用子波系数概率密度函数研究湍流多尺度结构的间歇性

用热线风速仪在充分发展平板湍流边界层中测量流向速度信号的时间序列并进行湍流多尺度结构统计特性的实验研究。用热线风速仪以高于对应最小湍流时间尺度的分辨率精细测量风洞中平板湍流边界层不同法向位置的流向速度分量的时间序列信号,用子波分析对湍流脉动速度信号进行多尺度分解,将推广的自相似性(ESS)应用于子波分析。用子波系数的概率密度函数验证了多尺度相干结构对间歇性的影响,并证明与距壁面距离有关。对比研究了提取湍流边界层多尺度相干结构前后湍流多尺度结构函数间歇性的变化规律及概率密度函数的变化规律,验证了多尺度相干结构是湍流边界层产生奇异标度律的原因。当这些相干结构被分离出后,由子波系数计算的ESS标度律就回到K olm ogorov线性标度律,这一现象在整个湍流边界层都是很明显的。      

可压缩湍流的多尺度分析

作者的研究团队近几年在可压缩湍流的多尺度性质方面开展了系统的研究工作。通过多过程分解,研究了可压缩湍流中的速度和热力学量的剪切部分、胀压部分、伪声模态、声模态、熵模态的多尺度性质,并总结了各类可压缩条件下的速度和热力学量的谱的标度律。通过滤波方法,研究了动能和热力学量的多尺度传输现象,并重点分析了可压缩性对动能胀压部分的多尺度传输的影响。在可压缩均匀剪切湍流中,可压缩效应更加明显,可压缩湍动能和耗散率等物理量的马赫数标度率与各向同性湍流类似,但胀压分量所占比重更大,并且变形速度张量特征值的概率密度函数和流动拓扑结构的比例分布等统计量随马赫数的变化也更加明显。对于振动非平衡可压缩各向同性湍流,平动-转动内能模式和振动内能模式间的弛豫效应导致密度梯度与振动温度梯度方向的偏离,从而弱化了流场中压缩和膨胀运动对振动弛豫率的影响。化学反应放热会显著增加流场的压缩与膨胀运动,导致速度胀压分量和热力学量的能谱在所有尺度均增大,湍动能和耗散率的标度律表现出马赫数无关性。     

利用林胶茶人工群落减弱台风对橡胶林破坏机理的风洞模拟试验研究

本文研究台风登陆时（中性大层结）胶茶人工群落内部及上部风速的变化，湍流结构的变化及阻力的变化，来分析判断基减弱台风破坏的机理，评定最佳防风效果的林胶茶人工群落方案。试验研究证明台风吹向胶茶人工群落，台风越过和穿过林带，由于气流与树冠，枝叶的冲击与摩作用，使台风风速大大降低，使动能大大损失，使原来动能强和湍流弱的较大尺度旋涡的台风，变成旋涡尺度较小的动能弱湍流强的湍流，湍流能量的增强反映了风速递减率     

温度边界层对壁湍流多尺度相干结构的影响

用热线风速仪以高于对应最小湍流时间尺度的分辨率精细测量了风洞中壁面加热平板湍流边界层不同法向位置流向速度分量的时间序列信号, 与常温情况相比, 热对流加速了壁湍流中流体的动量、质量和能量的交换, 加快了湍流边界层的发展;用子波分析方法研究了壁面加热对壁湍流多尺度相干结构喷射和扫掠条件相位平均波形的影响, 显示热对流明显增大了缓冲层相干结构扫掠过程和喷射过程的强度, 是增强壁湍流中流体的动量、质量和能量交换的根本原因.      

湍流边界层大尺度相干运动的阵列TRPIV测量

使用高时间分辨粒子图像测速技术，研究湍流边界层中大尺度相干运动。由于大尺度运动的流向空间尺度与边界层厚度δ有关，因此沿流向排列4个高速相机进行拍摄，得到了约6.7δ×1.2δ的湍流边界层大视场，实验雷诺数Re_τ=422。针对流场中不同法向高度的流向脉动速度，采用沿流向方向进行空间小波变换的方法，得到不同空间尺度分量的脉动速度，并计算其占总流向脉动动能的比例，发现湍流边界层外区存在流向最大能量流向尺度，约为1δ。通过小波分解将湍流脉动速度场分为大尺度分量和小尺度分量。使用速度门限法，沿时间序列提取大尺度相干运动，利用泰勒冻结假设，将时间结构转化为空间结构，并与直接从空间得到的大尺度相干结构做对比。使用相位平均法测得大尺度相干结构的几何形态，发现从时间维度和直接从空间维度得到的喷射事件的流向尺度相近，而直接从空间提取的扫掠事件要比从时间提取的大。结果表明：流场中1δ尺度左右的大尺度运动是湍动能的主要贡献者；利用泰勒冻结假设可以从时间中提取出大尺度相干结构，与从流场空间直接提取的结果有着良好的一致性。     

基于湍动能谱的自适应大涡模拟方法

为了在计算量有限的前提下实现对不同尺度上湍流燃烧结构的直接求解,提出了新的基于湍动能谱的自适应大涡模拟的概念。在这一概念下,利用湍动能谱和自适应网格技术建立了跨尺度算法,从而实现DNS和LES两种方法的耦合。在湍流非预混氢气射流火焰的模拟中,该方法既能捕捉大尺度湍流结构,又能分辨小尺度燃烧结构,计算出的物理量的瞬态和时均分布和DNS结果吻合得较好。计算偏差主要体现在DNS和LES区域的过渡处,这与亚格子湍动能在过渡处的变化不够平滑有关,表明跨尺度算法需要优化,以完善对不同尺度间湍动能传输的模拟。      

湍流边界层相干结构空间拓扑形态的 层析TRPIV测量

用层析TRPIV(time-resolved paticle image velocimetry)技术精细测量了水洞中平板湍流边界层三分量速度的时空序列信号,提出了空间局部平均多尺度速度结构函数的新概念描述湍流多尺度涡结构的空间拉伸、压缩、剪切变形和旋转.用空间局部平均多尺度速度结构函数对湍流脉动速度进行了空间多尺度分解.用空间局部平均多尺度速度结构函数的新概念,根据湍流多尺度涡结构在空间流向的拉伸和压缩特征,提出了新的湍流相干结构条件采样方法,检测并提取了层析TRPIV数据中相干结构的“喷射”和“扫掠”事件中的速度、涡量等物理量的空间拓扑形态.发现在喷射和扫掠事件中均存在一对反向旋转的准流向“马蹄形”涡结构.      

沟槽壁湍流多尺度相干结构实验研究

应用热线测速技术,对沟槽壁面平板湍流边界层的减阻机理进行了实验研究.测量了风洞中并排放置的沟槽壁面平板及光滑壁面平板湍流边界层在不同雷诺数下不同法向位置的瞬时流向、法向速度分量的时间序列信号.运用流向速度分量信号的多尺度子波系数辨识壁湍流多尺度相干结构,用条件采样和相位平均技术提取了壁湍流多尺度相干结构喷射和扫掠时流向速度分量、法向速度分量和雷诺应力分量的相位平均波形.分析了沟槽壁面平板及光滑壁面平板湍流边界层中多尺度相干结构的持续时间、条件相位平均波形等特征.对沟槽壁面平板及光滑壁面平板湍流边界层多尺度相干结构的多种统计平均特征进行了比较,从壁湍流多尺度相干结构控制的角度研究了沟槽壁面平板湍流边界层的减阻机理.      

湍流涡黏性模型方程中相位差的测量

基于理论上湍流相干结构复涡黏性模型对涡黏性系数的分析,应用热线测速技术测量了平板湍流边界层多尺度相干结构动力学方程中非相干结构成分对相干结构贡献的雷诺应力分量与相干结构流向速度流向变形率之间的相位差。分析了湍流边界层相干结构猝发过程中,非相干结构成分对相干结构贡献的雷诺应力分量与相干结构流向速度流向变形率之间的相位差沿湍流边界层法向的变化规律,为建立更加符合实际的湍流模型提供了实验依据。     

双压电振子异步振动主动调制湍流边界层流向涡减阻

以热线敏感丝为感受器、单片机(MCU)为控制器、双压电振子为动作器构成闭环控制回路,实现闭环主动控制湍流边界层相干结构减阻。采用安装在壁面上的展向布置的双压电振子异步振动方式,通过对压电振子输入3种不同振动频率,得到160 Hz工况实现最大减阻率为16.03%。压电振子振动使得湍动能更大程度地集中在能量峰值周围,改变了湍流边界层近壁区的含能结构,对相干结构产生调制作用。压电振子振动频率与相干结构特征频率越接近,减阻效果越好。闭环控制中控制压电振子所需要的电能节省开环的75%,实现与开环控制相近的减阻效果。施加控制加入条件检测的条件相位平均波形时间周期略变短,以压电振子壁面扰动方式调制近壁流向涡,减小壁面摩擦阻力,获得减阻效果。      

Solar Wind Turbulence and the Role of Ion Instabilities

Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are: (i) weakness of collisional dissipation and (ii) presence of several characteristic space and time scales. In this paper we discuss observational properties of solar wind turbulence in a large range from the MHD to the electron scales. At MHD scales, within the inertial range, turbulence cascade of magnetic fluctuations develops mostly in the plane perpendicular to the mean field, with the Kolmogorov scaling $k_{\perp}^{-5/3}$ for the perpendicular cascade and $k_{\|}^{-2}$ for the parallel one. Solar wind turbulence is compressible in nature: density fluctuations at MHD scales have the Kolmogorov spectrum. Velocity fluctuations do not follow magnetic field ones: their spectrum is a power-law with a ?3/2 spectral index. Probability distribution functions of different plasma parameters are not Gaussian, indicating presence of intermittency. At the moment there is no global model taking into account all these observed properties of the inertial range. At ion scales, turbulent spectra have a break, compressibility increases and the density fluctuation spectrum has a local flattening. Around ion scales, magnetic spectra are variable and ion instabilities occur as a function of the local plasma parameters. Between ion and electron scales, a small scale turbulent cascade seems to be established. It is characterized by a well defined power-law spectrum in magnetic and density fluctuations with a spectral index close to ?2.8. Approaching electron scales, the fluctuations are no more self-similar: an exponential cut-off is usually observed (for time intervals without quasi-parallel whistlers) indicating an onset of dissipation. The small scale inertial range between ion and electron scales and the electron dissipation range can be together described by $\sim k_{\perp}^{-\alpha}\exp(-k_{\perp}\ell_{d})$ , with α?8/3 and the dissipation scale ? _d close to the electron Larmor radius ? _d ?ρ _e . The nature of this small scale cascade and a possible dissipation mechanism are still under debate.     

Notes on Magnetohydrodynamics of Magnetic Reconnection in Turbulent Media

Astrophysical fluids have very large Reynolds numbers and therefore turbulence is their natural state. Magnetic reconnection is an important process in many astrophysical plasmas, which allows restructuring of magnetic fields and conversion of stored magnetic energy into heat and kinetic energy. Turbulence is known to dramatically change different transport processes and therefore it is not unexpected that turbulence can alter the dynamics of magnetic field lines within the reconnection process. We shall review the interaction between turbulence and reconnection at different scales, showing how a state of turbulent reconnection is natural in astrophysical plasmas, with implications for a range of phenomena across astrophysics. We consider the process of magnetic reconnection that is fast in magnetohydrodynamic (MHD) limit and discuss how turbulence—both externally driven and generated in the reconnecting system—can make reconnection independent on the microphysical properties of plasmas. We will also show how relaxation theory can be used to calculate the energy dissipated in turbulent reconnecting fields. As well as heating the plasma, the energy dissipated by turbulent reconnection may cause acceleration of non-thermal particles, which is briefly discussed here.     

采用DMD方法研究叶栅不同攻角的拟序结构

为分析平面叶栅分离流非定常拟序流动特征,对三个不同攻角下的叶栅进行了单通道的大涡模拟仿真,并采用动力模态分解（DMD）三个工况的流场结构进行了分析。DMD方法对包含复杂时空信息的叶栅分离流流场进行了解耦,剥离出了反映流场主要动力信息的模态,获得了其频率和与之对应的空间结构。并且通过DMD方法,将原本需要研究大量不同时刻的流场,转移到仅需要对少量模态的研究即可,实现了保留主要动力特征的低维近似。通过DMD分析表明:气流经过叶片前缘产生流动分离,形成不稳定的剪切涡结构,它和尾迹区脱落涡相互耦合,并形成新的拟序结构。随着攻角的增大,前缘剪切涡及其与尾迹涡的耦合也同时增强,流场变得更加复杂。      

Characteristics of reattached boundary layer in shock wave and turbulent boundary layer interaction

The reattached boundary layer in the interaction of an oblique shock wave with a flatplate turbulent boundary layer at Mach number 2.25 is studied by means of Direct Numerical Simulation(DNS). The numerical results are carefully compared with available experimental and DNS data in terms of turbulence statistics, wall pressure and skin friction. The coherent vortex structures are significantly enhanced due to the shock interaction, and the reattached boundary layer is characterized by large-scale...     

使用GAO-YONG方程组对湍流边界层拟序结构特性的研究

与以往的湍流模型不同,GAO-YONG不可压湍流控制方程组不需要任何经验系数及壁面函数。其级数形式的能量方程与非线性现象多尺度层次相对应,具备了描述湍流统计平均和拟序结构的双重功能。本文采用交错网格和SIMPLE方法求解GAO-YONG不可压湍流方程组,考察了GAO-YONG方程组中能量方程阶数以及计算网格对拟序结构的影响,证明了该方程在描述拟序结构方面具有一定的适定性。      

Fluctuations, Dissipation and Heating in the Corona

Mechanisms for the deposition of heat in the lower coronal plasma are discussed, emphasizing recent attempts to reconcile the fluid and kinetic perspectives. Structures at the MHD scales are believed to act as reservoirs for fluctuation energy, which in turn drive a nonlinear cascade process. Kinetic processes act at smaller spatial scales and more rapid time scales. Cascade-driven processes are contrasted with direct cyclotron absorption, and this distinction is echoed in the contrast between frequency and wavenumber spectra of the fluctuations. Observational constraints are also discussed, along with estimates of the relative efficiency of cascade and cyclotron processes. This revised version was published online in June 2006 with corrections to the Cover Date.     

Low frequency turbulence and energy dissipation in the Solar Wind

The possibility to perform in-situ measurements of velocity, magnetic field, density and temperature fluctuations in the Solar Wind has greatly improved our knoweledge of MHD turbulence not only from the point of view of space physics but also from the more general point of view of plasma physics.These fluctuations on the one hand extend over a wide range of frequencies (about 5 decades), a fact which seems to be the signature of turbulent non-linear energy cascade, on the other hand display, mainly in the trailing edge of high speed streams, a number of striking features: (i) a high degree of correlation between magnetic and velocity field fluctuations, (ii) a very low level of fluctuations in mass density and magnetic field intensity, (iii) a considerable anisotropy revealed by minimum variance analysis of the magnetic field correlation tensor. More recently it has been stressed that MHD turbulence in the Solar Wind displays a clear intermittent character.The picture which emerges from the most recent analytical theories and numerical simulations is presented. In particular the observations which give us informations about the dissipation mechanism, which remains yet largely unknown, are discussed.     

Investigation of flow unsteadiness in a highly-loaded compressor cascade using a dynamic mode decomposition method

Unsteady flow in the hub endwall region has long been a hot topic in the turbomachinery community. However important it is to the performance of the whole engine, the coherent unsteady flow phenomena are still not well understood. In this paper, the complex flow field in the hub endwall of a cantilevered compressor cascade has been investigated through numerical approach. The predicted results were validated by experimental data. To highlight the dominant flow structures among irregular and chao...