GRACE时变信号恢复方法对比分析

针对利用GRACE重力数据反演地表质量变化过程中产生的时变信号削弱和泄露现象,分别采用尺度因子法和迭代恢复法对信号进行恢复,并选用CSR Mascon产品从时间序列变化和空间分布两个角度对两种恢复方法的效果进行对比分析。结果表明:1)尺度因子法虽实现上较为简单,但其计算结果完全依赖于所选的先验模型,当所选模型的可靠性较差时,会影响到GRACE反演结果的可靠性。2)迭代恢复法的恢复过程仅受GRACE原始观测值的约束,能较好地恢复研究区域的长期趋势信号和周期信号,但在部分区域可能存在信号过量恢复的现象。建议采用迭代恢复法进行GRACE时变信号恢复。     

核电工程应用隔震技术的可行性探讨

本文旨在观察和分析有关基底隔震技术在核电工程中应用的相关问题,重点讨论如何将此类已经相当成熟的技术应用于核电这一类十分特殊、十分重要、十分敏感而又十分复杂的工程中.文中指出隔震技术有很多优点,可以整体改进核电工程的安全性和可靠性,有利于促进未来核电厂设计和建造的标准化,缩短建设时间,降低建厂的初始投资和生命周期中的运行...     

河北省黄壁庄水库坝基渗漏单井示踪试验研究

以河北省黄壁庄水库副坝坝基的渗漏塌坑为例，利用“九五”国家重点科技成果推广项目“智能化地下水动态参数测量仪”在天然流场下，测量出水库自然渗漏量地下水的渗透流速流向、垂直向流速流向，每米含水层的渗透系数等工程必须的水文地质参数。确定性地诊断和检测出黄壁水库坝基渗漏隐患出现的具体位置和高程，从而为大坝的渗漏处理和安全处理提供详细的现场测量数据。     

The symmetry energy and incompressibility constrained by the observations of glitching pulsars

We investigate the masses of glitching pulsars in order to constrain their equation of state(EOS). The observations of glitches(sudden jumps in rotational frequency) may provide information on the interior physics of neutron stars. With the assumption that glitches are triggered by superfluid neutrons, the masses of glitching neutron stars can be estimated using observations of maximum glitches.Together with the observations of thermal emission from glitching pulsars Vela and J1709–4429, the slope of symmetry energy and incompressibility of nuclear matter at saturation density can be constrained.The slope of symmetry energy L should be larger than 67 MeV while the lower limit of incompressibility for symmetric nuclear matter K_0 is 215 MeV. We also obtain a relationship between L and K_0:6.173 MeV + 0.283 K_0≤ L ≤ 7.729 MeV + 0.291 K_0. The restricted EOSs are consistent with the observations of 2-solar-mass neutron stars and gravitational waves from a binary neutron star inspiral.     

Constraints on the176Lu cosmochronometer

In an endeavour to resolve reported discrepancies in the value of the branching ratio of¹⁷⁶Lu at astrophysical energies, a new determineation of the¹⁷⁵Lu (nγ)^176mLu capture cross section has been measured as 958 ± 58 mb. This gives a value of the branching ratio of 0.21 ±0.05. This result indicates that some reequilibration of the ground and isomeric states of¹⁷⁶Lu occurs in stellar environments undergoing s-process nucleosynthesis, and confirms that¹⁷⁶Lu is not a reliable cosmochronometer. However the very existence of¹⁷⁶Lu in the solar system implies that the ground state of¹⁷⁶Lu was not completely depopulated, and provides the possibility of using this nuclide as a sensitive thermometer for stellar processes.     

Light‐element abundance variations in globular clusters

Star‐to‐star variations in abundances of the light elements carbon, nitrogen, oxygen, and sodium have been observed in stars of all evolutionary phases in all Galactic globular clusters that have been thoroughly studied. The data available for studying this phenomenon, and the hypotheses as to its origin, have both co‐evolved with observing technology; once high‐resolution spectra were available even for main‐sequence stars in globular clusters, scenarios involving multiple closely spaced stellar generations enriched by feedback from moderate‐ and high‐mass stars began to gain traction in the literature. This paper briefly reviews the observational history of globular cluster abundance inhomogeneities, discusses the presently favored models of their origin, and considers several aspects of this problem that require further study (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Double detonations at the core–envelope boundary in Type Ia supernovae

An off-centre detonation propagating near the interface between a C–O core and a He envelope in a Type Ia supernova explosion is modelled as a steady two-dimensional similarity solution at a plane interface. We assume that in both regions the energy release occurs in an infinitely thin detonation, which produces material in nuclear statistical equilibrium (NSE) in He and in nuclear statistical quasi-equilibrium in C–O. An α-network is then used to determine the effect of the associated rarefaction wave in the C–O on the final abundance of intermediate elements. We find that, although there is a significant effect, the rarefaction is not strong enough to quench the reactions and prevent the C–O from burning to NSE.     

国土资源涉密计算机泄密隐患分析与防范——以费县国土资源局为例

依据信息安全等级保护有关政策和标准,结合费县国土资源局信息化建设中涉密计算机管理工作实际,探讨如何从计算机信息输入和输出2个方面有效预防计算机失窃密。从计算机身份认证与访问控制、网口、UBS口电磁辐射,办公设备5个方面分析泄密隐患,并提出相应的应对措施,强调了在国土资源系统涉密计算机管理方面要加强保密意识,提高防范技能。     

A Study on the Abundance Distribution of Heavy Elements in Metal-poor Stars by the Parameterization Method

Based on a large amount of observed data of element abundances in metal-poor stars, taking the abundance distribution of heavy elements in the solar system as a standard, and selecting Sr, Ba and Eu as the typical elements of the three nucleosynthetic processes in metal-poor stars, namely the weak sprocess, main s-process and r-process, we have studied the contributions of the three kinds of neutron-capture processes to the abundance distribution of heavy elements in metal-poor stars, with the parameterization method. It is found that the higher the metal abundance, the greater the contributions of the weak s-process and the chief s-process to the abundances of lighter neutron-capture elements. The heavier neutron-capture elements are mainly produced by the r-process and the chief s-process; and that at low metallicity, the abundances of heavy neutron-capture elements are mainly produced by the r-process. In the early Galaxy, the weak s-process has almost no contribution to the element abundance.