斜向冲击强化换热特性试验

针对某型发动机主动间隙控制系统中典型冷却结构——45°斜向射流冲击,利用热膜法和红外热像仪测试技术,开展了局部强化冷却特性试验研究,分析了冲击雷诺数Re(33297～83242)、斜向冲击间距比H/d (2～6)等参数对冲击靶板表面局部换热特性参数Nu及Nu的影响.试验中发现位于驻点处和下游附驻点区出现了两个Nu峰值,当冲击Re较大、斜向冲击间距比H/d较小时,该现象尤为突出.试验结果表明:随着冲击Re的增大,靶板局部强化换热效果显著提升,Nu和Nu均显著增强;随着H/d的减小,驻点区域局部强化换热效果逐步提升,但增加幅度微弱;而在远离驻点区域,特别是在第二个峰值位置,冲击间距减小使得冲击强化换热效果明显增强.      

航空发动机排气喷管红外辐射特征数值研究

红外隐身技术对提高未来战机战场生存力具有重要意义,发动机排气系统是飞机后半球的主要红外辐射源。为了研究涡扇发动机排气喷管的红外辐射特性,采用与成熟商用CFD软件相结合的策略,基于离散传递方法,自主开发航空发动机排气系统红外辐射特征数值计算软件。提出一种射线行程追踪方法,用来提高软件计算效率和模拟精度;最后用该软件对某型涡扇发动机排气系统收缩喷管及两种采用不同红外抑制措施的喷管进行数值模拟研究。结果表明：相对于传统的收缩喷管,二元喷管能够在绝大部分探测方向上有效降低喷管的红外辐射,引射喷管可在大角度探测方向上起到显著的红外隐身效果。     

航空发动机表面发射率测量技术研究

测试发动机放热率的核心技术是在运行过程中获得发动机的表面发射率。介绍了航空发动机表面发射率的测量技术,阐述了应用前置反射器辐射温度计和动态红外数字成像仪测量固体表面发射率的原理和方法,提出了航空发动机表面发射率测量中应注意的事项,对几种发动机常用的材料分别采用上述2种方法进行了测量,试验结果表明了2种测量方法的可行性。     

双S弯喷管流动特性及红外辐射特性分析

基于分区控制技术,发展了型面易控的双S弯喷管型面设计方法,用CFD数值模拟技术,对双S弯喷管的流动特性进行了数值模拟.采用信息通道界面(MPI)并行算法编写了基于离散传递法的红外辐射特性计算程序,对双S弯喷管红外辐射特性进行了计算,并与具有相同进出口面积的轴对称收缩喷管的红外辐射特性进行了对比.研究表明:双S弯喷管宽边探测面红外辐射强度低于窄边探测面红外辐射强度,最大幅度为80%;与轴对称收缩喷管相比,双S弯喷管红外辐射强度明显降低,尤其在宽边探测面的30°~40°探测方向上,比轴对称收缩喷管的红外辐射强度低大约30%.      

基于传声器阵列的航空发动机噪声源识别研究

为了实现新一代发动机的噪声源识别技术,对于测试所得到的民用飞机发动机的整体噪声数据,通过部件噪声分解方法,将其分解到各个部件,并且认识当代民用飞机发动机噪声源的基本特征.开发出利用发动机整机噪声数据的噪声源识别系统,采用反卷积法将波束成型法的结果作为中间声源,从中获取所需要的声源信息,使得最终的结果更加准确.通过获取的发动机整机噪声数据,验证传声器阵列技术的可行性,并且证明了系统的可行性和有效性.     

收扩喷管加小突片对尾喷流红外辐射的影响

针对收扩喷管,在高温(约640℃)、高速(超音速)流动状态下,实验研究了加装小突片后对飞机发动机尾喷流红外辐射的抑制效果,并探讨了小突片堵塞比、小突片后倾角度等因素对红外辐射抑制特性的影响。结果表明,小突片对热射流的红外辐射具有明显的抑制作用,不仅使热射流的核心区长度大为缩短,而且使热射流的总体红外辐射信号大幅度下降(在本文实验范围内,最大可下降约57%)。      

带有双层壁扩压器的波瓣喷管混合流场的数值计算

采用三维贴体曲线坐标网格,边界网格加密且正交,在整个计算区域进行全场计算。为避免因波瓣造成的网格强烈的非正交引起解的发散,采用了Chen和Kim修正的k-ε湍流模型及同位网格SIMPLC计算方法,对带有双层壁扩压器的波瓣喷管混合流动进行了数值计算和分析。对波瓣及双层壁,采用大粘性的方法解决流固耦合。计算结果表明:在双层壁间有外界冷气流被引射进入,形成了壁面的冷却气流;自波瓣出口截面沿流向产生的环流速度场,强化了主次流的掺混,速度分布渐趋均匀。计算结果与实验数据符合良好,二者在离开波瓣52 mm的混合管内相对主流速度的最大误差为21.65 %。     

超音尾喷流红外抑制方案的研究

超音速发动机尾喷流的红外抑制是超音速飞行器隐身性能的重要组成部分。本文提出两种超音速尾喷流的红外抑制方案二次旋流方案与组合波瓣方案 ,并对两种方案共 7组试验件在不同的结构和二次流速度情况下进行了大量重复试验。在旋流方案试验中 ,对二次流加旋诱发大尺度流向涡进行了系统的研究 ,得到旋流角度、二次流速度等对掺混效果的影响规律 ,试验结果表明 :对于本结构方案 ,当二次流速度为 49m/s,旋流角在 3 0°左右 ,掺混效果最好 ,且随二次流流速的增加而加强。在组合波瓣方案的试验中 ,对组合波瓣用于超音尾喷流红外抑制进行了研究 ,试验结果表明可对超音尾喷流的红外起到有效的抑制作用。     

The Cassini Visual And Infrared Mapping Spectrometer (Vims) Investigation

The Cassini visual and infrared mapping spectrometer (VIMS) investigation is a multidisciplinary study of the Saturnian system. Visual and near-infrared imaging spectroscopy and high-speed spectrophotometry are the observational techniques. The scope of the investigation includes the rings, the surfaces of the icy satellites and Titan, and the atmospheres of Saturn and Titan. In this paper, we will elucidate the major scientific and measurement goals of the investigation, the major characteristics of the Cassini VIMS instrument, the instrument calibration, and operation, and the results of the recent Cassini flybys of Venus and the Earth–Moon system.This revised version was published online in July 2005 with a corrected cover date.     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.