Influence of fuel injection position and equivalent mixture ratio on chemical non-equilibrium effects of single expansion ramp nozzle

Chemical non-equilibrium flow was investigated for the scramjet single expansion ramp nozzle(SERN) with a strut-based liquid-kerosene-fueled combustor.Two-dimensional Reynolds-averaged Navier-Stokes(RANS) equations were solved with the species conservation equation for continuous phase and the renormalization group(RNG) k-ε turbulence model.Lagrangian discrete-phase model was analyzed for liquid-kerosene droplets behavior in the supersonic stream.Combustion was simulated by kerosene surrogate fuel's 10-species and 13-step reduced reaction kinetics mechanism with use of Arrhenius's laminar finite rate model.Parametric studies were carried out to estimate the influence of different fuel injection positions and equivalent mixture ratios on the SERN chemical non-equilibrium effects.Numerical calculation results show that the strut-based combustor enables convenient modeling of various SERN entry conditions,which is similar with many preceding investigations,by changing the injector strut position and controlling the mass flow rate of each injector.Chemical non-equilibrium effects function in the whole SERN,especially in the initial flow expansion region,leads to obviously higher SERN performance of the non-equilibrium flow than that of the frozen flow.Furthermore,the distributed fuel injection pattern plays a significant role in enhancing the combustion efficiency in combustor,but weakening the chemical non-equilibrium effects funciton in SERN.Additionally,while the equivalent mixture ratio increases,the SERN thrust coefficient and lift coefficient rise gradually,and the increment of non-equilibrium flow in relation to frozen flow becomes higher as well.To be specific,the equivalent mixture ratio is 0.6,the maximum increment of thrust coefficient and lift coefficient are 11.6% and 25% respectively.      

星载全球大气波动成像仪研究

在卫星上对中间层顶区域的气辉辐射成像观测, 对于全球大气波动的监测和研究具有重要的意义. 利用TDICCD对O₂A (0-0)气辉进行成像观测, 计算了曝光积分时间、信噪比和能达到的最高空间分辨率, 分析了地球自转对空间分辨率的影响, 在此基础上提出一种星载全球大气波动成像仪方案, 该方案可以观测垂直波长大于10km的大气波动, 最高水平分辨率可以达到0.33km.      

Assessment of Two Turbulence Models and Some Compressibility Corrections for Hypersonic Compression Comers by High-order Difference Schemes

The Spalart-Allmaras (S-A) turbulence model,the shear-stress transport (SST) turbulenee model and their compressibility corrections are revaluated for hypersonic compression corner flows by using high-...     

突跃型与平滑型斜爆震波起爆机制数值模拟

采用带有化学反应的Euler方程,对突跃型与平滑型2种形态的斜爆震波(ODW)在起爆机制和结构特点等方面的差异进行了研究.结果表明:斜激波(OSW)后是否存在亚声速区是判定斜爆震形态的依据.当波后火焰抬升斜激波面使得亚声速区存在时,横向激波与三波点结构就会出现并形成突跃型斜爆震.当波后所有区域皆为超声速区时,波后火焰燃烧无法影响到上游激波面,则会形成平滑型斜爆震.通过斜激波关系式给出了横向激波形成所需的临界斜激波角度,只有当斜激波角度大于此临界角度时才能形成突跃型斜爆震波,反之则形成平滑型斜爆震波.      

非对称喷管超声速流场的PIV实验与数值模拟

选取了跟随性能以及散射性能都上佳的二氧化钛粒子,利用了粒子图像测速仪(particle image velocimetry,PIV)对不同落压比下的非对称喷管(single expansion ramp nozzle,SERN)流场进行了测量,成功获取了相应流动结构,以及沿程上壁面压力分布和速度场等.在测得的图像中,可以清晰地观察到由于过膨胀产生的激波与膨胀波系,并进一步获得出口速度分布.运用计算流体动力学数值模拟方法,对实验状态下的非对称喷管进行了模拟.对比结果发现:PIV实验测得流场结构能很好地与其吻合,这互相验证了CFD计算和PIV实验的正确性及可靠性.      

Ion-acoustic waves in unmagnetized collisionless weakly relativistic plasma of warm-ion and isothermal-electron using time-fractional KdV equation

Collisionless unmagnetized plasma consisting of a mixture of warm ion-fluid and isothermal-electron is considered, assuming that the ion flow velocity has a weak relativistic effect. The reductive perturbation method has been employed to derive the Korteweg–de Vries (KdV) equation for small – but finite-amplitude electrostatic ion-acoustic waves in this plasma. The semi-inverse method and Agrawal’s method lead to the Euler–Lagrange equation that leads to the time fractional KdV equation. The variational-iteration method given by He is used to solve the derived time fractional KdV equation. The calculations show that the fractional order may play the same rule of higher order dissipation in KdV equation to modulate the soliton wave amplitude in the plasma system. The results of the present investigation may be applicable to some plasma environments, such as space-plasmas, laser-plasma interaction, plasma sheet boundary layer of the earth’s magnetosphere, solar atmosphere and interplanetary space.     

膨胀循环发动机推力室传热优化

针对膨胀循环发动机推力室身部燃气侧的内壁增强换热结构和冷却剂侧的冷却通道结构这两个影响推力室身部换热最关键的结构分别进行多种结构下的数值模拟对比。通过分析各结构的模拟结果,得到了能够合理提高推力室身部换热能力的内壁加肋结构和圆柱段冷却通道深宽比的结构特征。     

SAR图像伪加性相干斑噪声统计特性

研究了SAR图像加性模型中伪加性相干斑噪声分量的统计特性。分析了SAR图像中真实信号分量和乘性相干斑噪声分量的统计特性;在此基础上结合Edgeworth展开式和以Mellin变换为基础的第二类型特征函数及其对数累积量详细推导了伪加性相干斑噪声概率密度函数的近似表达式;各信号分量的概率密度函数中的参数采用对数累积量方法进行估计。最后利用SAR实测数据仿真分析了伪加性相干斑噪声的统计特性。实验结果表明,乘性的相干斑噪声转换为加性噪声后,其统计特性非常接近于高斯分布。     

中国经济由外需拉动向内需拉动转型的思考

国际金融危机冲击导致外需大幅下滑,我国经济增长受到较大影响,外需拉动型发展模式亟待向内需拉动型发展模式转变.转型虽然势在必行,但转型并非要依靠缩小出口的绝对规模来实现,而主要应通过扩大内需的相对规模来实现.从中长期看,扩大消费是实现转型的主要途径,保持较大投资规模仍是国情所需,提倡乐于消费的观念有助于促进转型的实现,只有全面深化改革才能实现转型.     

Wolf–Rayet optically thick winds with Alfvén waves

The Wolf–Rayet (WR) stars are hot luminous objects which are suffering an extreme mass loss via a continuous stellar wind. The high values of mass loss rates and high terminal velocities of the WR stellar winds constitute a challenge to the theories of radiation driven winds. Several authors incorporated magnetic forces to the line driven mechanism in order to explain these characteristics of the wind. Observations indicate that the WR stellar winds may reach, at the photosphere, velocities of the order of the terminal values, which means that an important part of the wind acceleration occurs at the optically thick region. The aim of this study is to analyze a model in which the wind in a WR star begins to be accelerated in the optically thick part of the wind. We used as initial conditions stellar parameters taken from the literature and solved the energy, mass and momentum equations. We demonstrate that the acceleration only by radiative forces is prevented by the general behavior of the opacities. Combining radiative forces plus a flux of Alfvén waves, we found in the simulations a fast drop in the wind density profile which strongly reduces the extension of the optically thick region and the wind becomes optically thin too close its base. The understanding how the WR wind initiate is still an open issue.