复合材料在红外隐身技术中的应用

根据红外隐身原理,将应用于红外隐身技术的复合材料进行分类阐述,分析复合材料在红外隐身技术中的地位和应用前景,并着重介绍了本实验室在基于热电制冷器（TEC）的智能温控复合材料系统方面的研究成果。研制了针对不同具体应用条件的多种智能温控复合材料系统;建立了智能温控复合材料系统的制冷性能理论计算模型;并考察TEC热电元件臂长、TEC热端散热方式等因素对系统温控效果的影响,进一步优化了智能温控效果,使该智能温控材料能够根据设定温度的复杂变化做出快速响应。最后对智能温控复合材料在红外隐身技术中的应用进行了总结和展望。     

导电高分子电致变色材料及其在飞行器和军事伪装中的应用

概述了导电高分子(CPs)作为新型电致变色材料的特点、电致变色原理及红外发射器件的设计，并对国外在飞行器导热控制和红外、雷达伪装上的应用发展状况进行了介绍。     

Calculation of high-temperature insulation parameters and heat transfer behaviors of multilayer insulation by inverse problems method

In the present paper, a numerical model combining radiation and conduction for porous materials is developed based on the finite volume method. The model can be used to investigate high-temperature thermal insulations which are widely used in metallic thermal protection systems on reusable launch vehicles and high-temperature fuel cells. The effective thermal conductivities（ECTs） which are measured experimentally can hardly be used separately to analyze the heat transfer behaviors of conduction and radiation for high-temperature insulation. By fitting the effective thermal conductivities with experimental data, the equivalent radiation transmittance, absorptivity and reflectivity, as well as a linear function to describe the relationship between temperature and conductivity can be estimated by an inverse problems method. The deviation between the calculated and measured effective thermal conductivities is less than 4%. Using the material parameters so obtained for conduction and radiation, the heat transfer process in multilayer thermal insulation（MTI） is calculated and the deviation between the calculated and the measured transient temperatures at a certain depth in the multilayer thermal insulation is less than 6.5%.     

波瓣喷管/气膜冷却混合管气动和红外辐射特性实验

 针对某型后向进气、前向排气的涡轴发动机用红外抑制器,提出了波瓣喷管和气膜冷却混合管组合的红外抑制概念,旨在进一步降低混合管壁面红外辐射强度。用实验的方法,对气膜混合管内流特性、红外辐射特性进行了研究。研究结果表明：混合管壁面的3个引射入口的静压都低于外界大气压力,从而自然形成引射驱动动力;引射流量比与主、次流温度比有关,通过实验得到的温度修正指数可以将冷态实验结果外推到热态情况;与一般混合管相比,整体引射流量提高30％,在3~5 μm波段内,红外辐射强度降低了12%~27%,在8~14 μm波段内,红外辐射强度降低了12%~28%,其总压损失仅仅提高了1%。     

具有周期性薄膜热源的多层介质非稳态传热数值仿真

为分析具有薄膜热源的多层介质非稳态传热问题,以某型飞机层合电加温风挡为例,构建了一种热流密度-温度边界条件,实现了薄膜热源热流和温度属性向多层介质内外两个方向上的实时传递,再现了薄膜热源温度对临近多层介质表面温度的影响,为具有薄膜热源的多层介质传热问题分析和加温控制规律设计提供了一种可行方法.     

利用红外技术进行层板冷却特性实验研究

为了研究层板冷却特性,应用远红外热像测温技术,对一个真实尺寸的层板结构进行了实验.层板的气膜孔、绕流柱及冲击孔直径分别为0.,0.8,0.8 mm,内腔高及总板厚分别为0.8,2.6 mm,孔柱数比为1:4:1.为了准确测量表面温度,采用了高精度热电偶校正法,建立修正关系;为了描述层板综合冷却效率,采用热像数字信号运算法,直接进行数据处理.实验在高温亚声速风洞中进行,实验结果展示了冷却介质注射量对层板冷却特性的影响,证明远红外热像技术用来研究层板冷却特性是一种有效的方法.      

基于增强型离散相模型和化学燃烧的红外诱饵弹建模方法

红外（IR）诱饵弹是一种主要的红外对抗武器，建立一种准确的红外诱饵弹模型将对红外制导算法的研究起重要作用。目前，针对红外诱饵弹的计算机流体仿真（CFD）建模方法中，通常不考虑红外药剂的燃烧对红外模型产生的影响，这将从机理上直接导致建模精度下降。针对这一不足，本文在增强型离散相模型（DPM）红外诱饵弹建模方法的基础上加入了化学燃烧相，建立了准确性更高的仿真模型。实验结果表明，与原有的模型相比，加入化学燃烧相后的新模型在图形特征的仿真精度上有明显提升。     

飞机座舱有机玻璃透明导电膜的制备及透光和微波散射性能

研究了用溅射法在飞机座舱有机玻璃上镀制金属-介质组合透明导电膜的工艺 ;测试和分析了金膜、银膜、氧化钛膜的光学特性、导电性及形貌结构 ;按薄膜光学原理进行膜系匹计算 ,并分别镀制了 Ti O2-Au-Ti O2 、 Ti O2-Ag-Ti O2 组合透明导电膜。在 40 0～ 760 nm可见光波段内 ,透光率分别达到了 74%和 81 % ,在 8～ 1 2 GHz频段内对垂直入射的微波 ,反射率分别达到-1 .1 d B和-0 .8d B。     

基于合作目标和视觉的无人飞行器全天候自动着陆导引关键技术

 GPS受他国控制和易受干扰对基于该导航系统的无人飞行器导航和着陆具有潜在危险,为了使其安全自动着陆,提出通过在着陆跑道(广场或公路)上预设具有受控发射红外光的地面合作目标,实现无人飞行器的视觉全天候自动精确着陆新技术。首先研究得到切实可行的工作过程;然后研制了合作目标,通过理论分析和实验得出,无论能见度高低,8~12 μm中远红外视觉系统探测到的合作目标图像质量远优于可见光视觉系统,研究得到合作目标和背景的温差在170~200 ℃时,成像效果最好。在识别研究中发现,基于传统的不变矩算法对合作目标的识别可靠性稍差,为了进一步准确地识别合作目标,又提出了基于方向链码的合作目标识别算法,该方法的耗时为不变距的96%,但是识别的可靠性比前者有显著提高。     

固液混合火箭发动机喷焰红外辐射特性分析

为了研究固液混合火箭发动机喷焰在不同飞行状态的红外辐射特性,建立了固液两相状态下喷焰的红外辐射计算模型,获得了喷焰在2~12μm波段的红外辐射.将喷焰的温度、压力、摩尔组分等作为输入条件,米氏散射(Mie)模型计算颗粒相的散射,采用有限体积法(FVM)离散辐射传递方程,利用中分辨率大气辐射传输(MODTRAN)模型计算不同观测距离的大气透过率,编程计算得到不同飞行高度,不同观测方向下喷焰的红外辐射.结果表明喷焰红外辐射亮度与温度分布类似,在2.7~3.0μm和4.2~4.5μm波段范围内的辐射较强,高温粒子在近红外比远红外对总辐射的贡献大,太空与地面观测不同飞行高度的发动机喷焰辐射率因大气衰减的不同而有所差异,可为目标跟踪与发动机设计提供参考.      

飞行器红外隐身效能工程评价方法

 针对飞行器的红外隐身问题,推导出红外辐射对比度与作用距离的理论关系,采用指数拟合获得大气透过率与作用距离的近似关系表达式,简化了对作用距离的计算,并通过实际算例考察了目标表面温度、目标发射率和飞行速度对红外辐射对比度及作用距离的影响。结果表明：对比度和作用距离随目标表面温度、发射率及飞行速度的下降趋势基本一致;在一定条件下,对比度可代替作用距离作为评价目标红外隐身效果的简单、快速的参数,对比度越小目标的红外隐身效果越好。对比度的计算快速、准确、灵活性强和适用范围广,为今后进一步对飞行器的红外隐身研究提供一定的理论参考。     

基于红外视觉/激光雷达融合的目标识别与定位方法

近年来,基于可见光图像的目标识别在无人车感知领域得到了广泛应用.然而,可见光图像目标识别无法应用于弱光和黑暗环境.针对于此,提出了一种基于红外视觉/激光雷达融合的目标识别与定位算法.首先,通过基于颜色迁移的数据增强训练方法,提高了红外目标识别算法的泛化性能.继而,提出了一种基于激光雷达修正的单目深度估计方法,通过视觉图像与激光雷达点云的数据融合,实现了基于稠密深度图对目标位置的估计,提高了对小目标的定位能力.试验结果表明,与传统Yolov3目标识别算法相比,该算法平均识别准确率可提升5.8％;此外,相对定位算法将包含小目标在内的物体相对定位精度提高了13.4％.     

各向异性复合材料平板气膜冷却特性实验和数值研究

针对不同编织方式形成的复合材料平板气膜冷却开展了实验研究，利用红外热像仪测量了热侧壁面的温度场分布，分析了平板导热系数、吹风比、主流温度等参数对综合冷却效率的影响。在实验验证的基础上，进一步对单向增韧特点的复合材料进行数值模拟,分析了X、Y、Z三个方向导热系数对单孔气膜冷却壁面温度场分布和综合冷却效率的影响。结果表明:随着吹风比的升高，气膜综合冷却效率升高；随着主流温度的升高，气膜冷却效率降低；25D编织复合材料冷却效率最高，3D编织复合材料冷却效率最低。各向异性复合材料内部的温度梯度、传热量都与材料的导热系数特征有关，X方向和Z方向的导热系数增大，沿程综合冷却效率升高；而Y方向导热系数的增大对气膜冷却效率几乎没有影响。      

可见光迷彩低红外发射率薄膜制备及其特性

采用多弧离子镀技术,在Al基底上制备了TiO2/TiN多层膜。通过控制基底材料的粗糙度使制备出的薄膜在可见波段具有非镜面反射效果。采用扫描电镜、红外辐射率测量仪、紫外-可见-近红外光光度计等测试手段对薄膜样品进行了表征。结果表明,采用多弧离子镀法在Al基底上制备了结合力良好、具有迷彩效果的低红外发射率薄膜。研究发现,随氧化层厚度增加,薄膜发射率趋向稳定(0.2左右)。薄膜电阻随氧化层厚度的变化无明显变化。     

Al/Ni含能多层膜在Al2O3陶瓷/不锈钢焊接中的应用

采用磁控溅射设备,生长AuSn合金做焊料层、Al/Ni含能多层膜做热量提供层,实现了不锈钢和Al_2O_3间的异质材料自蔓延高温扩散焊。利用SEM、XRD和DSC等测试手段表征AuSn合金和Al/Ni含能多层膜的微观形貌、相成分和放热量;用万能试验机测试焊接接头的力学性能。结果表明,AuSn合金的质量比基本达到80∶20,而多层膜的层状结构清晰,反应热达到1 239 J/g。焊接实验结果表明,仅使用AuSn焊料时,剪切强度仅为46 MPa,在增加Al/Ni含能多层膜后,其剪切强度可达90 MPa,强度提高了约一倍。焊接接头的界面显微形貌和相结构研究表明,剪切强度的增强主要是Al/Ni多层膜提供了额外能量使得界面处的反应剧烈,陶瓷金属化层与中间层的反应加剧,形成了新的反应生成物。     

Obscured Activity: AGN, Quasars, Starbursts and ULIGs Observed by the Infrared Space Observatory

Some of the most ‘active’ galaxies in the Universe are obscured by large quantities of dust and emit a substantial fraction of their bolometric luminosity in the infrared. Observations of these infrared luminous galaxies with the Infrared Space Observatory (ISO) have provided a relatively unabsorbed view to the sources fuelling this active emission. The improved sensitivity, spatial resolution and spectroscopic capability of ISO over its predecessor Infrared Astronomical Satellite (IRAS) of enabled significant advances in the understanding of the infrared properties of active galaxies. ISO surveyed a wide range of active galaxies which, in the context of this review, includes those powered by intense bursts of star formation as well as those containing a dominant active galactic nucleus (AGN). Mid-infrared imaging resolved for the first time the dust enshrouded nuclei in many nearby galaxies, while a new era in infrared spectroscopy was opened by probing a wealth of atomic, ionic and molecular lines as well as broad band features in the mid- and far-infrared. This was particularly useful, since it resulted in the understanding of the power production, excitation and fuelling mechanisms in the nuclei of active galaxies including the intriguing but so far elusive ultraluminous infrared galaxies. Detailed studies of various classes of AGN and quasars greatly improved our understanding of the unification scenario. Far-infrared imaging and photometry revealed the presence of a new very cold dust component in galaxies and furthered our knowledge of the far-infrared properties of faint starbursts, ULIGs and quasars. We summarise almost nine years of key results based on ISO data spanning the full range of luminosity and type of active galaxies.     

钙钛矿型La_(1-x)Ba_xMnO_3(0≤x≤0.5)的红外发射率和微波吸收性能

通过溶胶凝胶法制备钙钛矿结构的La_(1-x)Ba_xMnO_3(0≤x≤0.5),利用X射线衍射、四探针电阻测量仪、红外发射率测试仪、矢量网络分析仪分别研究Ba~(2+)掺杂对镧锰氧化物晶体结构、电阻率、红外发射率和微波吸收性能的影响。研究结果表明:当Ba~(2+)掺杂浓度比较低时,掺杂的元素几乎不改变镧锰氧化物的晶体结构;当掺杂浓度增加时,晶格畸变开始增大;样品红外发射率随Ba~(2+)离子掺杂浓度的增大先降低后缓慢增加,与电阻率的变化保持一致;Ba~(2+)离子可以对样品在2~18 GHz微波吸收性能进行调控,当掺杂浓度x=0.3时,样品的吸收效果最佳;在频率为10.8 GHz时,最低反射率为-32 d B;掺杂合适元素的镧锰氧化物材料有可能应用在红外/雷达兼容隐身领域。     

热障涂层杨氏模量和泊松比的测试

为了降低航空发动机热端部件的温度,空气等离子喷涂已被广泛地应用。为确定热障涂层的残余应力、结合力、断裂韧性、疲劳裂纹扩展速率等性能和特性,需要知道其杨氏模量和泊松比。因为涂层厚度非常薄且使用时是结合在基体上的,所以需要一个能够在原处测量涂层的杨氏模量和泊松比的方法。采用等离子喷涂工艺在GH150高温合金上喷涂了MCrAIY和陶瓷层,利用一种改进的悬臂梁方法测量了热障涂层的杨氏模量和泊松比。这种无损测试方法为测定其他薄膜材料的杨氏模量和泊松比提供了借鉴。     

Infrared irradiance calibration

Infrared astronomical measurements are calibrated against reference sources, usually primary standard stars that are, in turn, calibrated either by direct or indirect means. A direct calibration compares the star with a certified source, typically a blackbody. Indirect methods extrapolate a direct measurement of the flux at one wavelength to the flux at another. Historically, α Lyr (Vega) has been used as the primary standard as it is bright, easily accessible from the northern hemisphere, and is well calibrated in the visual. Until recently, the direct absolute infrared calibrations of α Lyr and those derived from the absolute solar flux scaled to the observed spectral energy distributions of solar type stars increasingly diverged with wavelength from those obtained using a model atmosphere to extrapolate the absolute visual flux of Vega into the infrared. The exception is the direct calibration by the 1996/97 Midcourse Space Experiment of the absolute fluxes for a number of the commonly used infrared standard stars, including Vega.In the mid-1980s, the Air Force Geophysics Laboratory began a program that led to the establishment of a network of stars with which to calibrate infrared space-based sensors. α Lyr and a CMa were adopted as the fundamental references and the absolute 1.2 to 35 µm infrared spectral energy distributions for the 616 secondary standard stars in the network were derived through spectral and photometric comparisons with the primary standards. The stars are also used for calibration at ground-based infrared observatories. For applications in which the network stars may not be bright enough, particularly at the longer infrared wavelengths, planets and the larger asteroids are used. Planets and asteroids move and rather sophisticated thermal modeling of the bodies is required to predict the disk-integrated brightness at a specific time with reasonable accuracy. The Infrared Space Observatory applied such a sophisticated ‘thermo-physical’ model to the largest asteroids to support calibration of the sensors to a claimed accuracy of within 5%. The AFRL program also created a spectral atlas of the brightest stars in the sky that, although they are variable, may be used for calibration if the large(r) attendant uncertainties are acceptable.This revised version was published online in July 2005 with a corrected cover date.     

Infrared Irradiance Calibration

Infrared astronomical measurements are calibrated against reference sources, usually primary standard stars that are, in turn, calibrated either by direct or indirect means. A direct calibration compares the star with a certified source, typically a blackbody. Indirect methods extrapolate a direct measurement of the flux at one wavelength to the flux at another. Historically, α Lyr (Vega) has been used as the primary standard as it is bright, easily accessible from the northern hemisphere, and is well calibrated in the visual. Until recently, the direct absolute infrared calibrations of α Lyr and those derived from the absolute solar flux scaled to the observed spectral energy distributions of solar type stars increasingly diverged with wavelength from those obtained using a model atmosphere to extrapolate the absolute visual flux of Vega into the infrared. The exception is the direct calibration by the 1996/97 Midcourse Space Experiment of the absolute fluxes for a number of the commonly used infrared standard stars, including Vega.In the mid-1980s, the Air Force Geophysics Laboratory began a program that led to the establishment of a network of stars with which to calibrate infrared space-based sensors. α Lyr and a CMa were adopted as the fundamental references and the absolute 1.2 to 35 µm infrared spectral energy distributions for the 616 secondary standard stars in the network were derived through spectral and photometric comparisons with the primary standards. The stars are also used for calibration at ground-based infrared observatories. For applications in which the network stars may not be bright enough, particularly at the longer infrared wavelengths, planets and the larger asteroids are used. Planets and asteroids move and rather sophisticated thermal modeling of the bodies is required to predict the disk-integrated brightness at a specific time with reasonable accuracy. The Infrared Space Observatory applied such a sophisticated ‘thermo-physical’ model to the largest asteroids to support calibration of the sensors to a claimed accuracy of within 5%. The AFRL program also created a spectral atlas of the brightest stars in the sky that, although they are variable, may be used for calibration if the large(r) attendant uncertainties are acceptable.