Temperature measurements using fiber optic polarization interferometer

A novel measurement method of temperature based on the phenomena that the phase difference between principle polarization states in the optical retarder is function of temperature is described. The polarization state of optical beam is changed as it passes through the optical retarder, which depends on the temperature. The temperature of optical retarder is determined by comparison of the power difference between principal polarization states. We demonstrate successfully the temperature measurement by using a polarization maintaining fiber as the optical retarder. With a 100 mm length of the fiber optic retarder, the change rate of phase difference on temperature was 0.236 rad/°C and the measurement error was ±0.038°C over the temperature range of −2.6 – +3.4°C. With a 11.5 mm length of the fiber optic retarder, the change rate of phase difference on temperature was 0.021 rad/°C and the measurement error was ±0.79°C over the temperature range of −8.5 – +86.5°C.     

Volumetric, ultrasonic and viscometric studies of binary mixtures of dimethyl sulphoxide with chloro and nitro substituted aromatic hydrocarbons at T = 303.15 K

Excess volumes (V^E) ultrasonic sound velocities (u), isentropic compressibilities (K_s) and viscosities (η) have been measured for the binary mixtures of dimethylsulphoxide (DMSO) with 1,2-dichlorobenzene, 1,3-dichlorobenzene, 1,2,4-trichlorobenzene, o-chlorotoluene, m-chlorotoluene, p-chlorotoluene, o-nitrotoluene and m-nitrotoluene at T = 303.15 K. The measured V^E values were positive over the entire composition range in all the binary mixtures. Isentropic compressibilities (K_s) have been computed for the same systems from precise sound velocity and density data. Further, deviation in isentropic compressibility (ΔK_s) from ideal behaviour was also calculated. The viscosity data are analysed on the basis of corresponding states approach. Deviation in viscosities are positive over the entire composition range. The measured data is explained on the basis of intermolecular interactions between unlike molecules.     

微加工薄膜变形镜特性分析

 借助测量微加工薄膜变形镜驱动器的面形影响函数,分析了驱动器的电压-位移函数和驱动器之间的线性叠加性;通过对连续面形变形镜拟合像差的理论分析和实验研究,建立了微加工薄膜变形镜电压解耦模型。分析了对前36阶Zernike模式的拟合残差和拟合能力,指出微加工薄膜变形镜仅可用来拟合低级像差并且有较大的拟合能力和较小的拟合残差,而不能拟合高级像差。     

Refractometer based on a tapered Mach–Zehnder interferometer with Peanut-Shape structure

A novel refractometer based on tapered Mach–Zehnder modal interferometer (MZI) is proposed and experimentally demonstrated. This sensor is composed of a pair of Peanut-Shape structures and an embedded taper – the former excites high-order cladding modes, while the latter enhances the evanescent field. As the effective refractive index (RI) of cladding is based on the changes of surrounding RI, thus extinction ratio will change due to the alteration of the distribution of power in the fiber which is induced by various differences of core and cladding for RI. As a result, the maximum RI sensitivity of 240.78 extinction ratio/RIU (refractive index unit) is achieved within the range from 1.3334 to 1.4081.     

Sagnac棱镜角公差与干涉光谱仪光谱分辨率的关系分析

根据干涉成像光谱仪光谱分辨率对角向差的要求,通过对实体Sagnac干涉仪结构和光路进行分析,从三个相互垂直的方向出发,研究了光谱分辨率和棱镜角公差之间存在的关系;并推导了满足光谱仪光谱分辨率要求的实体Sagnac干涉棱镜的角公差公式;用实例说明了关系式的应用方法,如果不考虑棱镜变形引起的色散及棱镜的面型误差和付氏镜的残余像差的影响,而只考虑棱镜的角误差对光谱分辨率的影响,则通常情况下干涉棱镜的角公差要求较严,约20″以内.     

Modeling of the Temporally and Spatially Modulated Fourier Transform Imaging Spectrometer working in orbit

Temporally and Spatially Modulated Fourier Transform Imaging Spectrometer (TSMFTIS) is a new kind of imaging spectrometer and is applicable in remote sensing. Compared with Temporally Modulated Imaging Interferometer and Spatially Modulated Imaging Interferometer, it employs immovable parts and abandons slit. Based on the analysis of its physical theory, optical principle, data gathering and processing, the mathematical model of the TSMFTIS working in orbit is proposed in this paper. The model is comprised of different function blocks, such as fore-optics, interferometer and so on. For simulation, a big remote sensing image is utilized as ground scene, and a conversion which is similar to color mode conversion from RGB to Lab is made to produce artificial spectra of various ground objects. At last, a validation experiment is performed with real-world spectra of four pieces of colorful cloths by using a commercially available spectrometer.     

利用等厚干涉条纹测量微光的调制传递函数MTF

通过对微光的调制传递函数 (MTF)的讨论 ,结合传统的“分辨率板法” ,提出了一种新的测量微光的MTF的方法。该方法直接从MTF的物理含义出发 ,利用迈克尔逊干涉仪产生一系列空间频率的等厚干涉条纹来模拟分辨率板的作用 ,在计算机的控制下 ,自动测量出连续的MTF曲线。给出的实验光路和实验结果表明 ,利用干涉条纹测量微光的MTF是一种可行的简便方法 ,在计算机的控制下 ,可快速完成夜视仪的传递函数测量     

干涉仪的微应力安装力学分析以及试验结果

干涉仪在系统中固定产生的应力会影响干涉条纹的调制度.将干涉仪的非通光面与干涉仪材料性能相同的玻璃平板胶合,做为干涉仪上下面的安装面,可以消除安装过程中对干涉仪产生的应力.选取航天通用的铸钛材料做为支撑件,可以避免恶劣航天环境中金属件热膨胀对干涉仪的破坏,采用XM31胶垫对干涉仪运输过程进行保护.整个装调中采用微应力装调.对整个系统采用工程分析软件进行了理论力学分析.结果表明,这种结构设计是可行的.同时采用2XSA60-T1000-32WL振动台,根据有关规范要求输入振动载荷,进行了力学环境试验.试验前后整个系统干涉图的MTF值基本不变.证明这种干涉仪结构设计以及微应力装调方法在工程应用上是可行的.     

Investigation of data format conversions based on MZI-SOA

Employing a Mach-Zehnder Interferometer (MZI), this paper describes simulation demonstration of an all-optical scheme for data format conversion between non-return-to-zero (NRZ) and return-to-zero (RZ). Data format conversion between NRZ and RZ at 120 Gb/s has been simulated for the first time using an MZI. In addition, we have proposed for the first time data format conversion from NRZ to RZ by using a single SOA in an MZI.     

Long baseline gravitational wave detectors—Status and developments

Gravitational waves-a prediction of Einstein’s General Relativity-are among the most elusive signals incident on the Earth. These signals-ripples in the curvature of space-time-carry information about what is happening deep in the heart of some of the most violent events in the Universe. However, their observation remains one of the most challenging problems in experimental astrophysics, as the measurement sensitivity required by the detectors is equivalent to measuring a change in the separation of the Earth and Sun by the diameter of an atom. A global network of such detectors-LIGO, Virgo and GEO-is now in operation, with enhanced versions being developed and other detectors planned. Further a space-borne detector, LISA, is under development as a joint ESA/NASA mission. In this short review, the nature of gravitational waves, how the detectors work, and the preliminary results which are already showing promise, will be discussed.