用状态空间模型递推模拟振荡器噪声

对振荡器的五种噪声之间的关系作了介绍,并对相位时间信号的状态空间模型的基本理论作了描述.在此基础上导出了五种噪声的递推模拟方法.最后模拟了这五种噪声并分析了它们的功率谱.结果表明,功率谱符合这几种噪声的定义.     

原子钟频率稳定度评估方法综述

原子钟通过稳定的频标来测量时间,但频标输出信号会受到不同来源噪声的影响,因此原子钟间相位偏差可以看作服从幂律∑h_αf^α的连续随机过程。该随机过程并非平稳的,一般是通过高阶的差分使得序列平稳化,常用的时域频率稳定度评估方法便是采用此种思路。幂律噪声实际是对白噪声过程进行微分和积分得来,不同幂律的噪声对应不同的随机微分方程,实际上幂律噪声的仿真也是通过白噪声基于此实现的。首先介绍了不同幂律噪声的鉴定方法,并结合文献给出常见幂律噪声对应的微分方程;然后介绍了不同频率稳定度评估方法之间的关系和其相应的传递函数,并简单总结了其置信区间的计算方法。该文的工作有助于构建原子钟随机模型和频率稳定度评估方法。     

一种频率源噪声频谱拟合方法的研究

在分析频率源的噪声特性的时候,经常需要由Allan方差或功率谱计算频率源的五种噪声强度系数的值,通常采用人工分析的方法,求出噪声系数,这严重阻碍了自动化处理的应用。给出的一种自动拟合算法可以满足这方面的需要。在最小均方误差意义下,这种算法能自动完成对噪声类别的判定、噪声区间的划分以及噪声系数确定,所有这些无须人工参予。最后,对模拟数据和实测的几种频率源的功率谱曲线进行拟合,实验研究的结果表明这种方法拟合的相对误差不超过11％。     

天文CCD片内放大器的噪声特性及其抑制方法

分析了低光度天文应用时CCD器件的主要噪声源的噪声特性和三种典型CCD读出信号处理方式的噪声抑制效果;提出了天文CCD读出信号的相关多次采样(CMS)处理新方法,并分析了四次采样抑制CCD读出噪声的实验结果。     

具有泊松噪声分布的图象复原方法

本文以ＣＣＤ图象为技术背景，指出ＣＣＤ图象噪声主要将以与信号有关的泊松噪声形式存在。根据图象形成的模型及图象统计特性，提出了最大似然法，最大后验概率法及最大复原方法，针对ＭＡＰ法提出了具体算法和参数估计方法，并提出应用图象分割法来提高计算机复原速度，节省存储空间。     

星系形成的超大型计算机模拟

扼要地就数值模拟在星系形成研究中的作用，数值模拟与解析模型之间的关系，数值模拟的局限性等几方面的问题作了综述，然后介绍了马普小组与日本东京大学最近的合作情况，包括合作得到的模拟样本，研究成晨和正在开展的工作。     

基于修正线性组合模型的原子钟钟差预报

原子钟钟差预报在时频工作中起着重要作用.目前常用的预报模型各有优缺点,为了综合各种预报模型特点,可以考虑组合这些模型预报的结果.针对线性组合模型预报钟差时存在的问题,提出了学习权的概念,以有效地利用各种精度信息,建立了修正组合预报模型.为了验证该方法的有效性,选取了4颗GPS卫星IGS(International GN...     

原子钟信号的神经网络模型

时间尺度的连续性要求对原子钟信号进行必要的预测,预测的实质是建立一个模型来逼近原子钟的信号,前向神经网络具有良好的副近非线性 函数的能力,用神经网络模型来预测原子钟信号,并与AD模型的预测结果作了比较。     

Real-time Solution of Atomic Clock Operating Parameters Based on Adaptive Kalman Filtering

The real-tine and accurate knowledge of the operation of an atomic clock is of great significance to satellite navigation and time keeping. In the light of the problems which exist in the real-time solution of the atomic clock operating parameters by means of the standard Kalman filtering, the method for applying the adaptive Kalman filtering model based on the prediction residual to the real-time solution of the clock parameters is proposed. An adaptive factor is constructed by the model based on the standard Kalman filtering model so that the accurate and reliable estimates of the operating parameters may be given rather fast after the frequency modulation or phase modulation of the atomic clock. Finally, in combination with the 3 computational examples of the work on the navigation and time keeping, the effectiveness of the method is verified.     

Monte Carlo Simulation of Solar Active-Region Energy

A Monte Carlo approach to solving a stochastic-jump transition model for active-region energy (Wheatland and Glukhov: Astrophys. J. 494, 858, 1998; Wheatland: Astrophys. J. 679, 1621, 2008) is described. The new method numerically solves the stochastic differential equation describing the model, rather than the equivalent master equation. This has the advantages of allowing more efficient numerical solution, the modeling of time-dependent situations, and investigation of details of event statistics. The Monte Carlo approach is illustrated by application to a Gaussian test case and to the class of flare-like models presented in Wheatland (Astrophys. J. 679, 1621, 2008), which are steady-state models with constant rates of energy supply, and power-law distributed jump transition rates. These models have two free parameters: an index (δ), which defines the dependence of the jump transition rates on active-region energy, and a nondimensional ratio ( ) of total flaring rate to rate of energy supply. For the nondimensional mean energy of the active-region satisfies , resulting in a power-law distribution of flare events over many decades of energy. The Monte Carlo method is used to explore the behavior of the waiting-time distributions for the flare-like models. The models with δ≠0 are found to have waiting times that depart significantly from simple Poisson behavior when . The original model from Wheatland and Glukhov (Astrophys. J. 494, 858, 1998), with δ=0 (i.e., no dependence of transition rates on active-region energy), is identified as being most consistent with observed flare statistics.     

铯原子喷泉钟低噪声频率综合器的研制

铯原子喷泉钟是现今的时间频率的基准,其中的频率综合器性能直接影响喷泉钟的稳定度性能.介绍了铯原子喷泉钟的低噪声频率综合器的设计和实现.对该频率综合器的测试表明,输出的9.2 GHz频率信号的相位噪声为-82 dB[Rad2/Hz]@offset1 Hz,满足设计要求.     

一种新的守时型原子钟综合时间尺度方法研究

在这篇文章中, 提出了一种基于改进的指数平滑和Vondrak_Cepek联合平滑的氢铯综合时间尺度产生方法. 以最小误差方法为理论基础, 动态估计氢原子钟频率漂移参数, 提升氢原子钟钟差预测准确度; 基于改进的二次指数平滑产生氢原子钟组时间尺度、加权平均方法产生铯原子钟时间尺度, 同时设计Vondrak_Cepek滤波器以结合两类时间尺度长短期稳定度优势, 提升综合时间尺度性能. 实验结果表明, 所提方法产生的氢铯综合时间尺度时稳可达1.60x10^-15,天稳可达3x10^-15,优于ALGOS、AT1和Kalman滤波3种经典方法产生的时间 尺度性能.     

Research on the Method of Noise Error Estimation of Atomic Clockstwo

The simulation methods of different kinds of noises of atomic clocks are given. The frequency flicker noise of atomic clocks is studied by using the Markov process theory. The method for estimating the maximum interval error of the frequency white noise is studied by using the Wiener process theory. Based on the operation of 9 cesium atomic clocks in the laboratory of time and frequency primary standards of NTSC (National Time Service Center), the noise factors of power-law spectrum models are estimated, and the simulations are carried out according to the corresponding noise models. Finally, the maximum interval error estimates of the frequency white noises generated by the 9 cesium atomic clocks are acquired.     

银河系球状星团轨道参数分布的Monte Carlo模拟

选取前文中所列出的29个累积光谱型为F型的球状星团中的3个作为样本，深入研究了初始观测资料的不确定性和选用不同的银河系引力势模型，对样本星团轨道参数的影响。首先采用Monte Carlo方法产生3个样本球状星团的模拟初始观测数据，而后，以这些模拟数据为初始条件，在3种不同的银河系引力势模型下进行轨道计算，得到此3个样本的模拟轨道参数。模拟计算的结果表明：根据模拟初始数据生成的样本轨道参数分布形态大致可分为高斯分布、准高斯分布和非高斯分布等3类；初始观测数据的不确定性对样本轨道参数分布的影响，与样本星团的选择和轨道参数的类型有关；选用不同的银河系引力势模型，对3个样本星团的各个轨道参数的分布和形态结构也会产生不同程度的影响。该工作的结果，可供深入研究球状星团的整体运动和动力学性质等问题参考。     

白噪声中f~(-2)随机过程的最优估计

从功率谱的角度分析了白噪声中f-2随机过程的最优估计问题，推导了线性估计方法的精度极限，并通过对若干线性估计方法的精度进行分析和比较，得到了一些有意义的结论。     

Simulation of extensive air showers at ultra-high energy using the CORSIKA Monte Carlo code

Extensive simulations have been carried out with CORSIKA version 5.62 to investigate the general properties of giant cosmic air shower in the energy range 1–100 EeV. The comparison between protons, heavy nuclei and γ initiated showers exhibits unexpected and interesting features. The apparent muon electron ratio at great distances (1.5 km from axis) tends to be comparable at ultra-high energy in both photon-induced cascades and hadronic cascades (compensation between the enhancement versus energy of photo-production cross-section and of the decrease of both pair production cross-section and the bremsstrahlung cross-section, with Landau–Pomeranchuk–Migdal effect); for proton and nuclei primaries, a correlation with lateral electron profile suggests a new energy estimator, in complement to electrons size or density at 600 m, suitable for the determination of the total primary energy spectrum. Another tendency is the local contrast in the abundance of positive and negative muons (with a possible ellipticity in the lateral muon distribution) induced by the geomagnetic field, especially visible for some azimuthal and zenith angles. These distortions are more intense for heavy primaries; they can be exploited on the most favorable horizontal axis or areas, for the discrimination between nuclei and protons.     

用Monte Carlo方法拟合超新星SN 1993J的早期光谱

通过把从光球辐射出来的连续谱能量分成大量的光子包，然后用MonteCarlo方法跟踪这些光子包从光球向超新星包层外运动的过程，这一方法能很好地解决超新星的光谱拟合中的谱线覆盖问题，由于同时编制了用于构造超新星包层中的密度结构和丰度分布的程序，以及大量的用于比较观测和理论拟合的绘图和支持程序，使我们的MonteCarlo光谱拟合软件包能够很好地运用于超新星的早期光谱研究。本文给出了SN1993J在1993年4月13日的观测光谱的运行实例。