Solar X-ray Monitor (XSM) on-board Chandrayaan-2 orbiter

The remote X-ray fluorescence spectroscopy is a powerful technique to investigate the elemental abundances in the atmosphere-less planetary bodies. The experiment involves measuring spectra of fluorescent X-rays from lunar surface using a low energy X-ray detector onboard an orbiting satellite. Since the flux of fluorescent X-ray lines critically depend on the flux and spectrum of the incident solar X-rays, it is essential to have simultaneous and accurate measurement of X-ray from both Moon and Sun. In the context of Moon, this technique has been employed since early days of space exploration to determine elemental composition of lunar surface. However, so far it has not been possible to exploit it to its full potential due to various reasons. Therefore it is planned to continue the remote X-ray fluorescence spectroscopy experiment on-board Chandrayaan-2 which includes both lunar X-ray observations and solar X-ray observations as two separate payloads. The lunar X-ray observations will be carried out by Chandra Large Area Soft x-ray Spectrometer (CLASS) experiment; whereas the solar X-ray observations will be carried out by a separate payload, Solar X-ray Monitor (XSM). Here we present the overall design of the XSM instrument, the present development status as well as preliminary results of the laboratory model testing. XSM instrument will have two packages namely – XSM sensor package and XSM electronics package. XSM will accurately measure spectrum of Solar X-rays in the energy range of 1–15 keV with energy resolution ∼200 eV @ 5.9 keV. This will be achieved by using state-of-the-art Silicon Drift Detector (SDD), which has a unique capability of maintaining high energy resolution at very high incident count rate expected from Solar X-rays. XSM onboard Chandrayaan-2 will be the first experiment to use such detector for Solar X-ray monitoring.     

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...     

基于红外技术的发动机低压涡轮叶片温度场测量

为了解某型发动机整机运行状态下低压涡轮工作叶片的温度分布情况,使用红外测试系统测量了该发动机整机状态低压涡轮工作叶片前缘及盆侧的温度场。试验前对该发动机进行了测试改装,设计了用于实现叶片定位的转速信号分析仪,以及用于提供高压气源的气体增压系统。试验共测得多个状态下发动机涡轮叶片的表面温度分布数据。结果表明:涡轮叶片前缘和叶盆中间位置的温度较高;相同位置下每片叶片的温度有轻微差异;叶片的最高温度位置位于测试区域的下方,与仿真计算结果相吻合。采用红外测温技术可以得到清晰的涡轮叶片表面温度分布云图,结合示温漆标记技术,可用于定位温度最高的叶片和叶片温度最高的位置。     

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。     

An Overview of the Instrument Suite for the Deep Impact Mission

A suite of three optical instruments has been developed to observe Comet 9P/Tempel 1, the impact of a dedicated impactor spacecraft, and the resulting crater formation for the Deep Impact mission. The high-resolution instrument (HRI) consists of an f/35 telescope with 10.5 m focal length, and a combined filtered CCD camera and IR spectrometer. The medium-resolution instrument (MRI) consists of an f/17.5 telescope with a 2.1 m focal length feeding a filtered CCD camera. The HRI and MRI are mounted on an instrument platform on the flyby spacecraft, along with the spacecraft star trackers and inertial reference unit. The third instrument is a simple unfiltered CCD camera with the same telescope as MRI, mounted within the impactor spacecraft. All three instruments use a Fairchild split-frame-transfer CCD with 1,024× 1,024 active pixels. The IR spectrometer is a two-prism (CaF₂ and ZnSe) imaging spectrometer imaged on a Rockwell HAWAII-1R HgCdTe MWIR array. The CCDs and IR FPA are read out and digitized to 14 bits by a set of dedicated instrument electronics, one set per instrument. Each electronics box is controlled by a radiation-hard TSC695F microprocessor. Software running on the microprocessor executes imaging commands from a sequence engine on the spacecraft. Commands and telemetry are transmitted via a MIL-STD-1553 interface, while image data are transmitted to the spacecraft via a low-voltage differential signaling (LVDS) interface standard. The instruments are used as the science instruments and are used for the optical navigation of both spacecraft. This paper presents an overview of the instrument suite designs, functionality, calibration and operational considerations.     

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。