多股自耦合射流相干流动和换热特性数值研究

采用数值模拟的方法对多股自耦合射流在相干条件下的流动和换热特性进行了研究.研究结果表明:三股自耦合射流都在出口附近耦合成一股射流向下游运动,两侧的射流受到中间一股射流的卷吸融合在一起,融合后仍然是一股沿中心线对称的自耦合射流.在短轴中心截面自耦合射流型面较宽,射流喷出后在下游的扩展角度大,而长轴中心截面射流的型面较窄,扩展角度较小.在冲击靶板上,整个冲击区域呈现出中心温度最低的近似圆形的对称性分布,对流换热系数曲线呈现出中心对称的波峰分布形状,表明自耦合射流驻点区换热最强.对流换热系数沿靶板不同方向的分布趋势基本保持一致.      

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。      

两股互击式喷嘴雾化研究及应用

用激光全息及图像处理技术,研究两股互击式喷嘴的撞击状况及雾化性能,获得了喷嘴的雾化性能参数,在喷嘴的水试雾化性能、热试燃烧效率及比冲对比后,提出用水试雾化性能评估其热试效果,检验喷嘴的加工质量。此技术已用于小推力发动机喷嘴的筛选。     

椭圆截面喷管排气辐射热流数值分析

本文对直升机红外抑制器椭圆截面喷管排气的辐射热流进行数值分析,并预估排气温度分布速度和燃气成分分布对辐射热流的影响。为了正确计算辐射热流,本文采用六热流辐射模型来考虑尾焰对周围环境传热的影响。紊流模型采用修正的双方程k—ε模型。由于喷管出口截面为椭圆形,因此排气为三元自由射流,控制方程为抛物型偏微分方程,可采用前进积分求解。计算结果与试验结果基本一致,说明本计算方法是可行的。     

非牛顿流体射流雾化特性研究进展

本文总结了有关非牛顿流体射流雾化特性的研究进展。首先,阐述了预测非牛顿液体射流初次雾化失稳特性的理论方法,介绍了有关非牛顿流体射流初次雾化的实验现象和特性参数。当射流初次雾化的过程结束后,破碎产生的液滴会在高速气流中发生二次雾化。随后,总结了国内外有关非牛顿流体液滴二次雾化实验研究的相关进展。分析了液滴二次雾化的实验现象,总结了不同种类液滴二次雾化过程中所研究特性参数,如破碎模态、临界韦伯数和初始变形时间等随来流气体参数之间的关系,并介绍了基于液滴二次雾化物理过程所建立的预测喷雾场液滴平均粒径的雾化模型。最后,基于目前的研究现状,给出了非牛顿液体射流初次雾化和二次雾化实验研究的后续重点研究方向及建议。     

旋转条件下带出流孔的受限空间内冲击换热

以旋转涡轮叶片内部冷却为背景,在旋转条件下对带出流孔的受限空间内冲击换热特性进行了实验研究。在冲击与旋转方向、相反两种情况下,通过改变冲击雷诺数Rej(5 000~10 000)、旋转数Ro(0~0.003 4)、无因次温比(Tw-Tf)/Tw(0.056~0.134)对冲击靶面的平均换热特性进行了研究。研究发现,靶面的换热随冲击雷诺数的增加而变好;旋转对冲击换热的削弱在雷诺数较大时表现更明显;实验参数范围内浮升力对换热的影响较小;离心力、哥氏力等对换热的影响程度与内部空气的流动结构及出流方式有关。     

解决湍流圆/平射流异常现象的数值研究

圆射流/平面射流异常现象是湍流研究领域的一个著名的难题,是验证湍流微分方程模型的试金石。本文用GAO-YONG不可压湍流控制方程对圆射流进行了数值验证,成功地解决了该难题,进一步证明了该方程对真实湍流的适定性和通用性。      

Formation of relativistic jets by collapsing stars to black holes

Formation of relativistic jets in the magnetosphere of collapsing stars is considered. These jets will be formed in the polar caps of magnetosphere of collapsing star, where the stellar magnetic field increases during the collapse and the charged particles are accelerated. The jets will generate non-thermal radiation. The analysis of dynamics and emission of particles in the stellar magnetosphere under collapse shows that collapsing stars can be powerful sources of relativistic jets.     

On ultra-high energy cosmic rays: Origin in AGN jets and transport in expanding universe

The cosmic ray source spectrum produced by AGN (active galactic nucleus) jets is calculated. A distinctive feature of these calculations is the account for the jet distribution on kinetic energy. The expected cosmic ray spectrum at the Earth is determined with the use of a simple numerical code which takes into account interactions of ultra-high energy protons and nuclei with the background radiation in an expanding universe.     

Determination of temperature maps of EUV coronal hole jets

Coronal hole jets are fast ejections of plasma occurring within coronal holes, observed at Extreme-UltraViolet (EUV) and X-ray wavelengths. Recent observations of jets by the STEREO and Hinode missions show that they are transient phenomena which occur at much higher rates than large-scale impulsive phenomena like flares and Coronal Mass Ejections (CMEs). In this paper we describe some typical characteristics of coronal jets observed by the SECCHI instruments of STEREO spacecraft. We show an example of 3D reconstruction of the helical structure for a south pole jet, and present how the angular distribution of the jet position angles changes from the Extreme-UltraViolet-Imager (EUVI) field of view to the CORonagraph1 (COR1) (height ∼2.0 R_⊙ heliocentric distance) field of view. Then we discuss a preliminary temperature determination for the jet plasma by using the filter ratio method at 171 and 195 Å and applying a technique for subtracting the EUV background radiation. The results show that jets are characterized by electron temperatures ranging between 0.8 and 1.3 MK. We present the thermal structure of the jet as temperature maps and we describe its thermal evolution.