厚度可明显缩短电池组热系统达到平衡态的响应时间;其次是套筒高度;改变底板厚度对电池组温度场变化影响不明显。该研究为镍氢电池组的结构优化和热控制研究提供理论基础。     

温度对磁屏蔽霍尔推力器磁场构型的影响研究

霍尔推力器磁路设计主要通过常温静态磁场仿真得到，并实测推力器非工作状态常温磁场进行复核。大功率霍尔推力器将面临更为严峻的热问题，推力器工作时磁路系统受高温影响，因此在常温下仿真得到的磁场位形会因温度升高而产生偏移，不能反映推力器真实工作时的磁场情况。为研究霍尔推力器工作时热量对磁路系统的影响，通过热磁耦合仿真对10kW磁屏蔽霍尔推力器的热态磁场分布进行研究，并对热态、常温仿真结果进行了对比，发现在阳极附近的径向磁感应强度Br的差异比放电室出口更大。常温设计的磁屏蔽构型在热态时偏离磁屏蔽，磁场和壁面最大不符合度达到13%，通过陶瓷出口型面修正后重新获得磁屏蔽效果，使最大不符合度降低到4.8%以下。合理热设计有助于降低热载荷，热仿真得到磁路系统最高温度低于500℃，低于0.78倍的居里温度Tc磁性急剧转变点，不会出现磁性能急剧下降，但热量对磁屏蔽霍尔推力器磁场构型的影响是应该考虑的。     

车载中频高速同步发电机设计

对车载中频高速同步发电机设计思路和设计特点进行阐述。根据设计思路和设计特点制造了试验样机,在制造过程中着重对磁极线圈的绑扎与固定、三相旋转整流器的内部结构做了改进。进行了电机性能的试验分析,对采取的技术措施进行验证,验证了设计方法的有效性。这为同类电机设计提供了参考。     

Simulation study of motion of charged particles trapped in Earth’s magnetosphere

This article aims to understand the motion of the charged particles trapped in the Earth’s inner magnetosphere. The emphasis is on identifying the numerical scheme, which is appropriate to characterize the trajectories of the charged particles of different energies that enter the Earth’s magnetosphere and get trap along the magnetic field lines. These particles perform three different periodic motions, namely: gyration, bounce, and azimuthal drift. However, often, the gyration of the particle is ignored, and only the guiding center of the particle is traced to reduce the computational time. It is because the simulation of all three motions (gyro, bounce, and drift) together needed a robust numerical scheme, which has less numerical dissipation. We have developed a three-dimensional test particle simulation model in which the relativistic equation of motion is solved numerically using the fourth and sixth-order Runge-Kutta methods. The stability of the simulation model is verified by checking the conservation of total kinetic energy and adiabatic invariants linked with each type of motion. We found that the sixth-order Runge-Kutta method is suitable to trace the complete trajectories of both proton and electron of a wide energy range, 5 keV to 250 MeV for L = 2 – 6. We have estimated the bounce and drift periods from the simulations, and they are found to be in good agreement with the theory. The study implies that a simulation model with sixth-order Runge-Kutta method can be applied to the time-vary, non-analytical form of magnetic configuration in future studies to understand the dynamics of charged particles trapped in Earth’s magnetosphere.     

Observations of the local interstellar medium with the Extreme Ultraviolet Explorer

Because of the strong absorption of extreme ultraviolet radiation by hydrogen and helium, almost every observation with the Extreme Ultraviolet Explorer (EUVE) satellite is affected by the diffuse clouds of neutral gas in the local interstellar medium (LISM). This paper reviews some of the highlights of the EUVE results on the distribution and physical state of the LISM and the implications of these results with respect to the interface of the LISM and the heliosphere. The distribution of sources found with the EUVE all-sky surveys shows an enhancement in absorption toward the galactic center. Individual spectra toward nearby continuum sources provide evidence of a greater ionization of helium than hydrogen in the Local Cloud with an mean ratio of H I/He I of 14.7. The spectral distribution of the EUV stellar radiation field has been measured, which provides a lower limit to local H II and He II densities, but this radiation field alone cannot explain the local helium ionization. A combination of EUVE measurements of H I, He I, and He II columns plus the measurement of the local He I density with interplanetary probes can place constraints on the local values of the H I density outside the heliosphere to lie between 0.15 and 0.34 cm^–3 while the H II density ranges between 0.0 and 0.14 cm^–3. The thermal pressure (P/k = nT) of the Local Cloud is derived to be between 1700 and 2300 cm^–3 K, a factor of 2 to 3 above previous estimates.     

Detailed magnetic structure and stochastic threshold

Non-linear evolution of reconnection is too slow to explain-by itself-fast phenomena such as internal disruptions in tokamaks or flares in the solar atmosphere. It has been proposed that the change in topology could lead to field line stochastization, and hence to highly increased transport. An important objection to this idea is that the increase of transport coefficients should smoothly follow the amplitude of the perturbation, while the observations show a catastrophic transition. We have shown 1) that the shape of the structures (and not only their size or amplitude) evolve during non-linear evolution 2) that the stochastic threshold can be strongly influenced by the detailed shape. Therefore, sharp transitions can appear during the evolution, due to the combination of these two effects. We will first consider an idealized situation, namely the two-waves problem in slab geometry, for which we will study the effect of the separatrix shape on the stochastic threshold. In the second part, we will present an application to the internal disruption in tokamaks, with anm=1 perturbation in a toroidal magnetic configuration. In the last part, we will discuss possible applications of the studies on shape effects to the behaviour of trapped particles in structures of the solar atmosphere.