激波对管内壁堆积粉尘作用的实验研究

用水平激波管研究了激波对管内壁堆积粉尘的抛撒效应。试验粉尘为玉米粉（平均直径５μｍ），采用ＹＡ－１６高速摄影机观察了激波特性和粉尘云的发展，结果表明，在激波扫过堆积粉尘与粉尘被扬起存在一定时间滞后，粉尘云的高度也是有限的。     

一种缩短碳氢燃料—空气混合物点火延迟的方法

采用激波风洞－微波管组合设备对顶混的碳氢燃料－空气混合物的点火与超声速燃烧进行了研究。为缩短碳氢燃料－空气混合物的点火延迟时间，通过激波风洞喷管入口与接触面之间的激波反射对经过雾化与气化的碳氢燃料（汽油）进行预热；此外，由燃烧驱动激波管产生的高温燃气作为引导火焰点燃激波风洞产生的预混与预热的超声速碳氢燃料－空气混合物。采用纹影系统对超声速可燃气流中的火焰传播进行流场显示。实验结果表明，上述方法可将碳氢燃料－空气混合物的点火延迟时间缩短至小于0．2ms，同时还得出了火焰相对于超声速可燃气流的传播速度。     

受限空间内激波与火焰作用的三维计算

激波与火焰的相互作用常发生在超声速燃烧和燃烧转爆轰过程中,为深入了解这一现象,采用带化学反应的三维Navier-Stokes方程,对平面入射激波及其反射激波与火焰的作用进行了计算研究,其中燃烧过程使用单步反应模型描述。研究结果显示:在受限空间内模拟激波与火焰作用,能更好地符合实验结果,从而体现出受限空间的三维效应;火焰在入射激波的作用下主要经Richtmyer-Meshkov不稳定而发生变形,此时火焰变形以物理作用为主,燃烧膨胀效果相对不明显;当反射激波与变形火焰再次作用后,火焰迅速膨胀变形,放热率维持在较高水平,此时化学反应过程起主要作用;在反射激波的作用下,变形火焰复杂三维涡结构的形成能强化热量与质量的输送,提高燃烧速率。     

堆积粉尘本构方程的实验测试

确定堆积粉尘的本构方程对讨论有关现象是十分重要的，设计了一种测试方法，利用阴影摄影和带示踪粒子的X光脉冲摄影，记录激波与堆积粉尘相互作用的流场，再通过对该流场的理论分析，以确定堆积粉尘的本构方程，以国淀粉为例，对所测的方程做了实验验证。     

惰性粉尘和抑爆过程的实验研究

在长9m，内径0．14m的燃烧管内进行了CaCO3颗粒其H2－O2混合物中发生爆炸过程的抑制作用的实验研究。该管分为三部分：激波成长段，抑爆段和抑爆后观察段。其中抑爆段装有10套可形成均匀颗粒悬浮流的喷粉系统。实验结果表明，仅当颗粒浓度大于某值时，才可能有效抑制爆炸，否则爆炸波会在抑制后重新成长。笔者还基于两相化学反应流的基本方程，通过分裂方法，全耦合TVD格式和Lax-Wen-droff-Rubin格式对粉尘抑爆现象进行了数值模拟，计划结果反映了惰性颗粒作用下激波的变化过程，其结果与实验结果一致。     

基于成像的RP-3煤油在激波管内自点火过程研究

为深入直观了解RP-3煤油在激波管内的自点火及燃烧过程,利用高分辨率纹影系统和高速摄像机对反射激波后点火燃烧过程进行拍摄,获取了丰富的光学图像。纹影图像显示得益于低压段内高比例氩气作为稀释气体,入射及反射激波均无分叉,为正激波结构,点火燃烧后对密度造成较大影响,流场中出现明显褶皱。针对燃烧过程的高速摄影图像显示激波后燃烧区域基本分为两部分,反射激波后小粒径雾化煤油完全燃烧呈现明亮的蓝色火焰,由于氧气的大量消耗随后将造成煤油液滴间的燃烧出现竞争关系,无法充分燃烧,出现分散的黄色火焰区,后期部分液滴由于贫氧及温度下降造成燃烧不充分而析出碳粒。     

超音速气流中氢燃料强化混合的燃烧实验研究

扼要介绍了在超音速气流中，采用后掠斜坡、多级喷射、振荡激波技术强化混合的氢燃料喷嘴，进行自点火和燃烧的实验概况。以实验模型结合喷射方式特点，分析了强化机理。实验表明，多级喷射的燃烧效率高，扩张型后掠斜坡喷嘴的抗干扰能力强，总压损失低，液体喷射产生的振荡激波能加强混合，提高燃烧效率。     

基于自适应网格的钝头体激波诱导燃烧现象数值模拟研究

钝头体激波诱导燃烧是爆震研究的一个基本问题。针对化学恰当量比的H2/Air预混气在Ma=4.79和Ma=6.46时的激波诱导燃烧现象开展数值模拟研究，采用基于有限体积法的块结构自适应网格加密程序AMROC对带化学反应源项的轴对称Euler方程解耦求解，考察了数值模拟中不同形式的MUSCL重构格式、限制器类型以及化学反应机理等重要因素对模拟结果的影响。结果表明，程序能够根据设定的加密判据较好地实现网格自适应加密，减小总网格量，实现高效数值模拟。通过与实验数据的对比，表明非定常激波诱导燃烧算例的准确程度不仅取决于化学反应机理，也取决于限制器类型，而采用两种不同形式的MUSCL重构格式获得的振荡频率则几乎一致，与试验结果的误差分别为1.17%和0.97%。模拟对比经典的Jachimowski机理和近年来新发展的几种包含压力相关反应步的氢/氧反应机理，模拟结果表明：对于Ma=4.79时的非定常激波诱导燃烧模拟，经典的Jachimowski机理仍然是能够给出与实验结果最接近的反应机理；而对于Ma=6.46时的定常激波诱导燃烧模拟，几种反应机理均能给出与实验吻合较好的结果。     

中心锥喷管喉道比参数对旋转爆轰燃烧影响的数值研究

旋转爆轰发动机的推进性能与尾喷管的设计有关。为探究中心锥喷管的喉道比参数如何影响旋转爆轰波的传播模态及旋转爆轰发动机的推进性能，采用三维欧拉方程结合氢气/空气基元反应模型，对不同喉道比参数下的旋转爆轰发动机进行了数值模拟与流动分析。数值结果显示，随着喷管喉道比的减小，旋转爆轰波依次呈现出稳定单波模态、单双波交替的混乱燃烧模态和爆燃燃烧模态。研究发现，喉道处产生的反射激波是影响RDW传播模态的关键因素。随着喉道比的减小，反射激波强度逐渐增强，并与新鲜来流混气作用引发局部热点，使单波模态转变为单双波交替的混乱燃烧模态；随着喉道比进一步减小，反射激波的高压作用使爆轰波熄爆，燃烧模态转变为爆燃燃烧。对推力性能的进一步分析表明，单波模态下发动机的推进性能随喉道比的减小而增强，且明显好于混乱模态和爆燃模态。     

液体射流在强化超音速燃烧中的应用

研究了在燃烧室入口马赫数为2的超音速燃烧中,液体射流所产生的振荡激波对强化超音速燃烧的作用。经过一维分析,证明了在离燃料喷嘴适当位置上喷射液体,所产生的振荡激波能强化超音速燃烧,提高燃烧效率。      

航空发动机砂尘吸入物静电监测仿真实验

提出了航空发动机砂尘吸入物静电监测的仿真实验方法,实验以软件ANSYS电磁场分析模块建立有限元模型为基础,模拟不同粒径、荷质比、运动速度及质量浓度情况下砂尘吸入物的静电感应信号,并分别从时域与频域对感应电荷与电压信号进行分析,研究砂尘吸入物的粒径及其他宏观参数与静电监测信号之间的关系,建立用以表征砂尘颗粒粒径大小的特征指标。基于IDMS(进气监测系统)感应电压信号功率谱密度分布建立了特征向量,并以其曼哈顿距离与欧氏距离作为特征指标表征砂尘颗粒粒径大小。经仿真实验验证:特征指标与砂尘粒径呈正相关,且不受砂尘吸入物运动速度及荷质比变化的影响,但受砂尘吸入物质量浓度影响。进一步研究将利用质量浓度对特征指标进行修正,并开展验证实验。      

采用非均匀反弹特性壁面的粒子分离器研究

为了在不改变流道几何型面的基础上实现对较大粒径砂尘轨迹的有效组织,借助数值仿真技术,对一类典型无旋式惯性粒子分离器流道内两相流场展开了模拟研究。通过对典型工况下粒子分离器内砂尘轨迹的追踪和细致分析,首先获得了壁面反弹主导下的较大粒径砂尘的三类基本运动模式及其主要特征。而后以此为基础,充分利用2024铝合金、7020橡胶以及45钢3种典型壁面在反弹特性上的差异,同时结合原流道型面,完成了一种基于非均匀壁面的粒子分离器方案设计。计算表明:通过对鼓包迎风面等关键区域的壁面材质的特殊设计,可在不降低气动性能的前提下实现AC砂及C砂分离效率的显著提升,其增幅分别为6.0%和13.7%。      

基于CFD-DEM耦合数值模拟的全尺寸直升机沙盲形成机理

为了研究直升机发生沙盲时沙尘云在悬停流场中的状态和分布规律,采用基于雷诺平均Navier-Stokes方程和Menter 剪切应力输运（SST）k-ω湍流模型的数值模型,通过应用程序编程接口耦合基于Hertz-Mindlin （No Slip）碰撞接触模型的离散元模型,并基于"多球法"构建了更加真实的非球形沙尘颗粒,计算了沙尘颗粒在流场中的运动和分布状态。与可得到的试验结果进行对比,验证了数值方法的有效性,并进行了地效状态旋翼拉力系数、桨尖涡位置以及沙尘云形成的宏观轮廓图的计算。应用所建立的方法,对不同悬停高度的直升机地效流场进行了计算,给出了流场的涡量以及速度云图,着重对比了不同悬停高度下沙尘云中沙尘颗粒速度和分布情况,分析了地效流场对沙尘颗粒状态的影响及沙尘云的形成机理,并计算出了沙尘云宏观分布图。结果表明：流场中大部分沙尘颗粒只能在地表随流场扩散而并不能形成沙尘云;沙尘云中外层空间的沙尘浓度比内层高;位于桨盘平面下层区域的沙尘颗粒以径向运动为主,切向速度较小,而位于桨盘平面上层的沙尘颗粒速度方向各异,速度大小接近。     

不同形状砂尘高速冲蚀TC4平板的数值仿真

含有砂尘的空气吸入发动机,会与压气机转子叶片以较高的相对速度发生碰撞,产生砂尘冲蚀现象,严重影响到飞行器飞行安全。通过采用能较好适应大变形的光滑粒子流体动力学(SPH)方法和有限元(FE)耦合的方法,建立不同形状砂尘冲蚀TC4平板模型,研究TC4平板表面受砂尘高速冲蚀的典型损伤形式及其规律。结果表明:砂尘尖角越小,冲击产生的弹坑越深,所造成的损伤也越大;随砂尘逐颗撞击平板,弹坑的深度变化越来越小,表现为平板表面的塑性硬化过程;在砂尘连续冲击下,受到冲击角的影响,损伤处的堆积物可能被砂尘冲脱平板,也可能被重新压回弹坑。      

Dust Near The Sun

We review the current knowledge and understanding of dust in the inner solar system. The major sources of the dust population in the inner solar system are comets and asteroids, but the relative contributions of these sources are not quantified. The production processes inward from 1 AU are: Poynting-Robertson deceleration of particles outside of 1 AU, fragmentation into dust due to particle-particle collisions, and direct dust production from comets. The loss processes are: dust collisional fragmentation, sublimation, radiation pressure acceleration, sputtering, and rotational bursting. These loss processes as well as dust surface processes release dust compounds in the ambient interplanetary medium. Between 1 and 0.1 AU the dust number densities and fluxes can be described by inward extrapolation of 1 AU measurements, assuming radial dependences that describe particles in close to circular orbits. Observations have confirmed the general accuracy of these assumptions for regions within 30° latitude of the ecliptic plane. The dust densities are considerably lower above the solar poles but Lorentz forces can lift particles of sizes < 5 μm to high latitudes and produce a random distribution of small grains that varies with the solar magnetic field. Also long-period comets are a source of out-of-ecliptic particles. Under present conditions no prominent dust ring exists near the Sun. We discuss the recent observations of sungrazing comets. Future in-situ experiments should measure the complex dynamics of small dust particles, identify the contribution of cometary dust to the inner-solar-system dust cloud, and determine dust interactions in the ambient interplanetary medium. The combination of in-situ dust measurements with particle and field measurements is recommended.     

Dust in Supernovae and Supernova Remnants I: Formation Scenarios

Supernovae are considered as prime sources of dust in space. Observations of local supernovae over the past couple of decades have detected the presence of dust in supernova ejecta. The reddening of the high redshift quasars also indicate the presence of large masses of dust in early galaxies. Considering the top heavy IMF in the early galaxies, supernovae are assumed to be the major contributor to these large amounts of dust. However, the composition and morphology of dust grains formed in a supernova ejecta is yet to be understood with clarity. Moreover, the dust masses inferred from observations in mid-infrared and submillimeter wavelength regimes differ by two orders of magnitude or more. Therefore, the mechanism responsible for the synthesis of molecules and dust in such environments plays a crucial role in studying the evolution of cosmic dust in galaxies. This review summarises our current knowledge of dust formation in supernova ejecta and tries to quantify the role of supernovae as dust producers in a galaxy.     

Dust Environment Modelling of Comet 67P/Churyumov-Gerasimenko

Dust is an important constituent of cometary emission; its analysis is one of the major objectives of ESA’s Rosetta mission to comet 67P/Churyumov-Gerasimenko (C–G). Several instruments aboard Rosetta are dedicated to studying various aspects of dust in the cometary coma, all of which require a certain level of exposure to dust to achieve their goals. At the same time, impacts of dust particles can constitute a hazard to the spacecraft. To conciliate the demands of dust collection instruments and spacecraft safety, it is desirable to assess the dust environment in the coma even before the arrival of Rosetta. We describe the present status of modelling the dust coma of 67P/C–G and predict the speed and flux of dust in the coma, the dust fluence on a spacecraft along sample trajectories, and the radiation environment in the coma. The model will need to be refined when more details of the coma are revealed by observations. An overview of astronomical observations of 67P/C–G is given, because model parameters are derived from this data if possible. For quantities not yet measured for 67P/C–G, we use values obtained for other comets, e.g. concerning the optical and compositional properties of the dust grains. One of the most important and most controversial parameters is the dust mass distribution. We summarise the mass distribution functions derived from the in-situ measurements at comet 1P/Halley in 1986. For 67P/C–G, constraining the mass distribution is currently only possible by the analysis of astronomical images. We find that both the dust mass distribution and the time dependence of the dust production rate of 67P/C–G are those of a fairly typical comet.     

Spatial distribution and orbital properties of interplanetary dust at high latitudes

Although the interplanetary dust cloud is assumed to be mainly concentrated in the ecliptic plane, there is a component of dust particles on highly inclined orbits that forms the out-of-ecliptic distribution. The ULYSSES mission for the first time makes this component accessible to in-situ, detection. Evidence for this dust component is also provided from the analysis of the Zodiacal light brightness and especially from the spherical shape of the solar F — corona. An obvious source for an out-of-ecliptic dust population is the activity of comets on high eccentric, highly inclined orbits. We discuss the dynamical conditions of particles under the influence of the radiation pressure when released from the comet and discuss their input to the dust cloud based on brightness analysis and in-situ results.     

微尘沉积形貌对冲击气膜冷却结构换热特性影响的数值研究

带有微尘的空气进入航空发动机,极易在涡轮叶片内冷通道发生沉积。为探究微尘沉积形貌对涡轮叶片内冷通道换热特性的影响,选取冲击气膜冷却结构,基于微尘沉积实验结果,构造微尘沉积形貌,由锥状突起和环状突起组成,通过数值模拟获得不同射流雷诺数下冲击靶面努塞尔数Nu。研究结果表明,冲击靶面微尘沉积层的出现,将大幅降低浸润面积平均努塞尔数Nuwetted,而对映射面积平均努塞尔数Nuavg影响较小;冲击驻点周围的高换热区范围减少;相邻冲击孔中点附近的高换热区努塞尔数Nu增大;此外,射流雷诺数的增大整体上提高了冲击靶面的换热强度。由于锥状突起和环状突起的扰动作用, 壁面附近回流涡增多, 使得冲击靶面大部分区域温度边界层厚度增加,因此换热性能降低。     

Cometary Dust

This review presents our understanding of cometary dust at the end of 2017. For decades, insight about the dust ejected by nuclei of comets had stemmed from remote observations from Earth or Earth’s orbit, and from flybys, including the samples of dust returned to Earth for laboratory studies by the Stardust return capsule. The long-duration Rosetta mission has recently provided a huge and unique amount of data, obtained using numerous instruments, including innovative dust instruments, over a wide range of distances from the Sun and from the nucleus. The diverse approaches available to study dust in comets, together with the related theoretical and experimental studies, provide evidence of the composition and physical properties of dust particles, e.g., the presence of a large fraction of carbon in macromolecules, and of aggregates on a wide range of scales. The results have opened vivid discussions on the variety of dust-release processes and on the diversity of dust properties in comets, as well as on the formation of cometary dust, and on its presence in the near-Earth interplanetary medium. These discussions stress the significance of future explorations as a way to decipher the formation and evolution of our Solar System.