一种铷原子钟双钟热备相位无扰切换系统的设计

为了满足时间统一系统中主钟与备份钟的时间、频率信号在切换时的连续性要求,提出并实现了一种铷原子钟双钟热备相位无扰切换系统的技术方案,阐述了双钟间频率与相位同步和信号无扰切换的方案原理,给出了系统组成与主要控制程序的框图及测试结果。采用本方案可使主钟与备份钟输出信号的时差小于±0．55ns,并实现了信号的无扰切换,满足了工程应用的要求。     

GNSS CV精密时间服务系统的可靠性改进

为了提高中国科学院国家授时中心基于GNSS CV精密时间服务系统的可靠性,提出并采用了主备服务器双机热备的技术方案.阐述了服务器主从模式双机热备的工作模式,包括主、备服务器间的数据备份、服务器运行状态的检测和切换.根据系统中数据类型和备份要求的不同,采用了相应的备份策略和备份程序实现主备服务器间数据备份;设计了主备服务器的运行状态检测和切换控制流程.测试表明,采用服务器双机热备技术显著提高了GNSS CV精密时间服务系统的可靠性.     

主钟的频率驾驭算法研究

各时间实验室产生的标准时间UTC(k)是UTC(协调世界时)在各时间实验室的物理实现.为了更好地驾驭主钟系统,使得主钟系统输出时间与标准时间UTC的偏差尽可能地小,且主钟系统输出的信号满足好的短、长期稳定度,因此提出了一种新的驾驭算法,并编制了相应的软件,自动定时计算给出相位微调仪的调整量,从而使频率驾驭后的主钟系统输出时间与标准时间UTC的偏差控制在较小的相位偏差范围内,并尽量不影响其稳定度.测试结果表明了新的主钟频率驾驭算法可以实现相位偏差保持在±15 ns之内,并且在保证不降低UTC(k)长期稳定度的前提下,可以提高它的短期稳定度.     

氢原子钟的频率驾驭算法研究

以氢钟作为主钟系统的频率源,可产生短期稳定度更好的本地时间UTC(k),氢钟通常具有频率漂移效应,这使得氢原子钟的长期稳定度随着时间的推移不断降低,进而影响UTC(k)的稳定度与准确度.为解决这一问题,比较分析了氢钟和铯钟的性能,改进了氢钟参与时间尺度计算的算法,并提出了基于主钟为氢钟的频率驾驭算法.通过搭建试验系统,编制相关的软件,对该算法进行了检验.测试结果表明当氢钟参与原子时计算时,可有效改善参考时间尺度的短期稳定度,同时主钟频率源为氢钟比主钟频率源为铯钟产生的本地时间UTC(k)具有更好的短期频率稳定度.     

SOHM型氢钟在国家授时中心的运行情况分析

上海天文台研制的型号为SOHM-3和SOHM-4的3台氢原子钟在中国科学院国家授时中心(NTSC)已经运行了一年多时间。收集了每个氢原子钟与NTSC主钟的时间比对数据。数据的分析结果给出了这几台氢钟在不同采样间隔上的频率稳定度,也显示出1台氢钟明显的相位跳变,讨论了这种相位跳变的原因。比较了这3台氢钟和从美国进口的Symmetricom公司制造的氢钟的频率稳定度的温度变化效应,指出了上海天文台研究制的氢钟存在的主要问题。     

氢钟守时应用

通过对氢钟时差测量数据的二次差分,获得频率漂移的准确量值后对氢钟时差测量数据进行修正,经过频率漂移修正后的氢钟数据在保持其良好短稳特性的基础上长稳性能得到了较大提升,达到或超过性能中上的高性能管的商品铯钟5071A的常稳指标,这种处理方法能提高守时氢钟对时间实验室所保持的时间尺度的贡献。     

脉冲星对氢原子钟的频率驾驭算法研究

氢原子钟具有较高的短期稳定度,将其作为主钟可在短期内产生高精度的本地时间信号.但氢钟存在频率漂移现象,导致其长期稳定度较差,从而影响本地时间的准确性.毫秒脉冲星自转高度稳定,借助于其长期稳定度高的特性,可定期实现对氢原子钟的频率驾驭,并对实时信号加以控制.首先分析了国际脉冲星计时阵(International Pulsar Timing Array,IPTA)第二批发布数据中四颗毫秒脉冲星的稳定度随时间的变化,同时采用哈达玛方差分析了中国科学院国家授时中心(National Time Service Center,NTSC)一台氢钟的频率稳定性能,最终给出了利用脉冲星驾驭氢原子钟频率的方法.     

北斗星地双向时频传递与广广播钟差精度分析

与其他卫星导航系统不同,北斗卫星导航系统采用星地双向时间比对技术,直接测量卫星钟相对于地面保持的系统时间的钟差,并用于广播电文钟差参数的建模。讨论了电离层延迟误差、卫星相位中心误差等不同误差源对不同类型卫星双向时间同步卫星钟差精度的影响。实测数据分析结果表明,星地双向卫星钟差内符合精度(RMS)优于0.15 ns。利用双向卫星钟差序列,对广播星历钟差参数预报精度进行了分析,统计结果显示广播电文钟差参数预报1 h,精度在2 ns以内,移动卫星刚入境时,钟差参数预报6 h误差可达10 ns。     

时间频率信号判别器的研制

本文叙述了对由频率源分频钟组成的时间频率系统的工作状态进行实时监测判别的方法以及该设备的工作原理。     

NTSC的双混频时差测量系统试运转结果分析

中国科学院国家授时中心(NTSC)新进口的由德国Timetech公司制造的双混频时差测量系统(dual mixer time difference system,DMTD)已经通过了试运行。介绍了DMTD的工作原理和设备结构。NTSC时频基准实验室的主钟(MC)信号作为DMTD的频率参考信号,5个氢钟和18个铯钟的频率信号作为被测信号与MC信号进行相位比对。用频率分配放大器输出的多路MC信号也作为被测信号用以监测DMTD本身的精度和稳定度。给出了DMTD和时间间隔计数器TIC实际测量结果的比较及误差分析。测量结果表明DMTD特别适用于频率短期稳定度非常高的氢原子钟这样的频标之间的频率和时间比对。该设备将用于NTSC的守时工作,不久的将来也将用于铯喷泉与氢钟的频率比对。     

A survey of orbits of co-orbitals of Mars

Many asteroids with a semimajor axis close to that of Mars have been discovered in the last several years. Potentially some of these could be in 1:1 resonance with Mars, much as are the classic Trojan asteroids with Jupiter, and its lesser-known horseshoe companions with Earth. In the 1990s, two Trojan companions of Mars, 5261 Eureka and 1998 VF₃₁, were discovered, librating about the L₅ Lagrange point, 60° behind Mars in its orbit. Although several other potential Mars Trojans have been identified, our orbital calculations show only one other known asteroid, 1999 UJ₇, to be a Trojan, associated with the L₄ Lagrange point, 60° ahead of Mars in its orbit. We further find that asteroid 36017 (1999 ND₄₃) is a horseshoe librator, alternating with periods of Trojan motion. This asteroid makes repeated close approaches to Earth and has a chaotic orbit whose behavior can be confidently predicted for less than 3000 years. We identify two objects, 2001 HW₁₅ and 2000 TG₂, within the resonant region capable of undergoing what we designate “circulation transition”, in which objects can pass between circulation outside the orbit of Mars and circulation inside it, or vice versa. The eccentricity of the orbit of Mars appears to play an important role in circulation transition and in horseshoe motion. Based on the orbits and on spectroscopic data, the Trojan asteroids of Mars may be primordial bodies, while some co-orbital bodies may be in a temporary state of motion.     

Estimation of the Time Scale of Merging of the Components of Contact Binaries of the W UMa Type

Time scales of the transition from contact binary systems of the W UMa type to single stars of the blue straggler type are estimated. A model of one-way mass transfer from the primary component to the companion inside a common envelope (Eggen et al.) and a model of a contact binary lying on the zero-age main sequence with a companion that is losing mass (F. van't Veer) are used to calculate these scales. The merging times of components were calculated for 304 contact systems of the W UMa type from the Catalog of Approximate Photometric and Absolute Elements of Eclipsing Variable Stars on a scale of loss of mass and orbital angular momentum due to magnetic braking, under the assumption of synchronization of the axial rotation and orbital revolution. On the basis of the resulting statistics, the characteristic merging scales are 0.4-0.6 and 0.5-0.7 Gyr, respectively, for the above two models. The results of a comparison with the work of other authors are discussed.     

Equation of state and anisotropy of pressure of magnetars

Magnetars are the neutron stars with the highest magnetic fields up to 10¹⁵–10¹⁶ G. It has been proposed that they are also responsible for a variety of extra-galactic phenomena, ranging from giant flares in nearby galaxies to fast radio bursts. Utilizing a relativistic mean field model and a variable magnetic field configuration, we investigate the effects of strong magnetic fields on the equation of state and anisotropy of pressure of magnetars. It is found that the mass and radius of low-mass magnetars are weakly enhanced under the action of the strong magnetic field, and the anisotropy of pressure can be ignored. Unlike other previous investigations, the magnetic field is unable to violate the mass limit of the neutron stars.     

Investigation of Times of Minima of Selected Early-Type Eclipsing Binaries

New precise times of minimum light for several early-type eclipsing binaries were obtained at three observatories. The changes of period of the following measured binaries are discussed: V1182 Aql, LY Aur, SZ Cam, FZ CMa, QZ Car, LZ Cen, V606 Cen, AH Cep and TU~Mus.     

On the application of optimization methods to the determination of members of families of periodic solutions

The techniques used for the numerical computation of families of periodic orbits of dynamical systems rely on predictor-corrector algorithms. These algorithms usually depend on the solution of systems of approximate equations constructed from the periodicity conditions of these orbits. In this contribution we transform the root finding procedure to an optimization one which is applied on an objective function based on the exact periodicity conditions. Thus, the determination of periodic solutions and families of such orbits can be accomplished through unconstrained optimization. In this paper we apply and compare some well-known minimization methods for the solution of this problem. The obtained results are promising. This revised version was published online in July 2006 with corrections to the Cover Date.     

淮河洪水的可公度性分析

分析了上两个世纪发生在淮河的洪水事件的可公度性，根据其可公度值及其黄金分割点指出1991年与2003年淮河洪水的不可避免，最后讨论了可公度性的局限及淮河洪水可公度值的可能机制。     

Modeling of lightcurves of binary asteroids

We present a numerical method for inverting long-period components of lightcurves of asynchronous binary asteroids. Data of five near-Earth binary asteroids, (175706) 1996 FG₃, (65803) Didymos, (66391) 1999 KW₄, (185851) 2000 DP₁₀₇ and (66063) 1998 RO₁, for two of them from more than one apparition, were inverted. Their mutual orbits' poles and Keplerian elements, size ratios, and ellipsoidal shape axial ratios were estimated via this inversion. The pole solutions and size ratios for 1999 KW₄ and 2000 DP₁₀₇ are in a good agreement with independent estimates from radar measurements. We show that uncertainties of estimates of bulk densities of binary systems can be large, especially when observed on short arcs.     

Influence of Neutron Star Parameters on Evolutions of Different Types of Pulsar

Influences of the mass, moment of inertia, rotation, absence of stability in the atmosphere and some other parameters of neutron stars on the evolution of pulsars are examined. It is shown that the locations and evolutions of soft gamma repeaters, anomalous X-ray pulsars and other types of pulsar on the period versus period derivative diagram can be explained adopting values of B < 10¹⁴ G for these objects if they have smaller mass (e.g. about 0.5 Solar mass) compared to the conventionally adopted values of mass. This approach gives the possibility to explain many properties of different types of pulsar.     

Study of the effect of metallicity on the amplitudes of Cepheids

Results concerning the dependence of photometric and radial velocity amplitudes on metallicity are presented based on about 200 Galactic classical Cepheids pulsating in the fundamental mode. The Galactic distribution of the [Fe/H] value of Cepheids is also studied. We show that the photometric amplitude ratio A_I/A_V is independent of metallicity. The observed dependence of this ratio on the pulsation period does not correspond to the theoretical predictions. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)