八面体桁架结构在内冷通道中的流动传热特性研究

为探究八面体桁架结构在航空发动机热端部件内冷通道中的可应用性,掌握八面体桁架结构的流动传热特性,本文采用理论推导和三维数值模拟的方法,对八面体桁架单体的有效导热系数以及八面体桁架阵列结构的流动结构和传热性能开展了研究。首先,针对八面体桁架单体结构,推导出了考虑节点效应的有效导热系数关系式,并通过与数值计算结果对比,验证了其有效性。其次,针对八面体桁架阵列结构,开展了整体结构的三维数值计算,分析了其内部通道的流动结构和温度分布,获得了不同结构的流动阻力和对流传热系数随雷诺数的变化规律。最后,考虑到结构的综合传热性能,本文针对不同孔隙率的八面体桁架阵列结构,进行了基于相同泵功率下努塞尔数的对比。根据计算结果,本文给出了获得最佳传热性能的无量纲直径范围0.07~0.08,相应的孔隙率变化范围 0.872~0.841。分析其原因,由于随着结构孔隙率的减小,即固体率的增加,对流传热强度不断提高,然而,当孔隙率减小到84.1%以下时,由于内通道中流动阻力骤然增大,导致传热效率降低。将八面体桁架结构应用于航空发动机热端部件内冷通道中,是同时出于高效冷却和力学性能的考虑,本文掌握八面体桁架阵列结构的流动传热特性,为其在实际工程中的应用提供了理论支撑。     

基于正交实验设计的螺旋通道变流器水动力性能数值分析

变流器是螺旋通道磁流体推进器推进通道中重要的水力部件之一,变流器的设计影响着推进器的水力性能和推进性能。提出了基于四阶贝塞尔曲线的螺旋通道变流器三维建模方法,明确了变流器的结构参数;采用正交实验设计方法,选用五因素四水平正交设计表基于CFD方法分析了变流器结构参数对螺旋通道水动力学性能的影响及其变化规律。分析结果表明螺旋通道导流器会大幅减小水力损失,整流器会增加水力损失,但能提高整流效果。分析结果可以为螺旋通道磁流体推进器的水力优化及推进性能提升提供有意义的指导作用。     

Exploring the global shock scenario at multiple points between sun and earth: The solar transients launched on January 1 and September 23, 1978

We revisit the transient interplanetary events of January 1 and September 23, 1978. Using in-situ and remote sensing observations at locations widely separated in longitudes and distances from the Sun, we infer that in both cases the overall shock surface had a very fast “nose” region with speeds >900 and >1500 km⁻¹ in the January and September events, respectively, and much slower flank speeds (∼600 km⁻¹ or less), suggesting a shock surface with a strong speed gradient with heliospheric longitude. The shock-nose regions are thus likely efficient acceleration sites of MeV ions, even at 1 AU from the Sun. Our 3D magnetohydrodynamics modeling suggests that a 24° × 24° localized disturbance at 18 solar radii injecting momentum 100 times the background solar wind input over 1 h can produce a disturbance in semi-quantitative agreement with the observed shock arrival time, plasma density and velocity time series in the January 1978 event.     

Azimuthal propagation of Pc5 geomagnetic field pulsations in the southern polar cap

A statistical analysis of low frequency geomagnetic fluctuations at the two Antarctic stations Mario Zucchelli Station (geographic coordinates: 74.7°S, 164.1°E; corrected geomagnetic coordinates: 80.0°S, 306.8°E) and Dumont D’Urville (geographic coordinates: 66.7°S, 140.0°E; corrected geomagnetic coordinates: 80.4°S, 236.0°E) is shown. The analysis focuses on power spectra, coherence and phase difference between the stations, which are both located in the polar cap, with a 5-h magnetic local time displacement along a geomagnetic parallel; in this situation, the phase difference between geomagnetic fluctuations indicates the direction of their azimuthal propagation. Coherent fluctuations have been found to occur preferably when both stations are on the same side (dawnward or duskward) with respect to the polar cusp; moreover, around local magnetic midnight, they occur essentially during open magnetospheric conditions. The phase difference for coherent fluctuations indicates a propagation direction away from local geomagnetic noon and midnight. Also the analysis of three individual pulsation events, occurring at different times during the day, is shown; they are characterized at the two stations by simultaneous, coherent fluctuations, whose phase difference finds correspondence with the statistical behaviour.     

A MHD-turbulence model for solar corona

The disposition of energy in the solar corona has always been a problem of great interest. It remains an open question how the low temperature photosphere supports the occurence of solar extreme phenomena. In this work, a turbulent heating mechanism for the solar corona through the framework of reduced magnetohydrodynamics (RMHD) is proposed. Two-dimensional incompressible long time simulations of the average energy disposition have been carried out with the aim to reveal the characteristics of the long time statistical behavior of a two-dimensional cross-section of a coronal loop and the importance of the photospheric time scales in the understanding of the underlying mechanisms. It was found that for a slow, shear type photospheric driving the magnetic field in the loop self-organizes at large scales via an inverse MHD cascade. The system undergoes three distinct evolutionary phases. The initial forcing conditions are quickly “forgotten” giving way to an inverse cascade accompanied with and ending up to electric current dissipation. Scaling laws are being proposed in order to quantify the nonlinearity of the system response which seems to become more impulsive for decreasing resistivity. It is also shown that few, if any, qualitative changes in the above results occur by increasing spatial resolution.     

Geosynchronous magnetic field response to the large and fast solar wind dynamic pressure change

We present a comparison of large and sharp solar wind dynamic pressure changes, observed by several spacecraft, with fast disturbances in the magnetospheric magnetic field measured by the GOES-8, 9 and 10 geosynchronous satellites. Almost 400 solar wind pressure changes in the period 1996–2003 were selected for this study. Using the large statistics we confirmed that increases (decreases) in the dynamic pressure always results in increases (decreases) in the magnitude of geosynchronous B_z component. The amplitude of the geosynchronous B_z response strongly depends on the location of observer relative to the noon meridian, from the value of solar wind pressure before the disturbance arriving and firstly – from the amplitude of the pressure change.     

航天磁悬浮发射脉冲磁流体供能系统方案分析

针对航天发射低成本、安全可靠运输方式的需要,阐述分析了航天运载器磁悬浮发射概念及其能量供给需求。在重点研究了固体火箭燃料脉冲磁流体发电机的关键技术及发展水平后,基于俄罗斯四台“Sakhalin”脉冲磁流体发电机单元,提出和设计了用于助推发射100吨地面载荷(飞行器和磁悬浮橇体)实现4g加速度的能量供给方案,同时分析磁悬浮发射过程中三相直线电机加速和控制的特点,提出可行的逆变器功率转换系统方案。     

Closing address

Impressions from the workshop are summarized. Difficulties within the present observational and theoretical context are outlined and directions for fruitful future work are indicated. The workshop subtitle, the interface between MHD and plasma physics, still appears to be a goal for the future, though some encouraging results have been reported at this workshop.     

行星际慢激波的传播和演化

采用二维理想MHD模型，分别在日球赤道面(二维二分量模型)和日球子午面(二维三分量模型)内研究太阳风中慢激波的传播和演化规律．结果表明，慢激波在向外传播的过程中逐渐演化为由原慢激波和新产生的快激波构成的激波系统，该激波系统在子午面内相对慢激波源中心法线基本对称，而在赤道面内则是不对称的：快激波阵面和慢激波阵面之间存在一个切触点，该处两个激波合并，蜕化为气体激波．上述切触点相对激波源中心法线东偏，且东偏角度在激波系统向外传播过程中不断增加．初步分析表明，行星际磁场的螺旋结构是产生日球赤道面内慢激波传播和演化的东西不对称性的主要原因．     

黄道面内行星际激波相互碰撞作用过程研究—能量效应

本文用两维半MHD数值模型,数值模拟研究了两邻近扰动源所产生的激波在行星际空间黄道面内不同能量时的相互碰撞过程。在内边界(18R_s)两扰动中心的间距取为36°。结果表明:两弱激波(速度在500km/s左右以下)不会产生汇合,而是各自独立地传播;两中等强度激波(速度在1000km/s左右)将发生汇合,但在IAU尚可分辨;两强激波(速度在2000km/s以上)则在1AU以内已发生汇合,汇合后形成一个新激波,其磁场结构与单激波明显不同。激波能量越大,两激波汇合的越快。