脉冲等离子体气动激励抑制翼型吸力面流动分离的实验

 为了提高等离子体气动激励控制附面层的能力,进行了脉冲等离子体气动激励抑制NACA 0015翼型失速分离的实验,研究了等离子体气动激励电压、位置、占空比和脉冲频率等对流动分离抑制效果的影响。在来流速度为72 m/s时,等离子体气动激励可以有效地抑制翼型吸力面的流动分离,翼型的升力增大约35%,翼型的临界失速迎角由18°增大到21°。实验结果表明：分离越严重,来流速度越大,有效抑制翼型失速分离的阈值电压越大;等离子体气动激励的最佳位置在流动分离起始点的前缘;调节占空比,可以在控制效果相当的情况下,降低等离子体气动激励所消耗的功率;当脉冲频率使斯特劳哈尔数等于1时,控制效果最佳。     

应用等离子体进行翼型前缘分离控制的数值模拟研究

将等离子体对中性气体的作用模型化为彻体力矢量,求解带源项的Navier-Stokes方程,数值模拟了等离子体激励器在NACA0015翼型大迎角下的分离控制效果,彻体力为净电荷在外加电场作用下的电场力.解拉普拉斯方程得到外加电场分布,等离子体中的净电荷分布由泊松方程给出.为了较好地模拟分离涡的发展,采用了雷诺平均与大涡模拟相结合的脱体涡模拟(Detached Eddy Simulation)方法.通过与实验结果对比,发现该模型能较好地模拟等离子体激励器的控制作用.     

激光干涉法测量微冲量数据处理方法

采用激光干涉法测量微冲量是一种新的微冲量测量方法。为了有效地测量10-4~10-8N.s量级的微小冲量,对力的加载过程进行定量的描述,在激光等离子体微推进器(μLPT)研究过程中采用该方法作为测试手段。介绍了测量系统的组成及测量方法,进行典型实验并提供了实验测量结果,重点讨论了测量系统的数据处理方法,对处理过程中存在的问题及数据处理方法的局限性进行了分析。研究工作对于激光干涉法应用于μN.s量级微冲量测量具有一定的参考价值。     

ROMAP: Rosetta Magnetometer and Plasma Monitor

The scientific objectives, design and capabilities of the Rosetta Lander’s ROMAP instrument are presented. ROMAP’s main scientific goals are longterm magnetic field and plasma measurements of the surface of Comet 67P/Churyumov-Gerasimenko in order to study cometary activity as a function of heliocentric distance, and measurements during the Lander’s descent to investigate the structure of the comet’s remanent magnetisation. The ROMAP fluxgate magnetometer, electrostatic analyser and Faraday cup measure the magnetic field from 0 to 32 Hz, ions of up to 8000 keV and electrons of up to 4200 keV. Additional two types of pressure sensors – Penning and Minipirani – cover a pressure range from 10⁻⁸ to 10¹ mbar. ROMAP’s sensors and electronics are highly integrated, as required by a combined field/plasma instrument with less than 1 W power consumption and 1 kg mass.     

利用等离子控制凸包流动分离的数值模拟

基于等离子发生器简化模型求解电势方程,得到电场及等离子分布,并将电场对等离子的作用力耦合到流动方程中.结果表明,电场力在电极交接处附近诱导气体运动并产生"壁面射流"效应,增加低能流体动量,显著改善附面层内速度分布;与无等离子控制措施相比,分离点位置最大延迟约4%特征尺寸,再附点位置最大提前约12%特征尺寸,分离范围明显减小.此外,电压较大、电极与流体接触式布置均能提高等离子控制流动分离的能力.      

Luminescent Nanocrystalline Silicon Carbide Thin Film Deposited by Helicon Wave Plasma Enhanced Chemical Vapour Deposition

Hydrogenated nanocrystalline silicon carbide (SiC) thin films were deposited on the single-crystal silicon substrate using the heli-con wave plasma enhanced chemical vapor deposition (HW-PECVD) technique. The influences of magnetic field and hydrogen dilution ratio on the structures of SiC thin film were investigated with the atomic force microscopy (AFM), the Fourier transform infrared ab-sorption (FTIR) and the transmission electron microscopy (TEM). The results indicate that the high plasma activity of the helicon wave mode proves to be a key factor to grow crystalline SiC thin films at a relative low substrate temperature. Also, the decrease in the grain sizes from the level of microcrystalline to that of nanocrystalline can be achieved by increasing the hydrogen dilution ratios. Transmis-sion electron microscopy measurements reveal that the size of most nanocrystals in the film deposited under the higher hydrogen dilution ratios is smaller than the doubled Bohr radius of 3C-SiC (approximately 5.4 nm), and the light emission measurements also show a strong blue photoluminescence at the room temperature, which is considered to be caused by the quantum confinement effect of small-sized SiC nanocrystals.     

In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections

The heliospheric counterparts of coronal mass ejections (CMEs) at the Sun, interplanetary coronal mass ejections (ICMEs), can be identified in situ based on a number of magnetic field, plasma, compositional and energetic particle signatures as well as combinations thereof. We summarize these signatures and their implications for understanding the nature of these structures and the physical properties of coronal mass ejections. We conclude that our understanding of ICMEs is far from complete and formulate several challenges that, if addressed, would substantially improve our knowledge of the relationship between CMEs at the Sun and in the heliosphere.     

Location of Magnetic Reconnection in the Magnetotail

It is a crucial issue to know where magnetic reconnection takes place in the near-Earth magnetotail for substorm onsets. It is found on the basis of Geotail observations that the factor that controls the magnetic reconnection site in the magnetotail is the solar wind energy input. Magnetic reconnection forms close to (far from) the Earth in the magnetotail for high (low) solar wind energy input conditions.With the early Vela spacecraft observations, it was believed that magnetic reconnection started inside the Vela position, likely at 15 R_E. The later ISEE/IRM observations put magnetic reconnection beyond 20 R_E. The Vela event studies were made for highly active conditions, while the ISEE/IRM survey studies were made for moderate or quiet conditions. The finding of the factor that controls the site of magnetic reconnection in the magnetotail resolves the apparent discrepancy among various spacecraft results, and suggests solar cycle variation of the magnetotail reconnection site.     

辉光放电等离子体对边界层流动控制的机理研究

本文求解电位势方程得到电场分布,假定电场强度大于击穿阈值的区域为等离子体区,给定电荷密度,得到了作用于流体上的电场力。通过求解带源项的NS方程,研究了一个大气压下的均匀辉光放电等离子体对边界层流动的影响,考察了电场力做功对流动的影响。本文研究结果同文献[6]一致,即电场力总体上使边界层流动加速。另外,电场力做功对流动参数的影响可以忽略。文献[6]给出的线化电场模型和本文得到的电场相比,具有较大的差别,该差别引起了流动参数显著差别。     

EUV and Radio Observations of an Equatorial Coronal Hole

An equatorial coronal hole has been observed on 18 and 19 October 1996 with SOHO-CDS and with the Nancąy Radioheliograph (RH). The CDS EUV line intensities are used to determine the coronal hole Differential Emission Measure (DEM); in turn this is used to compute the radio brightness temperature T_b at the observed frequencies, leaving the coronal electron temperature and density as free parameters. EUV line intensities, calculated from the derived models, show a good agreement with EUV observations. This revised version was published online in June 2006 with corrections to the Cover Date.