论新型城镇化背景下的人的现代化

城镇化是现代化的必由之路,尽管在发展的硬指标上新型城镇化的任务还比较艰巨,但也不能因此而忽视城镇化的软指标,即人的现代化.人的现代化的核心在于文化观念的转换,传统文化的观念系统存在着诸多影响现代化发展的因素.开展持久的关于现代文化意识的启蒙教育,在政治、经济制度领域实现彻底的现代转型,是实现人的现代化的关键.     

学习型组织理论与民航人力资源开发

建立学习型组织是知识经济时代发展的要求。民航人力资源的开发对民航行业的发展起着巨大的推动作用。本文试图从学习型组织的提出、学习型组织的内涵、创建学习型组织的意义等方面,结合我国民航的具体情况,阐明如何将学习型组织的理念引入民航人力资源开发以及学习型组织的理念引入对民航人力资源开发具有深远而重大的意义。一什么是学习型组织?所谓学习型组织,是指通过培养组织的学习气氛、充分发挥员工的创造性而建立起来的一种有机的、柔性的、扁平的、人性的、持续发展的组织。它具有如下几个要素:拥有终身学习的理论和机制;建有多元回…     

马克思交往理论的革命性意义——兼评"主体际"交往观

马克思的交往理论不仅揭示了人的活动的前提,而且揭示了前提本身的否定方面,即"非人的"社会关系的存在,亦即人的实践活动的批判维度,从而实现了对抽象的"人"及其关系的彻底颠覆。而主体际交往观所规定的主体本质上是虚幻的。     

PDM产品IMAN及其工程化实施

在总结PDM系统实施经验的基础上,概括性地介绍了PDM系统,特别是IMAN的主要特点和功能,并简要描述了实施PDM系统的主要过程、所建立的系统概况以及下一步的工作内容。文章的重点在于总结PDM系统实施的经验,包括管理制度的科学性、目标的长远性及实施的阶段性、效益的长远性、系统应用的强制性和实施工作的合作性等。旨在对PDM及其系统的实施有一初步的了解。     

精品欣赏

最美丽的放牧是心灵的放牧,置身于草原才能品食丰饶的思想,放眼于天际才能知觉无垠的动力。 看似孤独的也许并不孤独。 城市的人,应学会为自己创造偶尔的孤独,给自己一片放牧心灵的平静的草原。当面对碧蓝与葱翠交汇的地平线,可以只听到风吹过的声音。这个时候,在宁静的天地间细细地体会,慢慢地梳理,孤独,会成为一种内容丰富的享受。 看似简单的也许并不简单。 城市的人,应学会让自己回归偶尔的简单,带自己到一片可以放牧心灵的平静的草原。当真正面对这碧蓝与葱翠交汇的地平线,当耳际真正只听到风吹过的声音。这个时候,在宁静的天地间…     

浅谈“五度理论”在客舱服务中的应用

面对成千上万的旅客.不同的职业、不同的年龄、不同的文化背景、不同的社会习惯和不同的想法.有缘聚集在小小的客舱,自然也有着不同的服务需求。如何在旅客最需要的时候出现在他们面前,为他们提供需要的服务,需要的是乘务员敏锐的慧眼和灵活的反应能力。     

独立指数分布期望参数的Г极小极大估计

在参数的部分先验信息已知的条件下所获得的Г极小极大估计是一种介于有确定的先验分布函数的Bayes估计和无先验信息的极小极大估计之间的估计方法，因而更切合实际。以往的研究对二项分布参数的线性组合及负二项分布的参数在某些限制条件下的Г极小极大估计做了讨论。本文给出了独立指数分布的期望参数在一般的先验矩限制下的Г极小极大估计，同时讨论了两种特殊情况，即给出了在仅有先验二阶矩限制下的以及有确定的先验一阶矩和二阶矩限制下的指数分布的期望参数的Г极小极大估计。     

发动机各种融资方法介绍

一、发动机融资的概述在激烈竞争的航空市场中,航空公司应用金融的能力——财务管理的能力已变得越来越重要。如何筹措资金,规划与使用资金将直接影响到一个航空公司的生存与发展。航空融资的各种方法为航空公司提供了多种多样的筹措资金与使用资金的渠道。发动机的融资是航空融资的一个组成部分,它与飞机的融资有相似的地方也有它独特的地方。与飞机的融资相比,它的特点是(1)数额较小(2)方法更多样(3)容易操作。因此,发动机的融资已得到越来越多的航空公司的重视和应用。     

精品欣赏

云冈,凡有幸伫立于它的脚下仰望,必为它的壮美而屏息。当年的繁荣,何样的强盛,数千年后仍能在每一尊佛像的吐纳中被感受。生动的表情,完美的体态,各色的祥纹,如何也让人难以置信,这些宏大却极精巧的石像是几世几代的祖辈们仅用双手不懈凿刻而出。云冈,令人目不暇接的宝藏。头顶,左右,足下;染色的,失色的,原色的;坐者,立者,舞者;数万计的人们不断匆匆走过啧啧赞叹。而云冈的佛,身披霓裟,静静望岁月更替,恬然观世事变迁。秋,金灿灿的秋,内蒙古坝上的金灿灿的秋,这秋色没有丝毫飘零的忧戚,完全尽力溢扬着乐章中最华彩最贵族的气度。白的枝干明…     

物理学圣地——完美诠释哥本哈根精神

高度的智力活动、大胆的涉险精神、深奥的研究内容与快活的乐天主义"哥本哈根精神"是由20世纪初丹麦的著名科学家尼耳斯·玻尔所提出的,玻尔的挚友、著名物理学家罗森菲耳德为"哥本哈根精神"下的定义是:完全自由的判断与讨论的美德。不仅如此,玻尔倡导的"平等、自由讨论和相互紧密地合作的浓厚的学术气氛",已经成为放之四海皆宜的团队工作准则。只有在他积极营造的那种"使人感到繁忙、激动、活泼、欢快、无拘无束、和蔼可亲"的气氛中,"工作者"才会是美丽的。"哥本哈根精神"完美地诠释了团队精神,它以一个成功者的姿态存在:相互的沟通配合和较为明显的责任分担,需要更为统一的思想,对目标的认同和个人牺牲。     

Non-BBN Constraints on the Key Cosmological Parameters

Since the baryon-to-photon ratio 10 is in some doubt at present, we ignore the constraints on 10 from big bang nucleosynthesis (BBN) and fit the three key cosmological parameters (h, M, 10) to four other observational constraints: Hubble parameter (ho), age of the universe (to), cluster gas (baryon) fraction (fo fGh3/2), and effective shape parameter (o). We consider open and flat CDM models and flat CDM models, testing goodness of fit and drawing confidence regions by the 2 method. CDM models with M = 1 (SCDM models) are accepted only because we allow a large error on ho, permitting h < 0.5. Open CDM models are accepted only for _M 0.4. CDM models give similar results. In all of these models, large 10 ( 6) is favored strongly over small 10 ( 2), supporting reports of low deuterium abundances on some QSO lines of sight, and suggesting that observational determinations of primordial 4He may be contaminated by systematic errors. Only if we drop the crucial o constraint are much lower values of M and 10 permitted.     

Anomalous Cosmic Rays and Solar Modulation

We review aspects of anomalous cosmic rays (ACRs) that bear on the solar modulation of energetic particles in the heliosphere. We show that the latitudinal and radial gradients of these particles exhibit a 22-year periodicity in concert with the reversal of the Sun's magnetic field. The power-law index of the low energy portion of the energy spectrum of ACRs at the shock in 1996 appears to be -1.3, suggesting that the strength of the solar wind termination shock at the helioequatorial plane is relatively weak, with s 2.8. The rigidity dependence of the perpendicular interplanetary mean free path in the outer heliosphere for particles with rigidities between 0.2 and 0.7 GV varies approximately as R2, where R is particle rigidity. There is evidence that ACR oxygen is primarily multiply charged above 20 MeV/nuc and primarily singly-charged below 16 MeV/nuc. The location of the termination shock was at 65 AU in 1987 and 85 AU in 1994.     

Observed Densities in the Universe

Baryons observed in Ly absorbers contribute to the density parameter 0 by bar 0.06 in close agreement with the value of 0.06 from primordial nucleosynthesis (H0=55 km s-1 Mpc-1, = 0 assumed throughout). A number of methods are known to measure 0 from density fluctuations; bound structures tend to yield lower values (m 0.2-0.4), field galaxies over large scales higher, but still undercritical values (m 0.6 ± 0.2). The best compromise value is 0 0.5, but the present methods are blind to diffusely distributed, exotic matter which still could make 0 = 1. A satisfactory solution of 0 (and ) will only come from a fundamental cosmological test (e.g. the Hubble diagram of [evolution-corrected] supernovae type Ia) in combination with the CMB fluctuation spectrum.     

Primordial Helium and ΔY/ΔZ from H II Regions and from Fine Structure in the Main Sequence Based on Hipparcos Parallaxes

The primordial helium abundance YP is important for cosmology and the ratio Y/Z of the changes relative to primordial abundances constrains models of stellar evolution. While the most accurate estimates of YP come from emission lines in extragalactic H II regions, they involve an extrapolation to zero metallicity which itself is closely tied up with the slope Y/Z. Recently certain systematic effects have come to light in this exercise which make it useful to have an independent estimate of Y/Z from fine structure in the main sequence of nearby stars. We derive such an estimate from Hipparcos data for stars with Z Z and find values between 2 and 3, which are consistent with stellar models, but still have a large uncertainty.     

The Edison infrared space observatory

For five years, theEdison program has had the goal of developing new designs for infrared space observatories which will break the cost curve by permitting more capable missions at lower cost. Most notably, this has produced a series of models for purely radiative and radiative/mechanical (hybrid) cooling which do not use cryogens and optical designs which are not constrained by the coolant tanks. Purely radiatively-cooled models achieve equilibrium temperatures as low as about 20 K at a distance of 1 AU from the sun. More advancedEdison designs include mechanical cooling systems attached to the telescope assembly which lower the optical system temperature to 5 K or less. Via these designs, near-cryogenic temperatures appear achievable without the limitations of cryogenic cooling. OneEdison model has been proposed to the European Space Agency as the next generation infrared space observatory and is presently under consideration as a candidate ESA Cornerstone mission. The basic design is also the starting point for elements of future infrared space interferometers.     

The synthesis of helium and CNO isotopes in massive stars

We present helium and CNO isotopic yields for massive mass-losing stars in the initial mass range 15M M _i 50M . We investigate their dependence on assumptions about mass loss rates, internal mixing processes, and metallicity, and specify the contributions from stellar winds and from supernova ejecta.     

Nonlinear theory of the two-point correlation function

We consider the influence of the nonlinear stage of gravitational instability on the two-point correlation functions of gravitationally bound objects. Based on the theory of nonlinear gravitational contraction of a single density peak of dissipationless matter (Gurevich and Zybin, 1988a,b; 1990) we develop a method for calculating the two-point correlation functions of different objects of any mass. The method works good in the region of strong correlations and can be easily extended to calculate higher correlation functions. We show that the main contribution to the correlation function _i in the region of strong correlations _i 1 is made by pair systems located outside large clusters of objects. In this region the shape of _i is determined only by the nonlinear dynamics of gravitational contraction of dissipationless matter and has the form _i C ^–, where 1.8 is a universal parameter.     

Some results of ionospheric investigations by means of coherent radiowaves emitted by satellites

In this paper we discuss theoretical expressions, determining the difference of Doppler shifts of various coherent radiowave frequencies emitted by a radiator moving in the ionosphere or interplanetary medium. The rotating Doppler effect (Faraday effect) caused by the Doppler shifts ±H of the ordinary and extraordinary waves is also considered. In a three-dimensional inhomogeneous ionosphere, stationary in time (N/t = 0), is determined in the general case, by an equation with three variables. The equation for proper depends only on the local value of the electron concentration N _c around the radiator and on integral values, determining, by means of additional calculations, the angle of refraction or its components, the horizontal gradients of electron concentration N/x and N/y, and in some cases, the integral electron concentration ₀ ^zcN dz. We describe the analysis of the measurements, made with the satellites Cosmos I, II and partially XI, assuming that N/t = N/y = 0, with a two variables equation. The expected errors are considered. The results coincide well for different points (Moscow, The Crimea, Sverdlovsk) and thus agree with the measurements of _H and with height-frequency ionospheric characteristics. The curve giving electron concentration versus height N (z) in the outer ionosphere (above the maximum of F2), shows a new maximum higher than the main maximum of the ionosphere N _MF2 at 120–140 km. At this maximum the value of N (z) is (0.9–0.95) N _MF2. The new data on the large-scale horizontal inhomogeneities of the ionosphere, exceed the previous ones by about a factor 10. By means of the irregular variations of the spectrum W() of the inhomogenous formation is determined. Three unknown constant maxima with values 16 to 18 km, 28 to 32 km and 100 to 120 km are found. The spectrum W () mainly characterizes the local properties of the ionosphere along the orbit of the satellite.     

Electron coronal density irregularity\overline {n^2 } /(\bar n)^2 from measurements of K-coronal and lyman lines brightnesses

We propose a technique to derive the coronal density irregularity factor , wheren is the electron density. The absolute photometric comparison between the intensity of UV lines and the white-light K-coronal polarized brightness (pB) provides an unique constraint on the inhomogeneity of the corona. The ratio of the measured H I Lyman (Ly-) line intensity to the resonant-scattering dominated H I Lyman (Ly-) intensity can be used to extract the collisonal component of the Ly-. This component yields an estimate of . The quantity is then obtained from white-light K-coronal measurements. The use of lines of the same atomic species minimizes the effects due to outflow velocities (i.e., Doppler dimming), and reduces the errors introduced by the uncertainties in the ionization balance, the atomic parameters, and the solar abundances. The UVCS/SOHO unique capability of performing cotemporal and cospatial measurements of the Ly- and Ly- lines, and ofpB makes this instrument ideal for implementing this technique.     

Detection limits in the far infrared

The advent of far infrared arrays will change fundamentally the means of analyzing observations in this spectral region. Sources much fainter than traditional confusion limits will be extracted from images by using computer algorithms similar to CLEAN or DAOPHOT. We have conducted numerical experiments to evaluate these techniques and show that they will permit long integrations (10,000 sec at 60 m, 200 sec at 100 m) to achieve nearly photon-background-limited performance and hence very deep detection limits. The dominant noise sources—photon noise, confusion by distant galaxies, and confusion by IR cirrus — scale with nearly the same power of the telescope aperture. As a result, the integration times required to reach confusion limits are nearly aperture-independent.