机载曳光弹的紫外产生机理

立足于现有装备的基础上,大力发展经济,可靠,方便的紫外干扰技术,对我军而言不啻是一种我服的有效手段,在原子物理学理论指导下,本文详细地介绍了产生紫外线光谱重要的一环,原子材料紫外光谱的产生方法,文章的末尾还给出了实验的结果。     

Low-velocity impact response and infrared radiation characteristics of thermoplastic/thermoset composites

The low-velocity impact response and infrared radiation characteristics of composites have rarely been focused on simultaneously. This study aims to investigate the low-velocity impact response and infrared radiation characteristics of the glass fiber reinforced thermoplastic polypropylene and carbon fiber reinforced thermosetting epoxy resin laminates wildly used in the aircraft industry. The impact tests were conducted at five energy levels. Characterization parameters such as impact load, dis...     

智能分段测速系统的研制

介绍了一种基于单片机和红外线位置检测装置测量运动员通过各个不同路段速度的基本原理及方法,对此系统的功能、结构特点作了详细介绍并对测量误差进行了分析。     

富氮高能物质BTATz的热分解动力学和分解机理

为获得富氮高能物质3,6-双(1氢-1,2,3,4-四唑-5-氨基)-1,2,4,5-四嗪(BTATz)的热分解动力学参数、热分解机理函数、气相和凝聚相变化,为建立燃烧过程数学模型提供关键性热化学、热力学和化学动力学参数,通过热重(TG)、差示扫描量热(DSC)和气体(固体)原位反应池/快速扫描傅里叶变换红外光谱(RSFTIR)联用技术,研究了BTATz的热分解。实验结果显示BTATz的热分解过程对压强不敏感。基于Ozawa,Kissinger和Coats-Redfern方法,计算获得了BTATz的热分解动力学参数和方程。Kissinger法求得的活化能Ea和指前因子lgA分别为317.41 kJ.mol-1和28.07s-1。热分解反应机理服从n=1.5的Avrami-Erofeev方程,其热分解反应的动力学方程为dαdt=1.5×1028.07exp(-3.8178×104/T)(1-α)[-1n(1-α)]1/3。分析提出了BTATz的热分解机理,BTATz的热分解是从四嗪和四唑环的开环断裂开始的,分解产物又发生二次反应,465℃热分解凝聚相产物为NH4N3,聚胺和嘧嘞胺。     

任意形状凹面和相互可视表面φ2,φ3的分析计算

推导了空间任意形状凹面和相互可视表面的地球红外角系数φ３和地球反照角系数φ２的计算公式；并运用ＭｏｎｔｅＣａｒｌｏ法对半球凹地、抛物凹面、面相互可视的直角平板、平板表面外凸出圆柱表面的地球反照角系数和地球红外角系数进行了计算。运用这种方法，可以计算任意形状凹面和相互可视表面的φ２、φ３。     

喷管超声段壁面冷却热态试验研究

在高温条件下，对三种轴对称收－扩喷管超声段壁面排气引射冷却方案（缝隙式气膜冷却、离散孔气膜冷却和冲击－气膜组合冷却）进行了试验研究。得到了不同冷却方案的壁面压力分布、壁面温度分布和红外辐射特性，以及冷却气流量对这些性能的影响。结果表明：采用排气引射冷却技术可以大幅度降低喷管的壁温和红外信号特征，其中缝隙式气膜冷却的应用前景最好，离散孔式气膜冷却值得深入研究，冲击－气膜组合冷却不适合作为喷管排气引射冷却的基本方案。     

红外与可见光图像融合的空间碎片识别方法

针对暗弱空间环境中空间碎片的识别问题,提出了一种光照不均匀环境中的空间碎片识别方法。不同于现有识别方案,该方法从光照不均匀导致空间碎片图像源细节丢失造成识别性能下降的角度出发,首先将空间碎片的红外和可见光图像进行深度融合,并建立空间碎片融合图像数据库,然后基于训练样本采用深度学习技术训练得到空间碎片识别模型。算法分析表明,该图像融合方案具有高度的细节保留能力,识别模型具有在暗弱环境中高精度目标识别能力。最后进行了仿真实验,实验结果表明,该识别方案在姿态变化、图像源亮度变化等干扰条件下都具有较好的鲁棒性。     

红外成像制导中目标图像序列的仿真生成

在红外成像制导技术的算法研究中，目标红外图像序列是进行仿真验算的基础，通常真实的图像序列较难获得，本文通过建立空间目标的透《视投影模型来模拟红外成的过程，并由计算机作图得到目标的二值图像，为目标识别、跟踪算法及制导率的仿真验算打下了基础。     

The infrared space observatory (ISO)

The Infrared Space Observatory (ISO), a fully approved and funded project of the European Space Agency (ESA), is an astronomical satellite, which will operate at wavelengths from 2.5–240 m. ISO will provide astronomers with a unique facility of unprecedented sensitivity for a detailed exploration of the universe ranging from objects in the solar system right out to distant extragalactic sources. The satellite essentially consists of a large cryostat containing at launch over 2000 litres of superfluid helium to maintain the Ritchey-Chrétien telescope, the scientific instruments and the optical baffles at temperatures between 2 K and 8 K. The telescope has a 60-cm diameter primary mirror and is diffraction-limited at a wavelength of 5 m. A pointing accuracy of a few arc seconds is provided by a three-axis-stabilisation system consisting of reaction wheels, gyros and optical sensors. ISO's instrument complement consists of four instruments, namely: an imaging photo-polarimeter (2.5–240 m), a camera (2.5–17 m), a short wavelength spectrometer (3–45 m) and a long wavelength spectrometer (43–196 m). These instruments are being built by international consortia of scientific institutes and have been delivered to ESA for in-orbit operations. ISO will be launched in September 1995 by an Ariane 4 into an elliptical orbit (apogee 70000 km and perigee 1000 km) and will be operational for at least 18 months. In keeping with ISO's role as an observatory, the majority of its observing time is being made available to the general astronomical community via a Call for Observing Proposals.     

Olbers an interplanetary probe to study visible and infrared diffuse backgrounds

The visible extragalactic background (though as yet undetected) is insufficient to explain the abundance of heavy elements in galaxies: either there should be some diffuse extragalactic light in the near infrared (from 1 to 10 m) and/or in the far infrared (100 m) if dust has reprocessed the star light. We propose a new space mission to be dedicated to the search and mapping of primordial stellar light from the visible to the mid-infrared (20 m). In this spectrum range, detectors have reached such a sensitivity that the mission should aim at being (source) photon noise limited, and not any longer background photon noise limited. For that purpose, a small passively cooled telescope with large format CCDs and CIDs could be sent beyond the zodiacal dust cloud (which is absent beyond a solar distance of about 3 AU). In that case, the only remaining foregrounds before reaching the extragalactic background, is due to the Milky Way integrated emission from stars and the diffuse galactic light due to scattering and emission by interstellar dust, which are all unavoidable. Maps of the extragalactic light could be obtained at the arcminute resolution with high signal to noise ratio. This mission is the next logical step after IRAS, COBE and ISO for the study of extragalactic IR backgrounds. It has been proposed as a possible medium-sized mission for the post-horizon 2000 ESA program that could be a piggy back of a planetary mission.