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。     

被动式铷原子频标近十余年来发展概况

本文综述了近１０多年来被动式铷原子频标的发展概况．     

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。     

上海光机所小喷泉铷钟的设计和进展

对上海光机所正在研制的小喷泉铷钟及目前正在进行的工作作了介绍.该小喷泉铷钟吸收了原子喷泉的许多新技术,采用紧凑的结构设计,加入空心光束以提高探测原子数.预期该喷泉的准确度为10-14,短、长稳分别为10-13和10-15,信噪比为103.实验室完成了冷原子物理的准备工作,已经俘获冷原子团.     

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)。     

被动型原子频率标准体系内优势组合的研究

提出了被动型原子频率标准体系内优势组合的建议.扼要地介绍了以汽泡型铷原子频率标准为背景的体系内优势组合的研究情况及其初步结果.     

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。     

上海天文台大铯钟的研究与现状

本文介绍了上海天文台长铯束管束光学系统改进扫得的７条拉比台跃迁曲线和７条莱姆塞跃过曲线及连续开机四个月得到的数据．     

High resolution spectroscopy of two young active late type stars within 20 parsecs of the Sun

We present high-resolution optical echell spectroscopy of HIP 544 and HIP 46843, two nearby solar like stars. The discovery of these young stars at such a close distance to the Sun is really a surprising phenomenon. It will help us to have a better understanding of the structure and evolutionary history of the Milky Way. The radial ve-locities (RV) of HIP 544 and HIP 46843 are measured to be -6.88±0.13km s-1 and 8.30±0.16km s-1, respectively, which are more accurate than before. The equivalent widths (EW) of the Li I 6707.8 A absorption line of HIP 544 and HIP 46843 are mea-sured to be 110±5mA and 195±5mA respectively. Based on these properties, HIP 544 is estimated to be 100-800Myr old and HIP 46843 30-100Myr old using three relatively creditable methods.     

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)。     

On the thermal structure of Uranus

Uranus has an effective temperature close to the solar equilibrium value and undoubtedly a thermal inversion of at least 140 K at a pressure of ～3 dyncm^?2. With the inversion and the thermal opacity provided by a HeH₂ mixture in a ratio close to solar abundance, acceptable agreement can be achieved with the available infrared observations. The cause of the inversion is, however, uncertain. The use of the HeH₂ opacity for Uranus is justified by the excellent agreement of the frequency variation of that opacity with the thermal spectrum of Jupiter.     

Radiation spectrum of a magnetized supercritical accretion disc with thermal conduction

we examine the effect of thermal conduction on the observational properties of a super critical hot magnetized flow. We obtained self-similar solution of a magnetized disc when the thermal conduction plays an important role. Follow of our first paper (Ghasemnezhad et al. in Astrophys. J. 750, 2012 (hereafter GKA12)) we have extended our solution on the observational appearance of the disc to show how physical condition such as thermal conduction, viscosity, and advection will change the observed luminosity of the disc, Continuous spectra and surface temperature of such discs was plotted. We apply the present model to black-hole X-ray binary LMC X-3 and narrow-line seyfert 1 galaxies, which are supposed to be under critical accretion rate. Our results show clearly that the surface temperature is strongly depends on the thermal conduction, the magnetic field and advection parameter. However we see that thermal conduction acts to oppose the temperature gradient as we expect and observed luminosity of the disc will reduce when thermal conduction is high. We have shown that in this model the spectra of critical accretion flows strongly depends on the inclination angle.     

Isotopes of rubidium in the Sun

Photoelectric measurements of photospheric velocity fields have been carried out with the Sacramento Peak Doppler Zeeman Analyzer. Emphasis was given to long periods and low spatial wavenumbers in deep photospheric layers, where the 5-min oscillations are less dominant.Multiple or double peaks cannot be detected in power spectra of the 5-min oscillations, provided that a sufficient number of physically independent points on the solar surface are observed.The most frequent wave-numbers in the spectra of 5-min oscillations (as well as of the low frequency field) agree with those derived from a model assuming statistically independent oscillators of 10 to 20 diameter. These two velocity fields are anti-correlated spatially.Kinetic power in the 20-to-50-min range of periods is closely linked to brightness changes in the same layer, an increase of brightness lagging about 250 sec behind rising motion. Granules can be excluded as a possible source for the appearance of low frequency flow patterns. Different explanations are suggested.On leave from Fraunhofer Institut, Freiburg, Germany.     

Magnetic fields and thermal structure of solar plasmas

The connection between the magnetic field geometry and the thermal properties of solar coronal structures is investigated. Gravitational effects, that can modify the spatial dependence of the thermodynamical quantities, but have no influence on the plasma-field interaction, are omitted to simplify the problem. A series of two-dimensional models is constructed, in which a strong coupling between the magnetic field shear and the thermal structure of the loop is clearly pointed out.It is shown how it is possible to deduce detailed information on the small scale magnetic structure by the use of measurement of purely thermodynamical quantities. Similarly information on the spatial dependence of the energy deposition function can also be obtained.     

Energetics and thermal structure of the middle atmosphere

A study of a large number of temperature measurements in the middle atmosphere shows a much more complex thermal structure of this region than described in the U.S. Standard Atmosphere, 1976. The mesopause height which is generally assumed to be at 80 km varies between 70–100 km, often with two minima in temperature at about 70 and 100 km and a maximum between 80–85 km. By solving the energy balance equation and the equations of continuity, the physical significance of the observed thermal structure is discussed in terms of the energetics of the various regions of the middle atmosphere. It is shown that the solar u.v. radiation plays a major role only in the energy budget of the stratosphere and the lower thermosphere. The energetics of the mesosphere is primarily influenced by the dissipation of eddy energy. The temperature in this region is a good indicator of the eddy diffusivity and can be used in deriving the eddy diffusion coefficient.     

Multidimensional thermal structure of magnetized neutron star envelopes

Recently launched X-ray telescopes have discovered several candidate isolated neutron stars. The thermal radiation from these objects may potentially constrain our understanding of nuclear physics in a realm inaccessible to terrestrial experiments. To translate the observed fluxes from neutron stars into constraints, one needs precise calculations of the heat transfer through the thin insulating envelopes of neutron stars. We describe models of the thermal structure of the envelopes of neutron stars with magnetic fields up to 10¹⁴ G. Unlike earlier work, we infer the properties of envelope models in two dimensions and precisely account for the quantization of the electron phase-space. Both dipole and uniformly magnetized envelopes are considered.     

Mercury: Internal structure and thermal evolution

Astronomical observations and cosmochemical calculations suggest that the planet Mercury may be composed of materials which condensed at relatively high temperatures in the primitive solar nebula and may have a basaltic crust similar to parts of the moon. These findings, plus the long standing inference that Mercury is much richer in metallic iron than the other terrestrial planets, provide important constraints which we apply to models of the thermal evolution and density structure of the planet. The thermal history calculations include explicitly the differing thermal properties of iron and silicates and account for core segregation, melting and differentiation of heat sources, and simulated convection during melting. If the U and Th abundances of Mercury are taken from the cosmochemical model of Lewis, then the planet would have fully differentiated a metal core from the silicate mantle for all likely initial temperature distributions and heat transfer properties. Density distributions for the planet are calculated from the mean density and estimates of the present-day temperature. For the fully differentiated model, the moment of inertia C/MR² is 0.325 (J₂=0.302×10^?6). For models with lower heat source abundances, the planet may not yet have differentiated. The density profiles for such models give C/MR²=0.394 (J₂=0.487×10^?6). These results should be useful for preliminary interpretation of the Mariner 10 measurements of Mercury's gravitational field.