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noise generator     
相关语句
  噪声发生器
     A Type RM-888 Pseudorandom Noise Generator
     RM—888型伪随机噪声发生器
短句来源
     Design of chaos noise generator based on MATLAB and LabVIEW
     基于Matlab和LabVIEW的混沌噪声发生器设计
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     The using of FPGA to realize the digital white noise generator with variable variance
     方差可调的数字式白噪声发生器的FPGA实现
短句来源
     Impulse Noise Generator
     脉冲噪声发生器
短句来源
     Virtual white noise generator based on Logist eqution and Labview
     基于Logist方程和Labview的虚拟白噪声发生器的设计
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  噪声源
     This paper introduces a comparison system of cold noise generator, mainly describes the operational principle, system design, basic method, error analysis of the system and the application examples.
     介绍冷噪声源比对系统的工作原理,系统设计和采用的主要技术,系统误差分析及应用实例。
短句来源
     Circuit design scheme of the high-speed digital physical noise generator was mainly discussed in this paper.
     本文讨论了高速数字物理噪声源的系统级设计方案。
短句来源
     With the development of computing technology and cryptography, high-speed digital physical noise generator is urgently required in cryptography at present.
     随着计算技术和密码学的发展,当今的安全信息系统迫切需要更高速率的数字物理噪声源
短句来源
     Measurement Method for Low Frequency Noise Generator
     低频噪声源的测试方法
短句来源
     According to the result of uncertainty analysis, we think that using spectrum analyzer to calibrate noise generator is practicable in certain conditions.
     根据分析结果,认为用频谱仪校准噪声源在一定条件下是可行的。
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  “noise generator”译为未确定词的双语例句
     Annex B to ITU-T recommendation G. 729 defines the Voice Activity Detection(VAD), Discontinuous Transmission(DTX) and Comfort Noise Generator(CNG) algorithms.
     729的改进版,它描述了语音激活检测VAD、不连续传输DTX和舒适噪声产生器CNG等算法。
短句来源
     For hign quality random number is the foundation of white noise generator by the Monte Carlo method, new combined random number generator is adopted.
     高质量的随机数是采用MonteCarlo方法生成白噪声的基础,为此采用了新型的组合随机数发生器。
短句来源
     An automatic calibrating system for wide-band solid state noise generator
     宽带固态噪声源自动校准系统
短句来源
     Based on the M series and the inverse M series, this paper puts forward the structure of the multi dimensional inverse M series generator, which is approximate to a cyclic white noise generator with D.
     基于 M序列和逆 M序列 ,提出了多维逆 M序列发生器的结构形式。
短句来源
     A gaussian noise generator implemented with FPGA is also presented.
     还给出了正态分布随机数的产生法,用FPGA实现了算法。
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  noise generator
A formula is derived that linearly relates this duration to the signal from the antenna, in which the noise temperatures of the semiconductor noise generator and the matched load act as two reference values.
      
A large-aperture shf blackbody noise generator with a brightness temperature of 104 K
      
Correction to the noise temperature of a waveguide thermal noise generator due to nonuniform heating of the channel
      
The temperature distribution in the waveguide channel of a millimeter-band thermal noise generator is calculated.
      
Calculation of the temperature distribution along the transmission line of a thermal noise generator
      
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A low frequency noise generator using radioactive material as its noise source is dis-cussed in this paper. Four types of noise, i.e., the Gaussian, Rayleigh, random impulses and random square wave signals with poisson distribution can be obtained. The output of the generator is sufficiently large and stationary for analoque computation.

本文讨论了一种采用放射性物质作为噪声源的低频噪声发生器.这种噪声发生器能够输出四种噪声,即:随机脉冲序列、随机方波、正态噪声及瑞利噪声,并且足够大和比较稳定.

A thermal standard noise, gas discharge noise generators and a calibrating radiometer for 4mm band are discussed. Advantages and weak points of both the total-power and Dicke radiometers are evaluated. A calibrating system of total-power radiometer with IF attenuator has been set up, and its equalization and error equations are derived and analysed in this paper. An advantage of this system is that it can be used in all frequency bands. Furthermore, it uses fewer waveguide components, and the microwave...

A thermal standard noise, gas discharge noise generators and a calibrating radiometer for 4mm band are discussed. Advantages and weak points of both the total-power and Dicke radiometers are evaluated. A calibrating system of total-power radiometer with IF attenuator has been set up, and its equalization and error equations are derived and analysed in this paper. An advantage of this system is that it can be used in all frequency bands. Furthermore, it uses fewer waveguide components, and the microwave precision attenuator can be substituted by a precision IF attenuator. This is of practical significance for millimeter and submillimeter bands. This system, when used to calibrate gas discharge noise generators, gives an excess-noise ratio of 16.2 dB, the total error being ±0.45 dB. If the accuracy of the IF attenuator is 0.02 dB, the total crror will be ±0.3 dB.

本文论述了4mm波段热噪声标准、气体放电嗓声源以及定标辐射计,讨论了全功率辐射计与Dicke辐射计的优缺点,建立了中频衰减全功率辐射计的定标系统,并对系统的平衡方程及误差方程进行了推导和分析。

Simulating the stellar observation is a sort of very useful implement for the analysis and the reduction of photon counting data on Transit Instrument. In some cases, it is difficult to estimate the errors directly from the observed data because the data noise and the function of real signals is complicated. With the method of simulating observation, this problem would be solved. And the simulated data can be used to compare with the observed data in order to find out an experiential method for estimations....

Simulating the stellar observation is a sort of very useful implement for the analysis and the reduction of photon counting data on Transit Instrument. In some cases, it is difficult to estimate the errors directly from the observed data because the data noise and the function of real signals is complicated. With the method of simulating observation, this problem would be solved. And the simulated data can be used to compare with the observed data in order to find out an experiential method for estimations. The simulated data can be also used to study the reduction methods from a various number of methods and to determine the optimal one in order to get the best precision. The simulating observation is also worthy to study the instrumental accuracy and the influence of the hardware upon the precision of the observed data and their determinations. It has been found that the slit micrometer is very important to the precision. The optimal size of the slit is existed. With the method of simulation, the optimal slit size can be calculated. So that, better precision of the stellar observation will be achieved and fainter stars can be observed. In this paper, the simulating principle and process of photon counting data of meridian observations with one or muitislit micrometer will be discussed. In general, the output signal of meridian photon counting observation can be expressed as a convolution of the image profile function plus the background photon counts and their noise signal(cf.equation <1>)with a trapezoid weighting function.Because the atmospheric agitation is a random process, the image profile will be a gaussian function. The weighting function is determined by the constants of the slit, δ and the time interval of sampling. Asume Am is the amplitude of starlight counts with magnitude m_v, in order to get Am., we can observe the stars with magnitude m_0, and get their amplitude A_0. Am will be calculated from A_0. The background counts b can not only be experientially but also analytically determined. Using a Poisson random noise generator, the noise signal will be got. When the constants of the slit, the time interval of sampling,the variance of the image profile,the magnitude of the observed star and its declination are known, we can therefore simulate the meridian photon counting observation of the star. As an exaple, the application of the simulating method will be discussed. First, we analyse the image profile of a star, Simulated data will be used to find an experiential equation for the meridian observation on the Transit Instrument at Shaanxi Astronomical Observatory. This equation expresses a relation of an estimated parameter to the variance of a gaussian distribution. In comparison with the simulated data, the variance σ~2 of image profile can be calculated from the observed data of a star. By means of this method, we got σ=0″.7~1″.9. The second example is to discuss the influence of the slit width on the determining precision of meridian time. By experiences, we come to. the conclusion that the slit width of 20.6265 (used in the Transit Instrument at Shaanxi Astronomical Observatory) is not ideal one for stellar meridian observation. If the slit with 5″.width of the transparent part and with 15″ width of the reflective part were used, the determined precision of meridian time would be better,and fainter stars would be observed.

本文通过恒星子午光子计数观测过程的分析,给出了观测输出信号所满足的解析关系式。利用该关系式,采用实际信号的期望值加上Poisson随机噪声的办法得到输出信号的模拟值。通过对中星仪子午光子计数观测的模拟办法,得到恒星中天时光子计数模拟观测信号。利用模拟方法,讨论和解决了一个子午观测中的实际问题。

 
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