共查询到18条相似文献,搜索用时 55 毫秒
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为了满足现有时频系统对分配放大器的要求,设计了一种小型频标分配放大器。该小型放大器带宽范围1MHz~100MHz,有1个输入,4个输出,采用一种电流反馈型、超宽带集成运算放大芯片CLC449。测试结果表明:二次谐波<-50dBc;路间隔离度为92.5dB;反向隔离度为105dB;相位噪声从100Hz开始趋于平稳,约-155dBc,满足时频系统的要求。最后提出了一些改进建议。 相似文献
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3MHz区分放大器有天,VLBI接收机,国防科研中有广泛的应用,研制成功的5MHz区分放大器在相位噪声和隔离度上分达到了频期效果,相位噪声的插入损耗小于3dB,隔离度大于60dB,并且保持了氢频标信号的稳定度,还可用于长线传输,因此比较好的满足了时频系统,特别是主稳定本振系统的使用要求,而且有着良好的应用前景。 相似文献
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本文介绍CSAO203型高精度脉冲隔离放大器的设计出发点、工作原理、设计特点和主要性能指标。 相似文献
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本文指出了太阳射电快速记录系统中方波隔离放大器研制的必要性,并简要介绍了设计出发点,工作原理,设计特点及主要技术指标的测试 相似文献
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本文指出了太阳射电快速记录系统中方波隔离放大器研制的必要性,并简要介绍了设计出发点,工作原理,设计和主主要技术指标的测试。 相似文献
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钟信号分配放大器的主要用途是把原子钟的10MHz、5MHz、1MHz和1pps信号以高质量的缓冲分别以多路形式不失真地馈送给用户,其目的是:第一,隔离负载对原子钟的影响:第二,在同一原子钟情况下,能向负载提供5路与钟一样的信号。它是高精密时 相似文献
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本文介绍了夜间天空亮度及其测量方法,同时介绍了作者研制的一种便携式亮度计。该亮度计的主要性能为:精确度:±5.4%,相当于±0.06mag;分辨率:10-6cd/m2,相当于27.4mag/□″;重量:3.5kg。 相似文献
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A new optical speckle interferometer for use at the 2.34 meter Vainu Bappu Telescope (VBT), at Vainu Bappu Observatory (VBO), Kavalur, India, has been designed and developed. Provisions have been made for observation both at the prime focus (f/3,25), as well as at the Cassegrain focus (f/13) of the said telescope. The technical details of this sensitive instrument and the design features are described. An interface between the telescope and the afore-mentioned interferometer is made based on a concept of eliminating the formation of eddies due to the hot air entrapment. The performances of this instrument has been tested both at the laboratory, as well as at the Cassegrain end of the telescope. It is being used routinely to observe the speckle-grams of close-binary (separation < 1 arc second) stars. The size of the Fried's parameter, ro, is also measured. 相似文献
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Allan H. Marcus 《Earth, Moon, and Planets》1970,1(3):297-337
We derive the distribution and covariance function of elevations on a cratered planetary surface from a representation of the surface as the moving average of a random point process. It is assumed that an initially plane surface is excavated by primary impact craters with an inverse-power law size distribution. Crater rim height and rim-to-floor depth are assumed to be power functions of crater diameter. Crater shapes studied include rimless cylinders and paraboloidal bowls, and paraboloidal bowls with power-law external rims and ejecta blanket. The inverse-power law diameter distribution induces a positively skewed stable law elevation distribution, with heavy inverse-power law tails whose exponent (for small craters) is two smaller than the crater diameter distribution exponent. The covariance function (equivalently, power spectral density) is shown to be a power-law at moderate distances, whose exponent also depends on the parameters of the cratering process. Observations of lunar elevations and elevation spectral densities on a meter scale agree well with theory.This work summarizes and extends Bellcomm Technical Reports TR-68-340-3, 4, 5, which were supported by the National Aeronautics and Space Administration, Contract NASw-417.Now at Johns Hopkins University, Baltimore, Md. 相似文献