铷钟光谱灯老化的实验研究和寿命评估

铷光谱灯(铷灯)是汽泡式铷原子钟的关键部件。铷灯内金属铷的损耗是决定铷原子钟使用寿命的主要因素。为了预测铷灯使用寿命期内的铷消耗量,采用差示扫描量热技术对6个铷光谱灯开展了8a的铷消耗量测量。依据铷消耗模型的经验公式对铷消耗量数据用最小二乘法线性拟合,得到了一种肖特耐碱金属玻璃铷光谱灯铷消耗模型的各项参数。数据分析结果表明:铷与灯泡内所含杂质的反应消耗量在20~60μg之间,铷的消耗率稳定在0.18~0.28μg/h之间。以正常工作时铷消耗量最多的铷灯的拟合参数计算,10a使用寿命期的铷消耗量约为127μg。与相应时间内实际的铷量消耗的比较表明,使用该模型预测的结果是相对保守和可靠的。     

一种铷原子频标射频倍频单元的实现

讨论了射频倍频单元对汽泡型铷原子频标频率稳定度的影响,介绍了一种我们新研制的用于小型汽泡型铷原子频标的数字锁相倍频电路。将该数字锁相倍频电路接入铷原子频标系统后,闭环测得该频标系统的稳定度为σy（r=1s）≤3×10^-11,达到商用小型铷原子频标性能指标,而该倍频电路板的面积仅为原倍频电路板面积的1／2,功耗仅为原倍频电路的1／3。     

一种超小型汽泡铷原子频标

为满足对小型化铷原子频标的需求,设计了一种超小型汽泡铷原子频率标准。介绍了该超小型汽泡铷原子频标的设计。通过全新设计的小型光谱灯和集成腔泡系统,配合优化设计的电路部分,成功地将整机体积减小至140 cm3,重量仅为250 g,稳态功耗7 W。测试结果表明其短期稳定度优于1.5×10-11/τ(1 s≤τ≤100 s)。     

一种微型化铷原子钟

报道了一种微型化铷原子钟,它采用一种新型陶瓷填充微波腔来减小物理部分体积,其铷光谱灯采用升压电路以实现快速点亮,整机电子线路采用低电压技术,在国内首次对这类铷钟实现12V直流供电,并且首次对这类铷钟加入与外秒同步的功能。该铷原子钟体积为190mL,开机3min后可实现锁定,锁定后频率稳定度为1．5×10^-11／√τ（τ：1～1000s）,稳态功耗为5．5W。     

一种锁相环调频方法在铷原子频标中的应用

为了进一步实现铷原子频标小型化,分析了几种典型的锁相环调频电路及其特点,设计了一种锁相环二进制移频键控2FSK(binary frequency shift keying)调频方案,给出了调频信号的频谱测试结果。该调频方案已成功地应用在小型化数字式铷原子频标中,能够满足小型化铷原子频标的要求。     

铷原子频标小型化发展现状

铷原子频标使用最广泛,小型化是其最重要的发展趋势。微波腔小型化、电子线路数字化以及附加特殊功能是铷原子频标小型化的主要技术手段。相干布居囚禁(CPT)频标是一种可以做到芯片级的新型原子频标。目前相干布居囚禁频标的技术方案有:传统方案,物理系统采用MEMS(micro-electro-mechanical system)[0]技术的方案和整机采用MEMS[0]技术的方案。实现小型化后的原子频标将会迎来蓬勃发展的前景。     

铷原子频标微波高次倍频器的分析与设计

设计了一种采用阶跃恢复二极管来实现的、用于被动型铷原子频标的微波高次倍频器。调试结果表明:该倍频器的输入信号频率为90MHz;倍频次数为76;输出信号频率为6 840MHz;输出功率为-18.2dBm;对邻近谐波抑制度为28.75dB。该倍频器接入铷原子频标后,能实现闭环锁定,符合小型化铷原子频标的要求。     

DFB半导体激光抽运铷原子频标

在传统铷原子频标的基础上,利用一台780 nm的DFB半导体激光器代替铷光谱灯作为抽运光源,将激光的频率锁定在87Rb原子的循环跃迁线(52S1/2,F=2→52P3/2,F=3)上,实现了微波铷原子频标的闭环锁定,初步获得的短期稳定度指标为3.7×10-12τ-1/2(1~100 s)。     

一种可编程逻辑器件在原子钟频率综合电路中的应用

针对被动型铷原子频标电路模块中由三极管等数量众多的分立元件搭建的9倍选频放大模拟电路和种类繁多的集成电路搭建的5.3125 MHz综合器电路,给出了数字化电路解决方案。在此新方案中,通过使用一种复杂可编程逻辑器件对锁相环进行编程控制,可以实现对10 MHz参考信号18倍频的精确控制;同时,利用该复杂可编程逻辑器件内部"虚拟"的集成电路对10MHz参考信号进行分频变换可以得到5.3125MHz信号。实际使用证明,这种设计方案具备易于集成、调试简单的优点,在替换原有模拟倍频、综合器功能电路后,成功实现整机锁定,各项性能指标均达到或优于原有水平,使整机向数字化、小型化迈出重要的一步。     

一种汽泡型铷原子频标伺服电路中的相位稳定性问题

着重讨论了汽泡型铷原子频标伺服电路中T型选频电路和RC移相电路的相位稳定性,分析了它们的附加相移波动影响整机频率稳定度的机理。为改进原子频标的性能,提出了一种用现场可编程门阵列(FPGA)实现对同步检测参考信号进行数字移相的技术。该基于FPGA的伺服电路的温度附加不稳定度为1×10-12/℃。     

Acceleration of Numerical Integration of the Equations of Motion of Asteroids

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...     

Observations of the intensity of the penumbra of sunspots

Observations of the penumbral intensity of sunspots in 13 wavelength regions are presented. In 4 wavelength regions 54 sunspots are measured. In the other wavelength regions the number of sunspots considered ranges from 3–19.The penumbral intensity alters with position within the spot. This intensity variation is found to be comparable with the change in intensity from one spot to another. The penumbral intensity is found to be independent of spot size in the sample considered.The penumbra model of Kjeldseth Moe and Maltby (1969) with = 0.055 is supported by the measurements.     

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.     

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.     

Graphical representation of periodic motion of the line of nodes of the Moon

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.