Uniform solution for the flow past a slender body with an attached shock wave in radiative magnetogasdynamics

A systematic perturbation scheme is used to study the propagation of a weak shock wave attached to a slender body in a supersonic flow of plasma with thermal radiation and investigate as to how the coupling between the radiative transfer and magneto-hydrodynamic phenomena affects the flow field. The analytical solution of the flow field has been presented up to the second order of ε. The shape of the shock wave attached to the slender body of revolution is obtained, which however can be expressed explicitly in terms of known functions when the radiative decay length is of the same order as the typical body length. Also, the shock angle at the tip of the projectile is obtained.     

Growth and decay of weak discontinuities in radiative gasdynamics

Growth and decay properties of weak discontinuities headed by wave fronts of arbitrary shape in three dimensions are investigated in a thermally radiating inviscid gas flow. The effects of radiative transfer are treated by the use of a general differential approximation for a grey gas of arbitrary opacity including effects of radiative flux, pressure and energy density. The transport equations representing the rate of change of discontinuities in the normal derivatives of the flow variables are obtained, and it is found that the nonlinearity in the governing equations does not contribute anything to the radiation induced waves. In contrast to the radiation induced waves, the nonlinearity in the governing equations plays an important role in the interplay of damping and steepening tendencies of a modified gasdynamic wave. An explicit criterion for the growth and decay of a modified gasdynamic wave along bicharacteristics curve in the characteristic manifold of the governing differential equations is given and the special reference is made of diverging and converging waves. It is shown that there is a special case of a compressive converging wave for which the stabilizing influences of thermal radiation and the wave front curvature are not strong enough to overcome the tendency of the wave to grow into a shock.     

减压阀节流口流场仿真和分析

采用Fluent软件对火箭姿态控制系统减压阀环形节流口流场进行了数值仿真,得到了流场有关参数图形。减压阀节流口气体流场为非自由、紊动、冲击、壁面射流,气体在节流口达到音速,贴壁面高速射流出去后,相互撞击、压缩并撞击阀芯柱面产生激波,气流总压损失较大,建议采用等温过程进行特性计算。减压阀环形节流口后流场存在激波,总压并不守恒,目前通用的气流稳态流动力计算公式并不合适,应借助流场分析工具进行节流元件受力分析。     

火星进入气体辐射加热研究进展

针对飞行器进入火星大气时气体辐射加热对防热设计带来不确定性，在简述火星探测和气体辐射研究的发展历程的基础上，对火星进入气体辐射加热研究的进展进行综述。首先，针对火星大气环境描述了气体辐射加热的概念和问题由来。其次，重点综述了近年来火星进入气体辐射加热基础模型的数值和试验研究进展，其中包括：热化学非平衡气体动力学、气体辐射特性和辐射传输的计算模型与方法等数值研究；地面测试设备、试验技术和模拟火星大气环境的气体辐射测量与验证等试验研究。再次，综述了流动辐射耦合和后体气体辐射加热等火星进入器设计方面开展的研究。最后，对未来火星进入气体辐射加热研究进行了展望，提出了研究建议。     

高超声速混合流动的粒子模拟耦合算法

通过采用基于三维非结构网格的子网格技术,对适用于高超声速混合流动的自适应时间步长粒子模拟耦合算法(Improved Hybrid Particle Simulation Method,IHPSM)进行了改进,在保证算法计算效率的同时降低数值误差。通过对三维双曲钝锥外形的数值仿真及与DSMC(Direct Simulation Monte Carlo)计算结果的对比分析,证明改进的IHPSM算法具有较高的计算精度,且能较大幅度提高计算效率。基于改进的IHPSM算法,文中针对双曲钝锥外形进行了稀薄气体效应和飞行马赫数对高超声速流动影响规律的研究。结果表明,气体稀薄程度的增加会减缓双曲钝锥前端流场宏观物理量的变化梯度,使流场激波结构变厚;来流马赫数的增大会使激波明显增强,但对激波厚度与结构的影响较小。     

单喷管火箭自由喷流噪声数值模拟

利用非定常燃气流场数值模拟方法，研究超声速喷流核心区及其外围亚声速区燃气流动态分布和流动特性，在此基础上利用欧拉方程条件的伽辽金有限元方法以及FWH方法，实现并完成喷流噪声传播特性、辐射特性数值模拟。喷流噪声数值模拟结果显示：燃气流推进初期，强喷流噪声区域紧随燃气流前锋；燃气流场相对稳定后，强喷流噪声区域主要位于燃气流等能区末稍，一些小尺度试验的燃气流激波系附近也存在较强喷流噪声。这些强喷流噪声主要由燃气流前锋带动的大涡动态卷吸、燃气流强湍流脉动以及激波扰动引起。受数值模拟网格分辨率影响，当前仅能保持中低频段声压级数值模拟结果与实测结果总体接近。     

气体辐射与流场耦合对火星进入热环境影响

采用火星大气物理化学模型,求解带辐射源项的三维热化学非平衡N-S方程,对探路者号火星探测器进入过程中的高温流场和热环境进行了数值模拟,分析了气体辐射与非平衡流场耦合效应对流场和热流的影响。结果表明:1)探路者号火星探测器流场热化学非平衡效应显著,CO₂气体发生大规模离解,高度低至28.5 km仍存在热力学非平衡效应;2)热力学与化学非平衡效应的影响均与表面催化特性相关,完全催化热流要高于完全非催化热流50%以上;3)高温流场中的CO组分会产生较强的气体辐射加热,辐射热流与对流热流的比值为15%～45%,靠近肩部区域比值最大;4)气体辐射对非平衡流场的冷却效应使激波脱体距离减小;与非耦合方法相比,采用耦合方法得到的辐射热流降低约12%～25%。     

高超声速化学平衡流辐射流场数值解

本文用数值方法研究了高超声速大钝头体绕流辐射流场。采用粘性激波层控制方程和平衡化学反应气体模型。辐射部份包括连续辐射和线辐射。采用切平板辐射输运模型解决了空间推进的问题，计算结果表明：辐射传热与飞行器再入飞行速度，高度及头部半径密切相关，在计算的条件下，当再入速度小于７．６公里／秒时，辐射传热的影响可以忽略，当再入速度为１１公里／秒左右时，辐射传热可以与对流传热相比拟。当再入速度更大时，辐射传热远     

Shock waves in water foams

Propagation of shock waves in tubes filled with water foams is studied using pressure gauges. Low amplitude shock waves consist of a precursor which propagates at a velocity slightly less than the acoustic velocity in the gas, and of a main compression wave which propagates slower than the precursor. Stronger shock waves have a single front. Maximum pressure rise in the incident and reflected shock waves cannot be calculated using one-dimensional conservation equations at the shock front. It is suggested that the flow of the liquid in foam cells has to be taken into account in order to predict the behavior of shock waves in foams. The nature of the gas which fills the cells is shown to have a strong effect on the quenching of blast waves in foams.     

某固体火箭发动机点火启动过程三维流场一体化仿真

以某固体发动机的燃烧室和喷管为一体化研究对象,采用三维流场控制方程,应用有限体积法计算了发动机点火启动过程中燃烧室和喷管内燃气的流场特性。发动机药柱上的着火点最初出现在药柱星角尖上,然后向四周扩展;在药柱点火初期,燃气压力波先于火焰峰到达喷管;随着燃烧室内燃气压力升高,压力沿轴向分布逐渐平缓;当喷管进口压力与出口背压比达到某一值时,喷管扩张段内出现一道激波,随着压力比的升高,激波最终移出喷管,燃气流速在喷管出口处达到最大值。     

化学非平衡效应对返回舱再入气动力特性的影响

高空高马赫数条件下,化学非平衡效应将对飞行器气动特性产生影响,影响飞行器气动布局优化和飞行弹道设计。文章通过三维化学非平衡流动求解程序,针对再入返回器开展数值研究与机理分析,通过对比完全气体模型和化学非平衡气体模型获得的气动力参数,揭示化学非平衡效应对流场结构和气动力特性的影响和规律。结果表明,对Apollo的气动力计算结果验证了模型和计算方法;化学非平衡效应影响下,激波层内化学反应消耗大量能量,致使激波脱体距离减小,气体压缩性增强;典型状态高度为70 km,Ma=30条件下,化学非平衡效应导致返回器升力系数增大约6%、阻力系数增大约1.3%～3.3%、升阻比增大3%左右、俯仰力矩系数增大,从而使配平攻角减小约2.5＆#176;;通过机理分析,发现化学非平衡效应影响下表面压力系数发生变化的原因是飞行器周围激波形状及驻点压力改变,表现为气体沿流线经激波层、压缩区和膨胀区的历程变化;对于钝体形状的返回器,迎风面前体压力系数增加和后体压力系数降低,造成轴向力和法向力系数增大。     

On flows with vibrational relaxation behind an attached shock wave

The flow conditions are represented by an oblique shock attached to the vertex of a straight edged wedge, placed symmetrically with respect to a uniform supersonic flow in front, so that the flow after the shcok is along the wedge surface. The curvature of the attached shock wave, and the flow variable gradients at the wedge tip caused by non-equilibrium vibrational effects are determined for a steady two-dimensional flow of a vibrationally relaxing gas. A relation between the curvature of the shock and that of the stream line is obtained at the wedge-tip. The variation of entropy and an expression for the vorticity generated by the shock towards down-stream flow are determined. Calculations have been carried out for the shock curvature and flow variable gradients for a wide range of wedge angle and the up-stream flow Mach number.     

磁窗的一种理论模型

本文简要地回顾了“磁窗”减轻再入通讯中断的机理。推导出线极化波,园极化波穿透磁等离子体薄层时,场量的传输矩阵。给出了功率反射系数及透射系数表达式。通过这种磁窗理论模型,模拟算出了为减轻或消除再入通讯中断所需要的磁场强度。并通过激波管上进行的磁窗模拟试验,证实了这一结论。     

“人字形小肋”对激波/边界层干扰的影响研究

在曼彻斯特大学跨声速风洞开展激波/边界层干扰及“人字形小肋”对其影响的实验研究。在马赫数1.85流场条件下,应用高速纹影、油流、皮托压力测量和基于压敏漆的壁面压力测量技术,研究“人字形小肋”流动控制方法对激波/边界层干扰的流动分离结构与尺寸、压力分布特性与波系特征等影响。结果显示激波/边界层干扰诱发流动分离,分离区呈现三维特征,在“人字形小肋”的作用下,分离线呈现“波浪”形且整体向上游移动,干扰区流向尺寸增大,分离区高度减小且长度略增大,再附区的压力极值降低,这些特征与叶片、尖楔等微涡发生器的影响趋势相反。下一步工作中,拟针对“人字形小肋”开展参数优化研究,“人字形小肋”可能成为降低激波/边界层干扰诱发的高热流载荷的有效方法。     

Fine structure of interplanetary shock fronts from the data of the BMSW instrument of the PLASMA-F experiment

The paper is concerned with studying the thickness of fronts of 38 interplanetary shocks detected by the BMSW instrument, which is a part of the scientific payload of the SPEKTR-R spacecraft, which was launched into a highly elliptical orbit in 2011. The main parameters of the interplanetary shocks have been calculated as follows: the ratio of thermal pressure to magnetic pressure before the front β, the angle between the shock front normal and the undisturbed magnetic field θ_Bn, the ratio of the shock propagation velocity to the magnetosonic velocity in the undisturbed region M_ms, and the shock front velocity relative to the Earth. It has been shown that the front thickness determined from the plasma parameters approximately matches the front thickness obtained from the magnetic field measurements and lies between 0.5 and 5 proton inertial lengths. In some events, the oscillations have been observed (upstream and downstream of the shock) in plasma parameters and in the magnetic field data. The length has been found to be between 0.5 and 6 proton inertial lengths for the preceding oscillations and between 0.5 and 10 proton inertial lengths for the following oscillations. The average value of the proton inertial length is 62 km.     

超音速流在正规反射激波系后的参数优化特性

研究了超音速气流中正规反射波加一正激波结构下的参数优化特性，给出了求解这种优化结构的方法，通过计算得到了优化条件存在的区域和优化解的特性，它用可于指导超音速飞行器的进气道及相关装置的设计。     

激波在狭缝中绕射过程研究

针对固体火箭发动机药柱存在裂纹的情况，对运动激波在狭缝中绕射传播的非定常流场进行了计算，得到了清晰的流场变化图谱，从流场图中可分辨出激波在狭缝中的传播过程。对不同深宽比的狭缝进行研究，发现流场结构存在明显差别，在深宽比较小时狭缝内压力波振荡较小，当深宽比超过一定值时狭缝内的压力波产生剧烈振荡。研究结果表明，该方法可很好地描述激波在狭缝中的传播过程。     

高超声速条件下星光传输模拟方法与仿真

以高超声速飞行器为研究对象,建立了高速流场下的星光传输模拟仿真方法,定性、定量地研究平台气动光学效应对星光导航的影响。采用基于k-ω/SST两方程湍流模型的雷诺平均法计算星敏感器安装在飞行器不同位置处（头部、中部和尾部）的外流场密度分布,进而得到流场的空间折射率分布。在此基础上,利用几何光学法计算星光由高速层流流场引起的光程差、点扩散函数、像偏移等光学传输效应,得出经过层流流场的星光降晰图。同时运用统计光学理论计算高速湍流流场引起的星光出瞳面的波像差、密度均方差、相位均方差、Strehl比等光学传输效应,得出经过湍流流场的星光降晰图。仿真结果与理论分析吻合,从而为研究星光在高超声速流场中传输的机理提供了可靠的技术手段。     

Calculation of the Initial Magnetic Field for Mercury’s Magnetosphere Hybrid Model

Several types of numerical models are used to analyze the interactions of the solar wind flow with Mercury’s magnetosphere, including kinetic models that determine magnetic and electric fields based on the spatial distribution of charges and currents, magnetohydrodynamic models that describe plasma as a conductive liquid, and hybrid models that describe ions kinetically in collisionless mode and represent electrons as a massless neutralizing liquid. The structure of resulting solutions is determined not only by the chosen set of equations that govern the behavior of plasma, but also by the initial and boundary conditions; i.e., their effects are not limited to the amount of computational work required to achieve a quasi-stationary solution. In this work, we have proposed using the magnetic field computed by the paraboloid model of Mercury’s magnetosphere as the initial condition for subsequent hybrid modeling. The results of the model have been compared to measurements performed by the Messenger spacecraft during a single crossing of the magnetosheath and the magnetosphere. The selected orbit lies in the terminator plane, which allows us to observe two crossings of the bow shock and the magnetopause. In our calculations, we have defined the initial parameters of the global magnetospheric current systems in a way that allows us to minimize paraboloid magnetic field deviation along the trajectory of the Messenger from the experimental data. We have shown that the optimal initial field parameters include setting the penetration of a partial interplanetary magnetic field into the magnetosphere with a penetration coefficient of 0.2.     

Dust Plasma Dynamics in the Geomagnetic Tail

The results of numerical modeling of dust plasma dynamics in the geomagnetic tail are presented for the southward and northward orientations of the interplanetary magnetic field in the model with reconnection of magnetic field lines of geomagnetic and interplanetary magnetic fields. It is shown that in reconnection regions the compression shock waves arise, at the fronts of which the dust plasma fluxes with higher-than-background density are generated.