高比冲霍尔推力器启动特性研究

高比冲霍尔推力器从霍尔推力器研制初期就得到重视,但是与工程应用相关的参数对比、电流变化和振荡特性特的研究较少。通过测量推力器在不同工况下推力大小、电流变化和电流振荡波形,给出了HET 80HP高比冲霍尔推力器的性能特点和启动特性。研究结果表明,HET 80HP高比冲霍尔推力器相对于传统霍尔推力器,在较大流量和较高放电电压工况下具有更好的性能。冷启动时,正常磁场情况下放电电流存在电流尖峰,并且需要较长的时间才能达到相对稳定。不同磁场位形热启动情况下电流的变化过程表明,电流尖峰是否存在主要与磁场位形有关,启动时温度的高低与电流尖峰是否存在没有明显关系。此外,通过对比不同磁场下推力器比冲和平均频率的变化可知,推力器低频振荡平均频率的高低能够较好地反映推力器比冲的大小。     

Comparison of various cusp models with high- and low-resolution observations

Three major cusp models are systematically compared with low-resolution (large-scale) and high-resolution (fine-scale) low-altitude observations. Those models are (a) global magnetohydrodynamics (MHD) models (including MHD+drift models), (b) turbulent/diffusive entry models, and (c) direct flowing entry models. Although low-resolution data are mostly consistent with MHD models, high-resolution data mostly contradicts them. The data instead supports the other models in which the cusp is considered as a local `extra' open region. This is a good lesson to us: past supportive `tests' of MHD cusp models might have essential flaws in the methodology, and high-resolution data is necessary even for large-scale modelings.     

机翼动态气动特性实验研究

介绍了动态特性风洞实验的技术方案、测试系统和测试软件。对前缘后掠６０°的三角翼在迎角０°～９０°范围内快速上仰时的升力进行了测量。结果表明：机翼快速上仰时,随上仰速率增大最大升力系数增高,即动态升力效应更明显;失速迎角也增大。此外,给出了简缩频率、平均迎角、振荡振幅以及俯仰轴位置等对振荡机翼产生的非定常瞬时力的影响     

非结构网格高超声速化学非平衡MHD流场数值模拟

 在非结构网格上对考虑化学非平衡效应的二维高超声速磁流体绕钝头体流动进行了数值模拟。控制方程由二维理想磁流体动力学（MHD）方程和组元连续方程两部分组成,化学动力学模型为5组元17反应模型。MHD方程空间离散采用AUSM格式,时间推进采用显式5步龙格-库塔格式,并通过弱耦合的方式与化学反应控制方程结合在一起。计算模型为二维钝头体,外加磁场为偶极子场,磁场源位于钝头体内部。在高超声速来流条件下,对有、无磁场干扰,是否考虑化学反应下的4种工况进行了数值计算,得到了满意的结果,并与有限的参考文献进行了对比。结果表明本文发展的方法能准确地模拟考虑化学非平衡效应的高超声速MHD流场。     

MHD Waves and Heating in Coronal Holes

Coronal holes have been identified as source regions of the fast solar wind, and MHD wave activity has been detected in coronal holes by remote sensing, and in situ in fast solar wind streams. I review some of the most suggestive wave observations, and discuss the theoretical aspects of MHD wave heating and solar wind acceleration in coronal holes. I review the results of single fluid 2.5D MHD, as well as multi-fluid 2.5D MHD models of waves in coronal holes, the heating, and the acceleration of the solar wind be these waves.     

Saturn kilometric radiation as a monitor for the solar wind?

Since the Voyager mission it is known that Saturn Kilometric Radiation (SKR) is strongly influenced by external forces, i.e., the solar wind and in particular the solar wind ram pressure. Recent studies using Cassini data essentially confirmed these findings for particular periods during the first Cassini orbit of Saturn. The data coverage of SKR by the Cassini/RPWS experiment for the period of six months prior to Saturn Orbit Insertion (July 1, 2004) is rather continuous, whereas there are gaps in the solar wind plasma data. The strong correlation of SKR with the solar wind may provide an indication on the variations of the solar wind plasma, specifically during the gap periods. These periods lacking solar wind data are substituted by Ulysses solar wind data which have been propagated over ∼4 AU, applying magnetohydrodynamic propagation models. Cross correlation studies showed that Ulysses solar wind data can be taken as a substitute for missing Cassini data. The use of SKR as monitor for solar wind variations is discussed. With the present set of observations the SKR proxy lacks significant reliability.     

大功率霍尔推力器应用的滤波单元建模分析

放电电流低频振荡的抑制是霍尔推力器应用的主要问题之一,使用RLC滤波单元是抑制霍尔推力器放电电流低频振荡的最常用方法.对于大功率霍尔推力器而言,传统的RLC滤波器存在直流功耗大、发热严重的问题.提出并设计了一种新型耦合电感结构的滤波器,相比于传统的RLC滤波器,耦合电感结构的滤波器通过合理的参数设置存在明显的陷波特性,...     

汽车侧窗风振特性研究及控制

在对参考车型进行道路试验的基础上,应用CFD(计算流体力学)技术对豪华轿车的侧窗风振特性进行了仿真分析,分析结果表明后窗的风振比前窗剧烈得多;考查了频率及其强度与车速、车内体积、侧窗开启位置、侧窗开启数目的关系。根据风振产生的机理,采用两种措施对后窗的风振进行了控制,风振压力脉动最大降低了9dB。     

What are the physical mechanisms of eruptions and CMEs?

CMEs are due to physical phenomena that drive both, eruptions and flares in active regions. Eruptions/CMEs must be driven from initially force-free current-carrying magnetic field. Twisted flux ropes, sigmoids, current lanes and pattern in photospheric current maps show a clear evidence of currents parallel to the magnetic field. Eruptions occur starting from equilibria which have reached some instability threshold. Revisiting several data sets of CME observations we identified different mechanisms leading to this unstable state from a force free field. Boundary motions related to magnetic flux emergence and shearing favor the increase of coronal currents leading to the large flares of November 2003. On the other hand, we demonstrated by numerical simulations that magnetic flux emergence is not a sufficient condition for eruptions. Filament eruptions are interpreted either by a torus instability for an event occurring during the minimum of solar activity either by the diffusion of the magnetic flux reducing the tension of the restraining arcade. We concluded that CME models (tether cutting, break out, loss of equilibrium models) are based on these basic mechanisms for the onset of CMEs.