共查询到20条相似文献，搜索用时 62 毫秒
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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. 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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中国科学院国家授时中心(NTSC)BPL长波授时台升级改造项目要求实现BPL系统的工作钟信号T(PU)的自动监控.T(PU)的控制指标为T(PU)与NTSC时频基准实验室的主钟信号UTC(NTSC)之间的相位时间差的绝对值| UTC(NTSC)-T(PU)|小于50 ns;T(PU)的频偏绝对值优于5×10-13.为达到上述指标,并尽可能提高T(PU)的准确度,研究了在采用不同类型的原子钟作为工作钟频率源时所需采用的T(PU)的监控方法.结论是对日稳较好的频率源,用对工作钟频率源的频偏进行准实时预报得到的值和实测得到的相位时间差UTC(NTSC)-T(PU)来计算应该加到相位微调仪上的频率补偿值,从而进行工作钟的频率驾驭,可以大大提高工作钟信号T(PU)的准确度;而对不太稳定的频率源,频偏准实时预报准确度很差,采用几个月时间段内的平均频偏以及实时实测的相位时间差来进行频率驾驭,以便确保T(PU)的准确度. 相似文献
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《天文学报》2018,(6)
主动型氢原子钟是时间尺度建立和保持的主要频率源,具有短期稳定度高及相位噪声低等特性,目前在国际原子时TAI (International Atomic Time)及各地方时间尺度中的作用日益重要.首先结合主动型氢原子钟内部状态参数,分析状态参数与氢原子钟比对数据的相关性,提出了氢原子钟性能监测方法.其次,针对氢原子钟性能特点,在衡量氢原子钟性能最主要的两方面,即频率稳定度及"可预测性"方面,给出了氢原子钟性能评估方法,并利用该方法对目前国际通用的两种主动型氢原子钟(CH1-75型及MHM-2010型)进行性能评估.原子钟状态参数与比对数据联合分析结果表明,状态参数监测可以有效预报钟性能的变化.原子钟频率稳定度及"可预测性"评估结果表明,中、长期稳定度越高的原子钟"可预测性"也越好. BIPM (Bureau International des Poids et Measures)权重验证结果表明,基于BIPM公布数据以及基于2次模型两种预报方法计算出来的钟"可预测性"均与BIPM公布的权重相吻合,可以作为钟"可预测性"的定量评估方法. 相似文献
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该文根据NTSC 20多台原子钟的ADEV和HDEV的分析、BIPM发表的TAI系统中原子钟的速率公报和权重报告.讨论了在高精度守时系统中对原子钟频率稳定度的要求.建议用τ≈30 d铯钟的ADEV和氢钟的HDEV至少达到1E-14来作为一个钟能否用于高精度守时的判断标准. 相似文献
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SOHM-4型氢原子钟的设计改进与初步性能 总被引：1，自引：3，他引：1
氢原子钟是一种最稳定的 (除极短测量时间间隔之外 )频率标准 ,但是环境温度变化及微波谐振腔老化会引起原子钟输出频率的变化 ,从而导致氢原子钟长期性能变差。为了减小这些影响 ,可借助一种自动调谐器来确保谐振腔的频率始终工作在所需的频率上 ,并采用新的温度控制系统来改善氢原子钟的长期性能。针对这些年来许多氢钟出现的有关问题 ,上海天文台在借鉴国外氢钟实验室经验的基础之上 ,对原有氢钟进行了技术改造 ,并为国家授时中心研制了SOHM - 4型氢原子钟。对该型氢原子钟技术改造特点作了介绍 ,并给出了期望的性能指标及初步的测试结果 相似文献
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Solar System Research - Finding and studying possible collisions of asteroids approaching the Earth requires a significant amount of computation. This paper describes the R0 program created to... 相似文献
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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. 相似文献
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In the text-books of astronomy, sections generally related to the Moon deal with the orbital elements of the Earth-Moon system such asa, e, i, ,
and the time of perigee passage. While the MEAN of the first of the three elements do not vary, mean longitude of the ascending node-mean longitude of the lunar perigee and the time of perigee passage undergoes secular as well as periodic changes due predominantly to the action of the Sun's gravitational attraction. While to a certain degree, explanations related to the calculation of the lunar orbit parameters are given, not a single graphical representation of these short- or long-periodic changes are presented. We allow the number of data related to these periodic changes must cover a large span of time; and if regression of the line of nodes or advances of the line of apses are to be graphically seen, data covering 18.61 and 8.85 yr, respectively, are needed. In this work we particularly aim at the graphical representation of the periodic changes of the line of nodes. 相似文献
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R. A. Vardanian 《Astrophysics》1995,38(4):394-395
Published in Astrofizika, Vol. 38, No. 4, pp. 700–702, October–December, 1995. 相似文献
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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. 相似文献