光纤功率计非线性因子测量的优化设计研究

对光纤功率计非线性因子测量系统进行了优化设计。在理论分析和实验验证的基础上,优化了光路系统,抑制了光的干涉效应对光功率稳定性的影响,进行了实验验证;由光衰减器代替快门进行光的通断控制,扩展了测量范围,可以实现通用光纤功率计非线性因子的全量程测量。     

Errors in the remotely sensed ocean reflectance

An approximate method has been described to determine optical properties of the ocean surface from the reflected short-wave radiance at the top of the atmosphere. The non-scattered and singly scattered components of the radiation field have been taken into account exactly, the multiply scattered components - approximately. The calculations for a real atmospheric model have been compared with the results of an exact method for solving the radiation transfer equation.On the basis of the elaborated algorithm the sensitivity of the value of the remotely sensed spectral albedo of the ocean to the variations in optical thickness, single scattering albedo and aerosol phase function has been described as well as the influence of vertical inhomogeneity of the atmosphere.     

Optical and X-ray observations of 4U2129+47/V1727 CYG in a quiescent state

We observed the 5.2 h X-ray binary 4U2129+47 for more than one orbital cycle on 29 September and 4 October 1983 using the LE, ME and GSPC detectors of the ESA X-ray satellite EXOSAT. In neither detector an X-ray flux from the source could be detected. Quasi-simultaneous UBV observations using the 2.2 m telescop at the German-Spanish Astronomical Center, Calar Alto, failed to detect the large amplitude light curve reported in earlier observations but show the optical companion in a low intensity state. The large amplitude light curve has been interpreted as due to X-ray heating of the optical star by the X-ray source similar to the system Her X-1/HZ Her. Our optical observations indicate that the heating X-ray source has been shut off and nicely explain that EXOSAT failed to detect the source. 4U2129+47 seems to behave similar to Her X-1 in the optical quiescent state, seen for instance from 1949 to 1956.     

Spectral and temporal characteristics of aerosol optical depth over a wet tropical location in North East India

A network of multi wavelength solar radiometer (MWR) stations has been in operation since the 1980s in India for measurement of aerosol optical depth (AOD). This network was augmented recently with the addition of a large number of stations located across the length and breath of India covering a variety of climate regimes. The spectral and temporal variations of aerosol optical depths observed over Dibrugarh located in the North East of India (27.3°N, 94.5°E) are investigated by analyzing the data obtained from a MWR during October 2001–September 2003 using the Langley technique. AOD varies with time of the day, month of the year and season. From January to April and October to December, aerosol optical depth decreases with wavelength whereas during May–September aerosol optical depth has been found to be nearly independent of wavelengths. AOD is higher during pre-monsoon season (March–May) and lower in the monsoon (June–September) season at about all wavelengths. The temporal variation of AOD over Dibrugarh have also been compared with those reported from selected locations in India.     

多层膜光学常数的迭代椭偏测量研究

论述了多层薄膜光学的椭偏测量原理以及测量方法，采用导纳矩阵计算多层的椭偏参数；采用统计试验法与单纯形法相结合的数值逼近法进行反演计算。更重要的是本文首次提出迭椭偏测量法，使测量的重复性和精确度都大大提高。所谓选代椭偏测量法是不断地优选椭偏测量入射角，从而选出对核样品来说最佳椭偏测量入射角。用这种方法精确测量了相变光盘记录介质膜晶态下的光学常数，这对于相变光盘膜系结构优化设计很重要。     

基于光外差法的宽带示波器滤波器频响测试技术研究CSCD

分析了光外差测试频响的原理,提出了采用光外差法测试宽带示波器滤波器频响的方案,分析了偏振态和波长稳定性对于测试结果的影响。实验结果表明,光外差法测试宽带示波器光电模块频响方案可行,9.953Gbps滤波器下测试,3d B带宽频率处频响重复性小于0.1d B。     

A concept mission for the Stellar Population and Evolution with Cubesats (SPEC)

Binary or multiple stellar systems, constituting almost a third of the content of the Milky Way, represent a high priority astronomical target due to their repercussions on the stellar dynamical and evolutionary parameters. Moreover the spectral study of such class of stars allows to better constrain the evolutionary theories of the Galactic stellar populations. By resolving the members of stellar systems through photometric observations we are able to perform more detailed measurements to infer their mass. In this paper we investigate the feasibility of a cubesat based mission including an optical payload to directly optically discriminate the members of a selected sample of binary systems. The scientific targets, consisting 11?M class dwarf stars binary systems, have been extracted from the already studied Riaz catalogue. These subset has been selected considering the star distance, the members angular separation, and the distance from the Galactic plane (due to limit the background and foreground contamination). The satellite concept is based on a 6 unit Cubesat embedding some commercial off the shelf components and an ad hoc designed optical payload occupying almost 4 units. The optical configuration has been chosen in order to fit the angular resolution requirements, as derived from the target characteristics. Moreover, according to the optical analysis and the computed field of view some requirements on the attitude control system have been inferred and fulfilled by the component selection. The paper is organized as in the following: a brief scientific introduction is made; consequently the project is described with particular attention to the optical design and the standard sub-systems; finally the conclusions are drawn and the future perspectives are investigated.     

太阳吸收率计算公式的截断误差

详细地分析了工程上应用的太阳吸收率计算公式的截断误差;从数学上推导了截断误差的计算公式;并给出了计算实例。所得结果对卫星热控材料及太阳光谱利用涂层材料的光热学性能的测量具有一定的参考价值。     

铷吸收半导体激光稳频光波长标准研究

介绍了用铷吸收光谱法对半导体激光器进行稳频,通过对包括半导体激光驱动源、稳频器、吸收室、光路等系统的优化设计,达到具有高信噪比微分误差信号,从而大大提高了半导体激光器稳频锁定灵敏度和长期稳定性。采用文中介绍的方法建立的光波长标准系统,其波长的测量重复性、稳定性可满足当前和将来很长一段时间光波长计校准的需要。     

红外动态目标模拟器光学系统的设计

设计了一种用于红外导引头性能测试的红外动态目标模拟器,利用数字微镜阵列(DMD)对黑体红外辐射进行反射调制,并由光学准直系统实现红外场景生成系统与红外导引头的光学耦合。用光学设计软件（ZEMAX）对准直光学系统进行了设计和优化,准直光学系统成像质量良好,接近衍射极限,点列图直径小于艾里斑直径,畸变小于0.1%。结果表明该系统环境适应性强,能很好地用于红外导引头动态图像的校准。     

汽车模拟覆盖件的相位法测量

简述了相位法曲面全场无接触三维测量的基本原理，针对为汽车车顶抗凹性能研究而制作的模拟覆盖件的外形测量要求，设计了相位法三维测量的光学成象系统与图象处理系统，并应用到汽车模拟覆盖件的外形测量，测量结果与三坐标所测结果相近，说明了该测量系统的精确性。     

卫星光轴复合指向控制方法研究

卫星平台搭载光学载荷对空间运动目标进行跟踪指向技术已经成为卫星发展的重点,为了提升卫星光轴的指向范围、跟踪精度和机动性,仅依靠卫星的姿态调整已无法提升卫星光轴的性能.通过对由卫星姿态、星载光电转台和快反镜组成的卫星复合光轴指向系统的分析,需三者协同工作,输出有效叠加,才能有效提升卫星光轴的指向范围、跟踪精度和机动性.对...     

New progress on space solar telescope

The design of the Space Solar Telescope (phase B) has been completed. The telescope system has been manufactured (phase C) since the beginning of 1999, and it will be assembled by the end of 2000. In this paper, mainly the optical design, technique and manufacture will be described. The launch is planned for the summer of 2004.     

A comparison of atmospheric aerosol measurements by various satellite sensors

Investigations to measure the vertical optical thickness of aerosols over ocean surfaces has been conducted using several different satellite sensors. Landsat 1 and Landsat 2 data originally confirmed that a linear relationship exists between the upwelling visible radiance and the aerosol optical thickness (about 90% of this thickness is generally in the lowest 3 km of the atmosphere). Similar relationships have also been found for sensors on GOES-1, SMS-2, NOAA-5, and NOAA-6 satellites. The linear relationship has been shown theoretically to vary with the aerosol properties, such as size distribution and refractive index, although the Landsat data obtained at San Diego showed little variability in the relationship. The differences between the results found for the various satellite sensors are discussed, and are attributed mainly to uncertainties in the calibration of the sensors. To investigate the general applicability of the technique to different locations, a global-scale ground truth experiment was conducted with the AVHRR sensor on NOAA-6 to determine the relationship at eleven ocean sites around the globe. Analysis of the data shows good agreement between the satellite and ground truth values of the aerosol optical thickness, and indicates that the technique has global application. At two of the sites, multispectral radiometric measurements of the Junge aerosol size distribution parameter were made, and showed good agreement with a value inferred from the AVHRR Channels 1 and 2 radiances.     

大型天文望远镜研究

提出新建一台4.3m 光学红外新技术望远镜,并与北京天文台2.16m 望远镜用真空管道联机作CCD 照相和光干涉测量,提高集光能力达4.8m 口径,分辨率达10m 口径。     

Optical oxygen sensor instrumentation based on the detection of luminescence lifetime.

Optical oxygen sensors are mainly based on the principle of luminescence quenching. In contrast to arready existing intensity-based systems, the measurement of the luminescence lifetime provides certain advantages, such as insensitivity to photobleaching or leaching of the dye, or changes in the intensity of excitation light. This facilitates the use of simple optical systems or optical fibres. A new family of oxygen-sensitive dyes, the porphyrin-ketones, has been introduced, which exhibits favorable spectral properties and decay times in the order of tens and hundreds of microseconds. This allows the use of simple optoelectronic circuitry and low-cost processing electronics. An optical oxygen sensor module has been developed with the dimensions of only 120 x 60 x 30 mm. The prototype is based on the measurement of the decay time of the luminophore by measuring the phase shift between the square-wave excitation and the detected square-wave of the emission coming from the sensor. The instrument is based on semiconductor devices (light-emitting diodes, photodiodes) and may be used for the detection of oxygen in gaseous or liquid samples. The measurement range of the device is from 0 to 200 hPa oxygen partial pressure with a resolution of < 1 hPa over the whole measurement range. The overall measurement accuracy of < +/- 1 hPa has been obtained for periods of 24 h of continuous measurement in a thermostatted environment. The sensor response times t90 are typically < 1 s for gases and 0.5 to 5 min for liquid samples.     

Possible radio JETS in GX 1+4

GX 1+4 is an X-ray pulsar with a nominal period of 2 or 4 min. and has the highest of 0.22 yr⁻¹ among the X-ray pulsars. The source is identified with an optical counterpart V2116 Oph, however no binary period has been reported so far. There are several features of the source like , variable pulse shape, period history and the spectral changes which do not fit well with our present understanding of the source.

The radio observation of the galactic center region were made using Molonglo observatory Synthesis Telescope operating at a frequency of 843 MHz. A 12 hr observation was made with the field center at the position coordinates of the optical counterpart. No significant radio emission was seen corresponding to the center position.

The synthesis map however, showed the presence of two regions of radio enhancements almost equidistant from the optical source in the diametrically opposite directions/1/. The data is interpreted as due to synchrotron emission produced by the expanding jets of GX 1+4, similar to the radio jets observed in galaxies. Radio jets have been inferred for three galactic X-ray binary sources namely, Sco X-1, Cyg X-3, and SS 433. However, for all these sources no X-ray pulsation has been detected so far. The present observations if confirmed will be the first case of radio jets in a stellar system containing an X-ray pulsar.     

光学捷联基准导航计算机设计与实现

为满足当前光学捷联基准解算精度高、低功耗、小型化的需求,设计了一种基于现场可编程门阵列（FPGA）和数字信号处理器（DSP）为核心的嵌入式导航计算机。对导航计算机（ENC）硬件设计进行了阐述,并重点研究了导航计算机信息处理模块（MPM）和数据采集通信模块（DCM）的协同使用,充分体现了DSP和FPGA联合使用的优点。其次,研究了基于主惯导航向和计程仪速度组合的Kalman滤波器设计,以解决长时间工作对系统精度的影响。最后,将该导航计算机实际应用于捷联基准中,通过半实物仿真试验,验证了导航计算机硬件方案的可行性和Kalman滤波器设计的合理性。结果表明,基于FPGA和DSP双核的嵌入式导航计算机性能稳定,设计合理,满足光学捷联基准高精度、低功耗的使用要求。     

一种TeGe基快速相变型可逆光记录介质的研究

研制出一种在晶化激光功率为4mW时晶化时间为180ns的可逆相变型光纪录介质。其擦写循环次数可达10~6次。分析了其快速晶化机理。     

The space telescope program

The 2.4-m Space Telescope is well into its development phase and is planned for launch in early 1985. The major components of the optical telescope portion are completed and the supporting systems are being designed and acquired. The five scientific instruments, including the ESA provided Faint Object Camera, are on schedule for delivery by the summer of 1983. After successful completion of the optical components, the greatest design challenge has been the pointing and control system. The original design goals of near diffraction limited performance in the visible and near ultraviolet remain as do the other goals of versatility and long life.