碳纤维增强可溶性聚芳醚树脂基复合材料的表面与界面

首次对碳纤维增强含二氮杂萘酮联苯型聚芳醚砜酮(PPESK)基高性能热塑性树脂基复合材料的界面进行了研究。采用空气冷等离子体处理方法对碳纤维表面进行处理。用XPS测试分析了不同等离子体处理时间对CF-原丝表面元素组成的影响及其变化规律。用FT-IR测试分析了经等离子体处理前后碳纤维表面的官能团的变化。采用动态接触角测试分析了不同处理时间下,碳纤维浸润性的变化规律,进一步分析了复合材料界面的粘结机理。采用AFM测试分析等离子体处理时间对碳纤维表面粗糙度的影响。利用ILSS测试方法表征了碳纤维/PPESK复合材料的层间剪切强度,确定了最佳的等离子体处理条件。利用SEM观察了碳纤维/PPESK树脂基复合材料的层间剪切破坏形貌。结果表明:对碳纤维的最佳的等离子体处理条件为:处理功率200W,处理时间15m in。在这一条件下处理碳纤维,复合材料的ILSS值最达可提高13.5%。经过适当的等离子体处理后,碳纤维表面的极性基团的含量、浸润性能和粗糙度均得到改善,增强纤维与树脂基体间界面的粘结性能得到提高,从而提高了复合材料的力学性能。     

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.     

基于磁致伸缩作动器的主动隔振系统分析

基于材料的本构方程,建立主动隔振系统的模型,并对其动力学和控制稳定性进行了研究。分析和仿真表明,上层质量对主动控制力的影响较大,采用中间质量的加速度作为反馈量时下层刚度对隔振效果影响明显。在系统的前馈控制形式中,振动频率的变化不会影响系统稳定性,但反馈环节将会降低稳定裕度;在反馈控制形式中,随着振动频率的增大,次通道的延迟作用可能使系统不稳定。