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.      

“后方法”时代基础英语立体教学模式构建

"后方法"是一种基于语境的教学主张和一系列宏观策略,并从根本上超越传统"教学法"概念的外语教学思想,它不是否定教学法而是强调将各种教学法"本土化"。在后方法教学观指导下,通过教学观念、教学手段、教学内容、教学形式、教学评价等的立体化,构建基础英语立体教学模式,实现教师教学实践理论化,践行"教师赋权"和"学习者自主"。     

A Self-Consistent Determination of the Temperature Profile and The Magnetic Field Geometry in Winds of Late-Type Stars

Cool giant and supergiant stars generally present low velocity winds with high mass-loss rates. Several models have been proposed to explain the acceleration process of these winds. Although dust is known to be present in these objects, the radiation pressure on these particles is uneffective in reproducing the observed physical parameters of the wind. The most promising acceleration mechanism cited in the literature is the transference of momentum and energy from Alfvén waves to the gas. Usually, these models consider the wind to be isothermal. We present a stellar wind model in which the Alfvén waves are used as the main acceleration mechanism, and determine the temperature profile by solving the energy equation taking into account both the radiative losses and the wave heating. We also determine, self-consistently, the magnetic field geometry as the result of the competition between the magnetic field and the thermal pressure gradient. As the main result, we show that the magnetic geometry presents a super-radial index in the region where the gas pressure is increasing. However, this super-radial index is greater than that observed for the solar corona.     

Fluid instabilities around accreting X-ray sources

Some aspects of fluid instabilities occurring in the magnetospheres of accreting neutron stars are discussed. It is pointed out that (i) in the absence of strong differential rotation, the accreting plasma should be drawn out into spiralling, sheet-like structures, resulting in efficient mixing between the two media; (ii) the Rayleigh-Taylor instability also acts to limit the X-ray luminosity in super-critical sources; and (iii) magnetic shear has a strong stabilizing influence on Kelvin-Helmholtz modes, and its presence may allow substantial amounts of material to be supported around the magnetosphere.     

损失及落后角代理模型在多级轴流压气机特性预测中的应用

为了提高轴流压气机设计能力,进而提高发动机的特性,需要掌握一种能够较好预测轴流压气机的压比、效率等特性的方法。结合运用三元流动理论和传统损失落后角模型计算出的压气机流场数据,利用正则化径向基函数神经网络取代经验公式搭建了一种新的损失及落后角模型,计算了E3十级高压压气机的特性;并分别研究了不进行正则化和进行正则化对损失及落后角预测的影响与其对压气机效率和压比特性预测的影响。结果表明,在多级压气机中,在训练样本区分转静子、区分转速、区分工况条件下,使用正则化的径向基神经网络代理模型在大部分情况下能够较好地预测损失、落后角及多级压气机整体特性,但是对沿叶高分布的损失及落后角预测能力还有待提高。     

Application of ADER Scheme in MHD Simulation

The Arbitrary accuracy Derivatives Riemann problem method(ADER) scheme is a new high order numerical scheme based on the concept of finite volume integration,and it is very easy to be extended up to any order of space and time accuracy by using a Taylor time expansion at the cell interface position.So far the approach has been applied successfully to flow mechanics problems.Our objective here is to carry out the extension of multidimensional ADER schemes to multidimensional MHD systems of conservation laws by calculating several MHD problems in one and two dimensions: (ⅰ) Brio-Wu shock tube problem,(ⅱ) Dai-Woodward shock tube problem,(ⅲ) Orszag-Tang MHD vortex problem.The numerical results prove that the ADER scheme possesses the ability to solve MHD problem,remains high order accuracy both in space and time,keeps precise in capturing the shock.Meanwhile,the compared tests show that the ADER scheme can restrain the oscillation and obtain the high order non-oscillatory result.     

Spectral analysis of 3D MHD models of coronal structures

We study extreme-ultraviolet emission line spectra derived from three-dimensional magnetohydrodynamic models of structures in the corona. In order to investigate the effects of increased magnetic activity at photospheric levels in a numerical experiment, a much higher magnetic flux density is applied at the photosphere as compared to the Sun. Thus, we can expect our results to highlight the differences between the Sun and more active, but still solar-like stars. We discuss signatures seen in extreme-ultraviolet emission lines synthesized from these models and compare them to observed signatures in the spatial distribution and temporal evolution of Doppler shifts in lines formed in the transition region and corona. This is of major interest to test the quality of the underlying magnetohydrodynamic model to heat the corona, i.e. currents in the corona driven by photospheric motions (flux braiding).     

大弯角开槽叶栅槽道位置与结构研究

为拓宽大弯角扩压叶栅可用攻角范围,优化叶片吸力面流动分离结构,本文以一大弯角叶栅为研究对象,对叶片采用压力面到吸力面打通的双“C”型槽道结构处理,在保持槽道长度及其他参数不变的条件下,设置85%、80%、75%、70%轴向弦长四个出口位置研究槽道出口位置对叶栅性能的影响。研究发现,特定攻角下,槽道出口位于吸力面角区分离线起始点之后、尾缘分离线之前,对吸力面流动分离的控制效果较佳;在全攻角范围,槽道出口则取在0o攻角对应较佳出口位置为好。为减小槽道内总压损失,本文提出了一种“SC”型槽道改进结构,在80%轴向弦长槽道出口位置处与双“C”型槽道以及原型叶栅进行对比。结果表明,“SC”型槽道结构相比于双“C”型槽道结构,叶栅尾迹损失及槽道内总压损失减少,槽道出口射流速度提高,叶片尾缘处静压升高;相比于原型叶栅则能有效降低其在全攻角范围内的总压损失,基本消除叶片吸力面附面层分离,削弱角区分离,提高叶栅的扩压能力。     

超声速非平衡电离磁流体动力技术实验系统

介绍了超声速非平衡电离磁流体动力技术实验系统的设计思想和组成,设计、制作了马赫数为3.5的吸气式双喉道风洞,采用以陶瓷板为阻挡介质的电容耦合射频阻挡放电,实现了超声速流场中大体积、连续、稳定、均匀等离子体的产生.主要结论有:实验测试风洞稳定工作时间为18s,稳定运行时实验段静压为650Pa;电容耦合射频放电典型工作状态下,通过伏安诊断法测出超声速条件下等离子体的电导率为1.27×10-3S/m.      

月球尾迹的二维MHD模拟

采用理想的二维单流体MHD方程,对太阳风通过月球时所形成的尾迹结构进行数值模拟,得到了太阳风尾迹的粒子分布及磁场分布.模拟结果表明,在月球背阳面的本影区,太阳风粒子密度急剧下降,行星际磁场增强.当行星际磁场与太阳风流动方向平行时,尾迹被拖得很长,而磁场与太阳风流动方向垂直时,尾迹较短.