Nature of dark energy and polarization measurements

High sensitivity polarization measures, on wide angular scales, together with data on anisotropy, can be used to fix DE parameters. In this paper, first of all, we aim to determine the sensitivity needed to provide significant limits. Our analysis puts in evidence that there is a class of DE models that polarization measures can possibly exclude soon. This class includes models with DE due to a Ratra–Peebles (RP) potential. Using a likelihood analysis, we show that it is possible to distinguish RP models from ΛCDM and other dynamical DE models, already with the sensitivity of experiments like SPOrt or WMAP, thanks to their negative TE correlation at low-l, when the optical depth τ is sufficiently large. On the contrary, fixing the energy scale Λ for RP potentials or distinguishing between ΛCDM and other DE potentials requires a much lower pixel noise, that no planned polarization experiment will achieve. While reviewing this paper after the referee report, the first-year WMAP data were released. WMAP finds large positive anisotropy–polarization correlations at low l; this apparently excludes DE models with RP potentials.     

Cosmology of Vacuum

Shortly the vacuum component of the Universe from the geometry point of view and from the point of view of the standard model of physics of elementary particles is discussed. Some arguments are given to the calculated value of the cosmological constant (Zel’dovich’s approximation). A new component of space vacuum (the gravitational vacuum condensate) is involved the production of which has fixed time in our Universe. Also the phenomenon of vacuum selforganization must be included in physical consideration of the Universe evolution.     

钢箱梁典型病害分析及其检测与维护技术研究

基于对我国钢箱梁桥的钢箱梁病害调查,总结出我国钢箱梁典型病害的类型,分析各种钢箱梁典型病害产生的机理及导致其破坏的原因,提出了钢箱梁病害的日常检测与维护技术。针对钢箱梁的涂装劣化、钢材腐蚀、结构性损伤等病害,给出了日常检测与维护的主要项目,介绍了人工目视检测、超声波检测、磁粉检测及涡流检测等主要的检测方法的工作原理、优缺点和适用范围。     

The expansion field: the value of <Emphasis Type="Italic">H</Emphasis><Subscript>0</Subscript>

Any calibration of the present value of the Hubble constant (H ₀) requires recession velocities and distances of galaxies. While the conversion of observed velocities into true recession velocities has only a small effect on the result, the derivation of unbiased distances which rest on a solid zero point and cover a useful range of about 4–30 Mpc is crucial. A list of 279 such galaxy distances within v < 2,000 km s⁻¹ is given which are derived from the tip of the red-giant branch (TRGB), from Cepheids, and/or from supernovae of type Ia (SNe Ia). Their random errors are not more than 0.15 mag as shown by intercomparison. They trace a linear expansion field within narrow margins, supported also by external evidence, from v = 250 to at least 2,000 km s⁻¹. Additional 62 distant SNe Ia confirm the linearity to at least 20,000 km s⁻¹. The dispersion about the Hubble line is dominated by random peculiar velocities, amounting locally to <100 km s⁻¹ but increasing outwards. Due to the linearity of the expansion field the Hubble constant H ₀ can be found at any distance >4.5 Mpc. RR Lyr star-calibrated TRGB distances of 78 galaxies above this limit give H ₀ = 63.0 ± 1.6 at an effective distance of 6 Mpc. They compensate the effect of peculiar motions by their large number. Support for this result comes from 28 independently calibrated Cepheids that give H ₀ = 63.4 ± 1.7 at 15 Mpc. This agrees also with the large-scale value of H ₀ = 61.2 ± 0.5 from the distant, Cepheid-calibrated SNe Ia. A mean value of H ₀ = 62.3 ± 1.3 is adopted. Because the value depends on two independent zero points of the distance scale its systematic error is estimated to be 6%. Other determinations of H ₀ are discussed. They either conform with the quoted value (e.g. line width data of spirals or the D _n −σ method of E galaxies) or are judged to be inconclusive. Typical errors of H ₀ come from the use of a universal, yet unjustified P–L relation of Cepheids, the neglect of selection bias in magnitude-limited samples, or they are inherent to the adopted models.     

山西省原平市神经管畸形时空分析

神经管畸形是发生于中枢神经系统的一种先天性异常,在所有的新生儿出生缺陷中所占比例较高。在我国,作为矿业大省的山西,神经管畸形最为严重,原平市又是山西省出生缺陷的高发市之一。本文利用山西省原平市2007-2012年的神经管畸形病例资料,基于贝叶斯理论的时空建模方法,综合考虑时间组分和时空交互组分,对神经管畸形的时空规律进行研究。研究识别了研究区内疾病发生的热点区域、冷点区域、温点区域,并对这些区域随时间的变化趋势进行了分析。研究发现,原平市18个乡镇中有1个热点区域、17个温点区域,整体发病率较高;原平市神经管畸形整体上随时间变化呈缓慢下降趋势,但该趋势并不明显;1个热点区域疾病风险下降趋势慢于整体趋势,4个温点区域疾病风险下降趋势快于整体趋势,13个温点区域疾病风险时间变化趋势与整体趋势趋同。本文识别了山西省原平市神经管畸形发病的时间趋势和空间趋势,可以揭示神经管畸形潜在的风险因子或控制措施供进一步流行病学研究,也可以为公共卫生部门制定及时有效的防治控制措施提供一定的科学参考。     

均匀黏弹性地基中现浇X形桩低应变动测响应数值模拟

建立现浇X形桩(XCC桩)桩-土体系三维有限元模型,对XCC桩低应变检测动力响应进行数值模拟,得到完整桩和缺陷桩的桩顶速度响应结果,并分析完整桩及缺陷XCC桩桩顶速度响应特性及规律。计算结果表明:XCC桩低应变瞬态动测时桩顶速度响应存在明显的三维效应,桩心(激振点)附近点的入射波峰值较大,且到达时间较早;距离桩心越远点的入射波峰到达时间越滞后,入射波峰值从桩心到尖角边界先减小后增大。桩顶距桩心距离相同的环向上各点的入射波和反射波区别不大,而各点所受的高频干扰情况并不相同。变模量桩的入射波和完整桩相同,反射波峰值较完整桩小,反射波峰对应时间较完整桩滞后。局部缺陷桩桩顶距桩心距离相同环向各点的第一个缺陷反射波有微小差别,而第二个缺陷反射波有较大差别。     

基桩桩身完整性检测中的影响因素浅析

近年来,桩基础的广泛应用带动了检测技术的进一步发展,基桩检测技术也越来越受到人们的重视.本文从反射波理论出发介绍了反射波法的基本原理,指出了桩身完整性的判定标准,并系统的分析了基桩检测中的多种影响因素.本文通过分析和总结,指出了反射法测桩存在的不足,并提出了相应的注意事项及解决办法.     

基于贝叶斯理论的灌注桩多个缺陷统计特性分析

由于施工技术水平、岩土工程条件等不确定性因素的影响,基桩中经常出现各种缺陷。为此,提出了基于贝叶斯理论的灌注桩多个缺陷统计特性的分析方法。在考虑钻芯法检测不确定性的基础上,采用泊松分布模型模拟基桩中多个缺陷的出现概率,推导了缺陷平均出现率后验分布的计算公式。提出了估计缺陷尺寸修正的贝叶斯抽样方法,给出了评价钻芯法检测概率的方法。算例分析表明,钻芯法的检测概率对准确地估计缺陷平均出现率有明显的影响,如果不考虑检测不确定性因素的影响,缺陷平均出现率将被低估。随着检测到缺陷数目的增加,更新的缺陷平均出现率的均值逐渐增加,更新的变异系数逐渐减小。此外,先验的信息能够有效地减小缺陷平均出现率和缺陷尺寸估计的不确定性。     

岩石颗粒边界缺陷分布的概率模型

本文应用概率理论，研究了颗粒结构材料初始边界缺陷的分布问题，提出了一个概率模型，认为材料中的初始边界缺陷不会全部都是孤立地分布，总会有二个、三个或更多个基本边界缺陷相连在一起组成缺陷族的情况，缺陷簇的个数的数学期望值相对于其尺度符合指数衰减强度，衰减指数与缺陷发生的概率及边界网络的相似维数有关。推导得出了颗粒结构材料的拉伸强度与试样尺度、颗粒尺度及缺陷发生概率之间的关系，从理论上论证了材料强度的尺     

Cosmic thermal neutrino background: Can it be detected?

The detection of the Cosmic Thermal Neutrino Background (CTNB) would provide the “cleanest” evidence for the hot big bang model of the early Universe. I discuss some recent thoughts on the possibility of detecting the CTNB (especially if neutrinos have a small mass of ~ few eV) by looking for certain CTNB-induced features in the extremely high energy (E ≳ 10²⁰ eV) cosmic neutrino spectrum that may become measurable in the future by some of the large-area extensive air-shower detectors being built for detecting extremely high energy cosmic rays. NAS/NRC Senior Research Associate on sabbatical leave from Indian Institute of Astrophysics, Bangalore 560 034, India.