精密时钟噪声的按噪声分量分解与白噪声中f^—1随机过程的最优估计

对于任何精密时钟来说,其五种噪声分量的幂律谱系数不存在固定的比例关系,因而在对精密时钟进行最优综合时需要对其噪声进行按噪声分量分解。通过探讨白噪声中ｆ＾－１随机过程的最优估计,提出了一种分层次地对精密时钟噪声进行按噪声分量分解的方法。     

精密时钟噪声的半积分—半微分算子模型及其应用

通过确立半积分算子的概念，得到了精密时钟噪声中全部５种噪声分量与白噪声的时域联系，并建立了精密时钟噪声的与幂律谱模型完全等价的半积分－半微分算子模型，从而为分析和处理包含５种噪声分量的精密时钟噪声提供了新的、更有效的数学手段。     

时间尺度算法（精密时钟综合算法）的研究

时间尺度是通过综合众多精密时钟得到的。时间尺度的计算目前主要采用类ALGOS算法 ,这类算法的缺点是权值没有准确反映精密时钟噪声参数以及不能使五种噪声分量同时达到优化综合和不能形成实时的时间尺度。从精密时钟综合的优化算法原理出发 ,探讨了精密时钟噪声参数的估计、精密时钟噪声中噪声分量的分解等问题的解决方法 ,并由此提出了较优化的时间尺度算法 (精密时钟综合算法 ) ,还提出了对现有算法的改进意见。     

原子钟噪声误差估计方法研究

给出了原子钟不同噪声的模拟方法.研究了利用马氏过程理论模拟原子钟的频率闪变噪声,利用维纳过程理论估计频率白噪声的最大区间误差的方法.结合国家授时中心时频基准实验室9台铯原子钟的运行情况,估计了幂律谱模型的噪声系数,并根据噪声模型进行了仿真,最后得到了这9台铯原子钟的频率白噪声产生的最大区间误差估计.     

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。     

NTSC守时氢钟性能分析

首先对NTSC(National Time Service Center)守时实验室的氢原子钟进行了测试,为了规避铯原子钟噪声较大的影响,没有采用TA(k)或UTC(k)作为参考,而是以4台氢原子钟互为参考进行测试,利用四角帽法对氢原子钟的频率稳定度进行分析,估计出单台氢原子钟在不同取样时间上的Allan标准差.然后根据氢原子钟的特性,扣除趋势项,剔除异常值,利用数学方法平滑,分离出了氢原子钟的高斯噪声,并且通过了Kolmogorov-Smirnov检验,估计出单台氢原子钟高斯噪声.     

修正的极大似然法拟合幂律频数分布

针对包含饱和样本数据的频数幂律分布拟合,提出一个新的幂律分布指数的极大似然估计方法的修正公式.对比研究显示,修正公式适用于剔除异常饱和值的幂律频数拟合.如果不剔除饱和值,幂律指数的估计只能使用修正前的公式,其误差随幂律指数变化,指数较小时误差较大.由此建议,对于包含饱和样本的频数分布拟合,首先剔除异常的饱和值,然后对剩余不含饱和值的子集使用修正公式进行参数估计.     

在中意卫星时钟同步试验期间国内诸台站主钟之间的比对结果

本文列出了在1984年5月25日到6月7日中国和意大利两国利用Sirio-1卫星进行双向法卫星时钟同步试验期间,国内参加台站的主钟之间进行多种手段比对的统计结果,作了分析比较,并列出了最后采用的UTC(BAO)—UTC(i)逐日相位差表。中意卫星地面站工作钟之间的比对结果和意方台站钟之间的比对结果将另文刊载。根据本文及以上资料将很容易得出任何国内参加台站之间和国外参加台站之间的时钟比对结果.     

一种基于小波变换的氢铯联合守时算法研究

氢铯联合守时方法主要是研究两类性能不同的原子钟的有效组合而产生稳定的时间尺度.基于此,研究了一种联合守时算法,取得了初步结果.算法首先通过铯原子钟建立参考时间尺度,用于估计氢原子钟的速率和频率漂移;其次,利用小波多尺度分解的方法降低氢原子钟钟差多种噪声的影响;最后,利用氢原子钟的可预测性能,建立由氢原子钟产生的时间尺度.此算法的优点在于产生的时间尺度充分利用了氢原子钟的短期稳定度、氢原子钟的可预测性能并考虑了测量钟差带来的多种噪声的影响,是一种优化的原子时尺度算法.     

基于卡尔曼滤波的脉冲星计时研究

脉冲星是高速自转的中子星,其自转周期稳定,不受人为干扰破坏,可作为绝对时间的参考量.论文提出一种基于卡尔曼滤波算法的脉冲星授时方法,以太阳某同步轨道为例,对基于卡尔曼滤波的钟差控制以及脉冲星星表误差和脉冲到达时间(TOA)测量精度对授时精度的影响进行了仿真分析.结果表明,该方法可以有效消除星载时钟钟差并抑制其随时间的增加,解决了航天器搭载低成本时钟精度不能满足要求的问题.     

On Integrated Hard X-Ray Broken-Up Spectra of Solar Flares

The summation of two single power-law spectra with a rather big difference of the spectral indices and with comparable intensities looks like a broken-up spectrum. The spatially integrated hard X-rays contain contributions from different sources, like footpoint and looptop sources. Within the standard scenario of solar flares, the power-law index difference between the footpoints and looptop should be two. Taking the M7.6 flare on 24 October 2003 as an example, we showed that the hard X-ray spectrum itself for footpoints and looptop is a single power-law, but the spatially integrated spectrum presents a broken-up form. It is also shown that the time-integrated spectrum could present a broken-up form, although the spectrum in further refined intervals presents a single power-law. It is concluded that the integrated broken-up spectrum observed here is produced either by the summation of individual sources or by the temporal variation of a single source, not by the acceleration itself.     

同步辐射的局际性

由于同步幅射机制在天体物理应用中取得了巨大成功,近十多年来已出现滥用的趋势,“幂律能谱的电子－定辐射幂律谱”的传统观念其实有错误,对非均匀磁场,正确的公式应该是同步－曲率辐射公式,而不是同步辐射公式,将一般磁场都看成平衡匀匀场,用同步辐射讨论,很可能导致对天体情况的错误描述。     

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.     

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

For the first time a quasi-simultaneous multi-wavelength campaign has been performed on an Anomalous X-ray Pulsar from the radio to the hard X-ray band. 4U 0142+61 was an INTEGRAL target for 1 Ms in July 2005. During these observations it was also observed in the X-ray band with Swift and RXTE, in the optical and NIR with Gemini North and in the radio with the WSRT. In this paper we present the source-energy distribution. The spectral results obtained in the individual wave bands do not connect smoothly; apparently components of different origin contribute to the total spectrum. Remarkable is that the INTEGRAL hard X-ray spectrum (power-law index 0.79±0.10) is now measured up to an energy of ～230 keV with no indication of a spectral break. Extrapolation of the INTEGRAL power-law spectrum to lower energies passes orders of magnitude underneath the NIR and optical fluxes, as well as the low ～30 μJy (2σ) upper limit in the radio band.     

The luminosity function of low-mass X-ray binaries in galaxies

The X-ray luminosity function of low-mass binaries constructed from the observations of point like X-ray sources in galactic bulges can be explained in terms of the main evolutionary relations for the rate of mass transfer onto a compact object. The observed scatter of luminosities for individual low-mass X-ray sources in our Galaxy is shown to be satisfactorily described by a symmetric quasi-Lorentz curve with a dispersion proportional to the mean luminosity. Such a form of the mean luminosity function for individual sources does not affect the power-law pattern of the luminosity function for the entire population of sources that is expected for a power-law dependence of the mass transfer rate in a close binary on the mass of the Roche lobe—filling optical component.     

On Both the Time Histories of the 0.511 MeV Line and 2.223 MeV Line from the X4.8 Flare of 23 July 2002 Observed with Rhessi

High-spectral-resolution measurements of the 2.223 MeV neutron capture line and the 0.511 MeV positron-electron annihilation line have been made with the Reuven Ramaty High-Energy Solar Spectroscopic Imager during the X4.8 flare of 23 July 2002. We have tried to explain both the time histories of the 2.223 MeV line and the 0.511 MeV line, adopting a power-law spectrum of accelerated ions. The results show that with a power-law spectral index of 3.52, the calculational time histories can roughly reproduce the observations. An improved fit between the calculated 2.223 MeV line and the observed 2.223 MeV line can be achieved if we allow the spectrum of accelerated ions to vary with time.     

Electron acceleration in solar flares

We present observations of an intense solar flare hard X-ray burst on 1980 June 27, made with a balloon-borne array of liquid nitrogen-cooled germanium detectors which provided unprecedented spectral resolution (≲1 keV FWHM). The hard X-ray spectra throughout the impulsive phase burst fitted well to a double power-law form, and emission from an isothermal 10⁸–10⁹K plasma can be specifically excluded. The temporal variations of the spectrum indicate that the hard X-ray burst is made up of two superposed components: individual spikes lasting ∼3–15 s, whch have a hard spectrum and a break energy of 30–65 keV; and a slowly varying component characterized by a soft spectrum with a constant low-energy slope and a break energy which increases from 25 keV to ≳100 keV through the event. The double power-law shape indicates that acceleration by DC electric fields parallel to the magnetic field, similar to that occurring in the Earth's auroral zone, may be the source of the energetic electrons which produce the hard X-ray emission. The total potential drop required for flares is typically ∼10² kV compared to ∼10 kV for auroral substorms.

     

Hard X-ray spectrum of Mkn 421 during the active phase

Spectral measurement of Mkn 421 were made in the hard X-ray energy band of 20–200 keV using a high sensitivity, large area scintillation counter telescope on November 21, 2000 and these coincided with the onset of an active X-ray phase as seen in the ASM counting rates on board RXTE. The observed spectrum can not be fitted to a single power law similar to the PDS data of BeppoSAX. The data can be fitted both by a two component power-law function or a combination of an exponential function with a power law component at the high energies above 80 keV. We identify these components with those arising from the synchrotron self compton and the high energy power-law tail arising from the upgrading of the thermal photons due to multiple Compton scattering a la Cyg X-1. A comparison with the earlier data clearly suggests a spectral variability in the hard X-ray spectrum of the source. We propose a continuously flaring geometry for the source as the underlying mechanism for energy release.     

Angular power spectrum of CMB anisotropy from WMAP

The remarkable improvement in the estimates of different cosmological parameters in recent years has been largely spearheaded by accurate measurements of the angular power spectrum of cosmic microwave background (CMB) radiation. This has required removal of foreground contamination as well as detector noise bias with reliability and precision. Recently, a novel model-independent method for the estimation of CMB angular power spectrum from multi-frequency observations has been proposed and implemented on the first year WMAP (WMAP-1) data by Saha et al. [Saha, R., Jain, P., Souradeep, T., 2006. ApJL, 645, L89]. We review the results from WMAP-1 and also present the new angular power spectrum based on three years of the WMAP data (WMAP-3). Previous estimates have depended on foreground templates built using extraneous observational input to remove foreground contamination. This is the first demonstration that the CMB angular spectrum can be reliably estimated with precision from a self contained analysis of the WMAP data. The primary product of WMAP are the observations of CMB in 10 independent difference assemblies (DA) distributed over five frequency bands that have uncorrelated noise. Our method utilizes maximum information available within WMAP data by linearly combining DA maps from different frequencies to remove foregrounds and estimating the power spectrum from the 24 cross-power spectra of clean maps that have independent noise. An important merit of the method is that the expected residual power from unresolved point sources is significantly tempered to a constant offset at large multipoles (in contrast to the l² contribution expected from a Poisson distribution) leading to a small correction at large multipoles. Hence, the power spectrum estimates are less susceptible to uncertainties in the model of point sources.