Distributed optical passive star couplers

A technique is presented by which a single centralized passive star coupler in an optical star network is replaced by a distributed one. This is done by partitioning the star coupler into numerous pieces and placing them at the network nodes. Such a placement results in a great saving in the number of fibers required to build the star network. In addition to this saving, the problems associated with constructing a large single N*N star coupler are bypassed.<>     

Reflective single-mode fiber-optic passive star couplers

Architecture arrangements for constructing reflective single-mode fiber-optic passive star couplers for high-speed optical local-area networks using simple components, e.g. 3-dB couplers and mirrors, are presented. Besides the savings of fibers, the number of components needed to construct a reflective star is shown to be half of that needed for an equivalent transmissive star. To avoid unpredictable interference effects, only structures that are free of multipaths are considered     

Amplified distributed reflective optical star couplers

A practical configuration for an amplified distributed reflective N-star coupler using 2×2 3-dB fiber couplers and minimum numbers of erbium-doped fibers, pump lasers, and standard fibers is presented. The constitution and characteristics of this coupler are investigated. Besides a tremendous amount of saving of the required standard fibers, this distributed coupler is more efficient, more reliable, more flexible for future expansion, and more cost-effective for application in optical networks     

Amplified integrated star couplers with zero loss

It is shown that it is possible to compensate for the approximately 17 dB splitting and excess loss of a 19*19 integrated star coupler with erbium-doped fibers (EDFs) connected to the output channels. The amplifier fibers are pumped to near-quantum-limited noise performance using only one laser source at 0.98 mu m, which is connected to one of the input ports and is distributed to the EDFs through the star itself. The integrated star coupler's near-wavelength-independent performance is able to transmit both the pump light at 0.98 mu m and the signal at 1.55 mu m with a loss differential on the order of only 1 dB.<>     

New reflective type star couplers for full duplex channels

A new reflective-type singlemode fibre-optic passive star coupler is described. For this new type of coupler, power entering any one of the ports is divided to all ports except the input port, and thus the optical signal is prevented from returning to its own source.<>     

Efficient N×N star couplers using Fourier optics

A technique for constructing an efficient N×N star coupler with large N at optical frequencies is described. The coupler is realized in free space using two arrays, each connected to N single-mode fibers. The highest efficiencies are obtained using a planar arrangement of two linear arrays separated by a dielectric slab serving as free-space region. The coupler is suitable for mass production in integrated form, with efficiencies exceeding 35%     

Bitaper star couplers with up to 100 fibre channels

Biconically tapered fibre-optic star couplers with up to 100 fibre channels are reported which have excess insertion losses as low as ?0.56 dB and normalised standard deviations of output poers as low as 4.4%     

Evaluation of star couplers for application to FOAM experiments

The light-splitting properties of several commercial 8 × 8 transmission- type fiber optic star couplers were investigated for use under abnormal launch conditions. A severe modal selection process was observed. The results of this selection process were first observed in the variation of the throughput for each output fiber depending upon the input fiber used. Subsequently the effect on the emitted radiative profile was measured under a variety of launch conditions. Modal selection was maximized when the launch into the coupler underfilled the input fibers of the coupler, and the effect was minimized when the input was overfilled.     

Broad-band high-silica optical waveguide star coupler withasymmetric directional couplers

A broadband optical waveguide star coupler with asymmetric directional couplers is proposed. A coupling or splitting ratio of the coupler is flattened with respect to wavelength by choosing appropriate values for Δβ and complete power transfer length. The wavelength characteristics of uniform and alternating Δ&thetas;b directional couplers are investigated, and their broadband operation is shown theoretically. To demonstrate the feasibility of the new proposal, 8×8 star couplers composed of such asymmetric directional couplers are fabricated by using high-silica waveguides on a silicon chip. A star coupler composed of asymmetric directional couplers exhibited 2-dB loss variation in the wavelength range of 1.3-1.55 μm, and this value was almost one fourth of that of a star coupler composed of symmetric directional couplers     

New design for low-loss star couplers and arrayed waveguide gratingdevices

We propose a new loss reduction method in star couplers employing UV-written tapers that replace the free propagation region in the conventional star couplers and apply them to an arrayed waveguide grating (AWG) device. The insertion loss of the new AWG device can be reduced to 0.31 dB, which is about 0.7 dB lower than that of the AWG without UV-written tapered waveguides     

Comparison of different polymeric multimode star couplers forbackplane optical interconnect

This paper describes a comparison of three types of 8×8 multimode star couplers made in polymeric multimode waveguides. Their geometry was designed with a ray tracing tool, measurements show low loss for all designs, but a symmetrical design, based on a tree of Y-junctions yields the best uniformity     

An N*N optical multiplexer using a planar arrangement of two star couplers

The author describes the design of an integrated N*N multiplexer capable of simultaneously multiplexing and demultiplexing a large number (up to about 50) of input and output wavelength channels. The multiplexer is a generalization of the 2*2 Mach-Zehnder multiplexer. It consists of two N*M star couplers connected by M paths of unequal length. Aberrations caused by mutual coupling in the waveguide arrays are minimized by a correction scheme that causes each star coupler to accurately perform a Fourier transformation. The multiplexer should be useful as a wavelength routing device for long haul and local area networks.<>     

Wavelength accuracy and output power of multiwavelength DFB laser arrays with integrated star couplers and optical amplifiers

In this letter, we report the static performance of multiwavelength DFB laser arrays with integrated star couplers and optical amplifiers built for the reconfigurable optical network testbed. By the use of wavelength redundancy and proximity effect, wavelength deviations of /spl plusmn/0.2 nm or less from the designated eight-wavelength comb have been achieved with high yield. Simultaneous operation of eight wavelengths has also been demonstrated. In spite of the inherent splitting loss of 13 dB, high output powers of about -13 dBm and 0 dBm per wavelength have been measured into a single-mode fiber without and with on-chip optical amplification, respectively.     

Modeling of Ti:LiNbO3 waveguide directional couplers

A simple and accurate method is presented for studying the coupling characteristics of 3D diffused channel waveguide directional couplers. The method is based on the scalar variational principle and differs from other methods as it does not require any assumption for the functional form of the trial field. The authors also propose an equivalent 2D directional coupler that also gives accurate results and, hence, saves considerable computational time, Comparison with experimental and other theoretical results is also presented     

全天时星敏感器的建模分析与实验验证

全天时星敏感器技术可以将星敏感器的应用推广到临近空间飞行器如平流层飞艇和高空气球等平台,是星敏感器未来发展的一个重要方向。由于白天受到强烈的大气背景辐射的影响,可见光波段星敏感器的探测能力显著受限。大气背景辐射在短波红外处的强度迅速降低,因此利用短波红外成像系统在0.9~1.7m波段下进行恒星探测成为研究全天时星敏感器技术的一种有效可行的方案。为了系统地分析并验证短波红外全天时星敏感器的可行性,文中在分析全天时星敏感器探测模型的基础上,重点讨论了短波红外探测器噪声对星敏感器探测能力的影响并基于探测模型确定了20 km高度处全天时星敏感器的光学参数。基于短波红外探测器研制了全天时星敏感器原理样机,结合地面处的观星实验,测试了原理样机的探测性能并验证了全天时星敏感器探测模型的正确性。     

多视场星敏感器数学模型与精度分析

多视场星敏感器与传统单视场星敏感器相比不仅具有更高的可靠性和自主性,也具有更高的精度和动态性能,是未来星敏感器发展的重要趋势之一.为获得最佳性能,需要对多视场星敏感器的视场大小和布局进行优化.为此,首先建立了多视场星敏感器的数学模型,重点介绍了星点成像和姿态计算.然后推导了多视场星敏感器测量精度的数学表示,分析了影响精度的因素.通过仿真分析了多视场星敏感器视场大小和布局对各因素和精度的影响.仿真结果表明,视场大小对星敏感器精度的影响取决于星敏感器的运动情况,当角速度较小时,视场越小,精度越高;当角速度较大时,视场越大,精度越高.而各视轴相互正交的视场布局下,多视场星敏感器的测量精度最高.     

Small-hole couplers

A proof is provided of the fact that the formulas for the coupling due to a small hole, obtained by Bethe, correctly apply even to structures which do not exhibit the symmetry, in the plane of the hole, postulated by Bathe.     

Wavelength-flattened fused couplers

A technique is reported for the fabrication of fused couplers, which yields devices having splitting ratios substantially independent of wavelength. A low-loss, stable, single-mode 2×2 port coupler has been fabricated using this technique. The coupler has 50/50% coupling at both 1.3 and 1.52 ?m and 50% ± 9% coupling over the wavelength range 1.23 to 1.57 ?m.     

船用星敏感器姿态测量误差建模与仿真分析

为提高船用星敏感器姿态测量精度,对星敏感器船体姿态测量误差模型进行了理论分析。首先针对船用星敏感器的使用环境构建了船用星敏感器观测模型,然后推导了基于角度测量的船用星敏感器误差模型,最后仿真分析了星敏感器地平滚动角测量误差、安装角度对船体姿态测量精度的影响。误差模型与仿真结果表明,星敏感器地平姿态测量误差、安装角度标定误差以及安装布局等是影响船体姿态测量精度的主要因素,其中当星敏感器地平滚动角测量误差为100″时,船体姿态测量误差最大可达112″;安装布局对船体姿态测量精度有一定的影响,其中船体姿态测量误差随安装方位角的变化而呈周期性振荡趋势,纵摇测量误差随安装仰角的增加而增大;当星敏感器沿艏艉线方向安装时,航向测量误差随安装仰角的增加而增大,当沿垂直于艏艉线方向布局时,横摇测量误差随安装仰角的增加而增大。     

Asymmetric multimode couplers

An asymmetric multimode coupler consists of two dissimilar multimode fibers. A simple theoretical analysis of asymmetric multimode couplers that will enable couplers to be designed with specific performance parameters is presented. The theoretical predictions are compared with the measured behavior of specially fabricated couplers. A novel technique to determine the performance of a linear bus of identical asymmetric couplers from measurements on a single coupler is introduced