数值分析加力燃烧室的燃烧效率和燃烧流场

本文对装有钝体火焰稳定器的加力燃烧室燃烧效率特性进行了数值分析和实验研究。计算中用k-s双方程模型描述紊流特性,用Magnussen的涡团耗散模型以及燃烧模型估算化学反应速率。为了考虑火焰辐射对燃烧效率的影响,采用热通量法辐射模型估算辐射通量。由于燃烧流场密度变化较大,故在守恒方程中采用密度加权平均来处理。试验中用热电偶测量温度,对燃烧效率和壁面温度作了研究。最后,将计算结果与试验数据作了比较,结果表明本文的计算方法和计算程序是合理可行的。     

Magnetic energy release near accreting black holes

The observed non-thermal emission from accreting compact objects is often understood in terms of the expected magnetic activity of accretion disks. This review discusses the constraints on this view point that can be obtained from, principally, the X-ray spectra and the X-ray variability of black hole candidates.Furthermore, the traditional view of an accretion disk corona, put forward as the source of the non-thermal emission, analogous to the solar corona is shown to be wrong on a few important points. Firstly, the density in the equilibrium accretion disk corona is extremely low. A reasonable plasma density is retained by pair production processes similar to those existing in the pulsar magnetosphere. Secondly, the dominant resistivity in the accretion the disk on the current carrying electrons.     

超音速混合气流场的有限元分析与探讨

系统阐述了超音速混合气流场的特性及求解过程。针对复杂流场求解过程中有限元模型的建立、边界条件的确定以及求解过程的具体实现等进行了深入的理论分析和探讨。本文最后给出了一个运用FLUENT软件求解超音速气流场的实例。     

波瓣形排气引射混合器的试验研究

在常压、低速排气引射条件下, 以常规环形排气引射混合器为基准, 试验研究了波瓣出口角度 α/β、相对混合长度 L/D和波瓣穿透率 H/H_o 等结构参数对波瓣形排气引射混合器气动性能的影响。试验表明, 波瓣形排气引射混合器的气动性能明显优于环形排气引射混合器; 在不引起波瓣内气流分离的情况下, α/β对气动性能影响不大; 加大 L/D可以改善气动性能, 存在气动—重量综合性能最好的最佳L/D;较大的H/H_o 有利于两股气流的混合, 但引射能力下降      

Topological and statistical properties of nonlinear force-free fields

We use our semi-analytic solution of the nonlinear force-free field equation to construct three-dimensional magnetic fields that are applicable to the solar corona and study their statistical properties for estimating the degree of braiding exhibited by these fields. We present a new formula for calculating the winding number and compare it with the formula for the crossing number. The comparison is shown for a toy model of two helices and for realistic cases of nonlinear force-free fields; conceptually the formulae are nearly the same but the resulting distributions calculated for a given topology can be different. We also calculate linkages, which are useful topological quantities that are independent measures of the contribution of magnetic braiding to the total free energy and relative helicity of the field. Finally, we derive new analytical bounds for the free energy and relative helicity for the field configurations in terms of the linking number. These bounds will be of utility in estimating the braided energy available for nano-flares or for eruptions.     

Three-dimensional magnetic reconnection regimes: A review

The magnetic field in many astrophysical plasmas – such as the solar corona and Earth’s magnetosphere – has been shown to have a highly complex, three-dimensional structure. Recent advances in theory and computational simulations have shown that reconnection in these fields also has a three-dimensional nature, in contrast to the widely used two-dimensional (or 2.5-dimensional) models. Here we discuss the underlying theory of three-dimensional magnetic reconnection. We also review a selection of new models that illustrate the current state of the art, as well as highlighting the complexity of energy release processes mediated by reconnection in complicated three-dimensional magnetic fields.     

Radiation from relativistic shocks in turbulent magnetic fields

Using our new 3-D relativistic particle-in-cell (PIC) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron–positron jet propagating in an unmagnetized ambient electron–positron plasma. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value as predicted by hydrodynamic shock compression. In the jet (reverse) shock behind the bow (forward) shock the strongest electromagnetic fields are generated. These fields may lead to time dependent afterglow emission. In order to calculate radiation from first principles that goes beyond the standard synchrotron model used in astrophysical objects we have used PIC simulations. Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We then used the technique to calculate emission from electrons in a small simulation system. From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability. A fully developed shock within a larger simulation system may generate a jitter/synchrotron spectrum.     

共轴式双旋翼尾迹流场的水洞PIV测量

采用粒子图像测速(PIV)技术,对共轴式双旋翼在悬停和以不同前进比前飞时的流场进行水洞实验.将激光片光定位于旋翼的纵向截面,桨叶的方位角和图像的获取是同步的.测量得到了旋翼流场的瞬时涡量和速度分布、桨尖涡的结构和脱落轨迹、悬停时的尾迹边界收缩和前飞时的尾迹边界倾斜角等.研究了不同状态下共轴式双旋翼流场的气动干扰特性.为了比较,对单旋翼也进行了同样的测量.实验得到了有价值的结果,对共轴式直升机的气动计算和合理设计具有重要意义.      

Effect of Interplanetary Transients on Cosmic Ray Anisotropic Variations

In the present work the cosmic ray intensity data recorded with ground-based neutron monitor at Deep River has investigated taking into account the associated interplanetary magnetic field and solar wind plasma data during 1981—1994.A large number of days having abnormally high/low amplitudes for successive number of five or more days as compared to annual average amplitude of diurnal anisotropy have been taken as high/low amplitude anisotropic wave train events(HAE/LAE).The amplitude of the diurnal anisotropy of these events is found to increase on the days of magnetic cloud as compared to the days prior to the event and it found to decrease during the later period of the event as the cloud passes the Earth.The High-Speed Solar Wind Streams(HSSWS)do not play any significant role in causing these types of events. The interplanetary disturbances(magnetic clouds)are also effective in producing cosmic ray decreases.Hαsolar flares have a good positive correlation with both amplitude and direction of the anisotropy for HAEs, whereas PMSs have a good positive correlation with both amplitude and direction of the anisotropy for LAEs. The source responsible for these unusual anisotropic wave trains in CR has been proposed.     

角区三维漩涡流动的新分离结构

分别用数值计算和PIV(Particle Image Velocimetry)实验方法研究角区层流边界层三维定常分离的流动结构,证实了角区确实存在有别于传统分离现象的附着鞍点结构,对称面上游的流线并非从壁面向上抬起从壁面分离,而是经由空间某个奇点向壁面附着.角区马蹄涡的传统分离鞍点结构和附着鞍点结构之间存在着一定的演化规律,影响参数包括模型头部钝度、边界层厚度和雷诺数.一定的边界层和雷诺数条件下随着模型头部钝度减小,角区马蹄涡将从传统的分离鞍点结构逐步过渡为附着鞍点结构;对一定的模型若雷诺数越大、边界层越厚则角区流动越趋向于传统的分离鞍点结构,反之则倾向于附着鞍点结构.