镀膜光纤声相位调制器的研究

本文主要讨论氧化锌镀膜光纤光相位调制器。首先介绍了氧化锌镀膜光纤的几何结构,然后分析了此几何结构压电声光振荡的基本原理并推出了氧化锌镀膜光纤声光相位调制器Ｔ型网络的等效电路模型,最后给出了氧化锌镀膜光纤声光相位调制器的实验测试装置及基本工程原理。     

火箭喷管极性自动化测试系统的改进设计研究

使用计算机视觉方法进行的发动机极性自动化测试是火箭地面测试中重要的测试环节,该环节存在进一步改进和提升的空间。将递归全对场变换(Recurrent All-pairs Field Transforms, RAFT)光流算法替代传统光流法检测技术用于发动机喷管实时运动监测,并根据现场测试场景对光流算法进行了优化,提升了运动检测速度与测量精确度,使自动测试系统具备了摆角的估测能力;在软件系统设计层面,引入差异图像直方图法监听法辅助喷管动作识别,避免了光流法对于未处在监测流程中的摄像头的冗余监听资源消耗,降低了系统硬件设备的负载,同时实现了一种可视化在线判读软件的设计。提出的软件与算法方面的改进在当前已投入使用的极性自动化测试系统上实现了进一步的优化。     

多光谱扫描仪的杂光计算

本文采用蒙特卡洛法计算太阳光进入星载光学系统的杂光数量级。并对一具体结构的多光谱扫描仪进行了计算，以确定其消杂光能力。对某些参数的变动也进行了计算，为设计和修改提供了依据     

光纤外差干涉位移传感器

非接触式光纤外差干涉位移传感器是将半导体激光器线性调频技术和光纤传感技术相结合制成的1种新型外差干涉仪。它的位移测量范围可达26mm，分辨率为0．02μm；对不同材料、不同粗糙度的对象面，有着几乎相同的测量灵敏度和测量精度；探头和对象面无需严格垂直。     

SiC光学反射镜发展现状

主要综述SiC作为光学反射镜材料在设计、制造、光学加工和应用方面的发展现状，同时对今后SiC作为光学镜片材料的发展趋势进行了展望。     

齿轮接触斑点测量仪光学机械系统的设计分析

介绍１种新近开发的齿轮接触测量仪，该仪器利用先进的ＣＣＤ光电接收器件作测量传感器，并利用ＩＢＭＰＣ／ＸＴ计算机作数据和图象处理，使齿轮接触斑点的测量从测量精度和效率方面都比传统的目视观察，手工描绘提高一大步，本文着重讨论仪器光学机械系统的原理结构。     

一种光纤快速测温系统研究

介绍了一种比色光纤快速测温系统。该系统适合于一些特殊环境下的测温要求，解决了传统测温方法无法测量的问题。它可以用于脉冲爆震发动机温度测量，也可以用于铸造，铸造，高频加热以及陶瓷烧结等测量。     

The optical to X-ray spectrum of the broad-line ultrasoft AGN RE J2248-511

We present a series of monitoring observations of the ultrasoft broad-line Seyfert galaxy RE J2248-511 with XMM-Newton. Previous X-ray observations showed a transition from a very soft state to a harder state five years later. We find that the ultrasoft X-ray excess has re-emerged, yet there is no change in the hard power-law. Reflection models with a reflection fraction of 15, and Comptonisation models with two components of different temperatures and optical depths (kT₁ = 83 keV, T₁ = 30 eV, τ₁ = 0.8; KT₂ = 3.5 keV, T₂ = 60 eV, τ₂ = 2.8) can be fit to the spectrum, but cannot be constrained. The best representation of the spectrum is a model consisting of two blackbodies (kT₁ = 0.09 ± 0.01 keV, kT₂ = 0.21 ± 0.03 keV) plus a power-law (Γ = 1.8 ± 0.08). We also present simultaneous optical and infrared data showing that the optical spectral slope also changes dramatically on timescales of years. If the optical to X-ray flux comes primarily from a Comptonised accretion disk we obtain estimates for the black hole mass , accretion rate and inclination cos(i)  0.8 of the disk.     

Geosynchronous satellites expanding a future GNSS satellite constellation: A precise orbit determination study

The integration of geosynchronous orbit (GSO) satellites in Global Navigation Satellite Systems (GNSS) is mostly discussed to enable a regional enhancement for tracking. But how do GSO satellites affect the orbit determination of the rest of the constellation? How accurately can these orbits be determined in a future GNSS tracking scenario with optical links? In this simulation study we analyze the benefit of GSO satellites as an expansion of a MEO (Medium Earth Orbit) satellite constellation – we selected the Galileo satellite constellation – for MEO Precise Orbit Determination (POD). We address not only the impact on POD of MEO satellites but also the possibility to precisely determine the GSO satellites – geostationary orbits (GEO) and inclined geosynchronous orbits (IGSO) – in such an expanded MEO constellation. In addition to GNSS microwave observations, we analyze the influence of different optical links between the participating entities: Optical two-way Inter-Satellite Links (OISL) and ground-space oriented Optical Two-Way Links (OTWL). These optical measurements together with the GNSS microwave observations give a remarkable benefit for the POD capability. In the case of GNSS and OTWL, we simulate the measurements with regard to a network of 16 ground stations. We pay great attention to the simulation of systematic effects of all measurement techniques. We discuss the influence on the systematic errors as well as the formal orbit uncertainties. A MEO constellation expanded with GSO satellites as well as the use of optical links together with GNSS observations not only improves the MEO satellite orbits but also the GSOs to a great extent.     

The Swift Ultra-Violet/Optical Telescope

The Ultra-Violet/Optical Telescope (UVOT) is one of three instruments flying aboard the Swift Gamma-ray Observatory. It is designed to capture the early (∼1 min) UV and optical photons from the afterglow of gamma-ray bursts in the 170–600 nm band as well as long term observations of these afterglows. This is accomplished through the use of UV and optical broadband filters and grisms. The UVOT has a modified Ritchey–Chrétien design with micro-channel plate intensified charged-coupled device detectors that record the arrival time of individual photons and provide sub-arcsecond positioning of sources. We discuss some of the science to be pursued by the UVOT and the overall design of the instrument.