行波液体静压轴承浮力及其稳定方法的实验研究

提出了一种基于蠕动传输作用的新型行波液体静压轴承。首先基于行波液体静压轴承原理,建立了轴承原理验证装置。然后基于差动螺纹机构建立了轴承面倾斜调整机构,实现轴承的完全上浮。利用所开发的轴承验证装置,实验研究了行波液体静压轴承在上浮方向上有导轨时的轴承承载能力,证明了行波液体静压轴承及其稳定方法的可行性,并给出了驱动参数,例如:驱动电压和驱动频率,以及轴承间隙高度对轴承浮力稳态值的影响规律。     

A study of a long duration B9 flare-CME event and associated shock

We present and discuss here the observations of a small long duration GOES B-class flare associated with a quiescent filament eruption, a global EUV wave and a CME on 2011 May 11. The event was well observed by the Solar Dynamics Observatory (SDO), GONG H$\alpha$, STEREO and Culgoora spectrograph. As the filament erupted, ahead of the filament we observed the propagation of EIT wave fronts, as well as two flare ribbons on both sides of the polarity inversion line (PIL) on the solar surface. The observations show the co-existence of two types of EUV waves, i.e., a fast and a slow one. A type II radio burst with up to the third harmonic component was also associated with this event. The evolution of photospheric magnetic field showed flux emergence and cancellation at the filament site before its eruption.     

非均匀磁化等离子体层的电磁特性分析

基于分层传播原理提出了一种计算电磁波在非均匀磁化等离子体层中反射率和吸收率的模型,并数值分析了等离子体密度与碰撞频率,以及背景磁场强度对电磁波的反射和吸收特性的影响.研究表明:该法所得结果与文献的传播矩阵(SMM)法一致.数值分析发现:低密度高碰撞频率等离子体可减少等离子体层对入射波的功率反射;高密度高碰撞频率等离子体可改善其对入射波的功率反射宽频带吸收特性;背景磁场强度可明显改变等离子共振吸收频段.     

信号传输中的驻波处理

给出了驻波处理的简便方法,考察了有关的理论,给出了新的计算公式。     

一种改进的MUSCL格式

给出了一种改进的二阶精度的ＭＵＳＣＬ格式，并用来求解Ｅｕｌｅｒ方程，改进后的ＭＵＳＣＬ格式在线化插值步中，用Ｖａｎ Ｌｅｅｒ的插值斜率对特片变量进行插值，并对与熵波、剪切波对应的特片变量使用了小耗散的插值斜率，在迎风步采用Ｒｏｅ的近似黎曼解求得迎风通量。比较一维和二维的计算结果均可以看出，改进后的ＭＵＳＣＬ格式在消除数值振荡的同时，明显提高了流场间断的分辨率。     

真实火箭燃气流场的测量与数值仿真

对用激光－莫尔偏折法测出的真实火箭燃气射流流场进行了数值仿真,在计算中采用了二阶精度的ＭＵＳＣＬ格式,将三维问题转化为二维问题,结果表明,理论计算与实验测量结果符合较好。     

液态燃料喷注压力对旋转爆轰波影响的实验研究

为了深入研究液态燃料旋转爆轰波传播特性,以汽油为燃料,富氧空气为氧化剂,开展了液态燃料喷注压力对旋转爆轰波传播特性影响的实验研究。使用马尔文粒度仪对不同喷注压力下的雾化流场进行测量,结果表明在距离喷嘴出口各平面上的液滴粒径均满足正态分布;且随着喷注压力的增大,液滴雾化细度不断改善,在距离喷嘴出口60 mm处二次雾化基本完成。在汽油质量流率为96 g/s,当量比为1.3工况下,旋转爆轰波以单波模态传播,传播频率为2494 Hz,平均传播速度为1198 m/s。液态燃料的喷注压力对旋转爆轰波的传播特性具有较大的影响,当喷注压力为0.6 MPa时,由于液滴的雾化粒径较大,无法形成旋转爆轰波。随着喷注压力的增大,液滴雾化细度得到改善,旋转爆轰波可以成功起爆并稳定自持传播,传播速度和平均压力均逐渐增大,传播稳定性也得到改善。     

碳化硅颗粒增强铝基复合材料弹性常数测量

为研究粉末冶金制备的碳化硅颗粒增强铝基复合材料(SiCp/Al)中SiCp含量对材料机械性能的影响,使用弹性波法测量了SiCp含量不同的标准试样的弹性常数矩阵.利用Christoffel方程建立了横观各向同性材料波速与弹性常数之间的关系,介绍了水浸斜入射法测量准横波和准纵波波速的基本原理和测量过程,基于上述原理进行了试验,计算出了被测试件的弹性常数.结果表明,SiCp/Al沿挤压方向的机械性能最高,并且随着SiCp含量的增加,弹性常数变大,材料的强度升高.     

Vertical wavenumber spectra of atmospheric ozone measured from ozonesonde observations

Vertical profiles of ozone have been measured at balloon altitudes. Our purpose is to examine the character of vertical wavenumber spectra of ozone fluctuations, to assess the possible roles of gravity wave field in ozone fluctuations, and to determine dominant vertical wavelengths of ozone spectra. Vertical wavenumber spectra of 12 ozone fluctuations obtained during June–August 2003 are presented. Results indicate that mean spectral slopes in the wavenumber range from 4.69 × 10⁻⁴ to 2.50 × 10⁻³ cyc/m are about −2.91 in the troposphere and −2.87 in the lower stratosphere, which is close to the slope of −3 predicted by current gravity wave saturation models. The consistency of the observed spectral slopes with the value of −3 predicted by current gravity wave saturation models suggests that the observed ozone fluctuations are due primarily to atmospheric gravity waves. At m = 1/(1000 m) the mean spectral amplitude is over 30 times larger in the lower stratosphere than in the troposphere. Mean vertical wavenumber spectra in area-preserving form reveal dominant vertical wavelengths of ∼2.6 km in the troposphere and ∼2.7 km in the lower stratosphere, which is consistent with the values varying between 1.5 and 3.0 km estimated from the velocity field and temperature field at these heights.     

Cosmological Shock Waves

Large-scale structure formation, accretion and merging processes, AGN activity produce cosmological gas shocks. The shocks convert a fraction of the energy of gravitationally accelerated flows to internal energy of the gas. Being the main gas-heating agent, cosmological shocks could amplify magnetic fields and accelerate energetic particles via the multi-fluid plasma relaxation processes. We first discuss the basic properties of standard single-fluid shocks. Cosmological plasma shocks are expected to be collisionless. We then review the plasma processes responsible for the microscopic structure of collisionless shocks. A tiny fraction of the particles crossing the shock is injected into the non-thermal energetic component that could get a substantial part of the ram pressure power dissipated at the shock. The energetic particles penetrate deep into the shock upstream producing an extended shock precursor. Scaling relations for postshock ion temperature and entropy as functions of shock velocity in strong collisionless multi-fluid shocks are discussed. We show that the multi-fluid nature of collisionless shocks results in excessive gas compression, energetic particle acceleration, precursor gas heating, magnetic field amplification and non-thermal emission. Multi-fluid shocks provide a reduced gas entropy production and could also modify the observable thermodynamic scaling relations for clusters of galaxies.