Numerical Simulations of the Warm-Hot Intergalactic Medium

In this paper we review the current predictions of numerical simulations for the origin and observability of the warm hot intergalactic medium (WHIM), the diffuse gas that contains up to 50 per cent of the baryons at z∼0. During structure formation, gravitational accretion shocks emerging from collapsing regions gradually heat the intergalactic medium (IGM) to temperatures in the range T∼10⁵–10⁷ K. The WHIM is predicted to radiate most of its energy in the ultraviolet (UV) and X-ray bands and to contribute a significant fraction of the soft X-ray background emission. While O vi and C iv absorption systems arising in the cooler fraction of the WHIM with T∼10⁵–10^5.5 K are seen in FUSE and Hubble Space Telescope observations, models agree that current X-ray telescopes such as Chandra and XMM-Newton do not have enough sensitivity to detect the hotter WHIM. However, future missions such as Constellation-X and XEUS might be able to detect both emission lines and absorption systems from highly ionised atoms such as O vii, O viii and Fe xvii.     

Equilibration Processes in the Warm-Hot Intergalactic Medium

The Warm-Hot Intergalactic Medium (WHIM) is thought to contribute about 40–50% to the baryonic budget at the present evolution stage of the universe. The observed large scale structure is likely to be due to gravitational growth of density fluctuations in the post-inflation era. The evolving cosmic web is governed by non-linear gravitational growth of the initially weak density fluctuations in the dark energy dominated cosmology. Non-linear structure formation, accretion and merging processes, star forming and AGN activity produce gas shocks in the WHIM. Shock waves are converting a fraction of the gravitation power to thermal and non-thermal emission of baryonic/leptonic matter. They provide the most likely way to power the luminous matter in the WHIM. The plasma shocks in the WHIM are expected to be collisionless. Collisionless shocks produce a highly non-equilibrium state with anisotropic temperatures and a large differences in ion and electron temperatures. We discuss the ion and electron heating by the collisionless shocks and then review the plasma processes responsible for the Coulomb equilibration and collisional ionisation equilibrium of oxygen ions in the WHIM. MHD-turbulence produced by the strong collisionless shocks could provide a sizeable non-thermal contribution to the observed Doppler parameter of the UV line spectra of the WHIM.     

Clusters of Galaxies: Setting the Stage

Clusters of galaxies are self-gravitating systems of mass ∼10¹⁴–10¹⁵ h ⁻¹ M_⊙ and size ∼1–3h ⁻¹ Mpc. Their mass budget consists of dark matter (∼80%, on average), hot diffuse intracluster plasma (≲20%) and a small fraction of stars, dust, and cold gas, mostly locked in galaxies. In most clusters, scaling relations between their properties, like mass, galaxy velocity dispersion, X-ray luminosity and temperature, testify that the cluster components are in approximate dynamical equilibrium within the cluster gravitational potential well. However, spatially inhomogeneous thermal and non-thermal emission of the intracluster medium (ICM), observed in some clusters in the X-ray and radio bands, and the kinematic and morphological segregation of galaxies are a signature of non-gravitational processes, ongoing cluster merging and interactions. Both the fraction of clusters with these features, and the correlation between the dynamical and morphological properties of irregular clusters and the surrounding large-scale structure increase with redshift. In the current bottom-up scenario for the formation of cosmic structure, where tiny fluctuations of the otherwise homogeneous primordial density field are amplified by gravity, clusters are the most massive nodes of the filamentary large-scale structure of the cosmic web and form by anisotropic and episodic accretion of mass, in agreement with most of the observational evidence. In this model of the universe dominated by cold dark matter, at the present time most baryons are expected to be in a diffuse component rather than in stars and galaxies; moreover, ∼50% of this diffuse component has temperature ∼0.01–1 keV and permeates the filamentary distribution of the dark matter. The temperature of this Warm-Hot Intergalactic Medium (WHIM) increases with the local density and its search in the outer regions of clusters and lower density regions has been the quest of much recent observational effort. Over the last thirty years, an impressive coherent picture of the formation and evolution of cosmic structures has emerged from the intense interplay between observations, theory and numerical experiments. Future efforts will continue to test whether this picture keeps being valid, needs corrections or suffers dramatic failures in its predictive power.     

On the Measurements of D/H in QSO Absorption Systems Closing in on the primordial abundance of deuterium

We present our measurements of the deuterium to hydrogen ratio (D/H) in QSO absorption systems, which give D/H = 3.40 ± 0.25 × 10-5 based on analysis of four independent systems. We discuss the properties of two systems which provide the strongest constraints on D/H. We outline the systematic effects involved in measurements of D/H and introduce a sophisticated method of analysis which properly accounts for these effects.     

Future Instrumentation for the Study of the Warm-Hot Intergalactic Medium

We briefly review capabilities and requirements for future instrumentation in UV- and X-ray astronomy that can contribute to advancing our understanding of the diffuse, highly ionised intergalactic medium.     

Observations of Metals in the Intra-Cluster Medium

Because of their deep gravitational potential wells, clusters of galaxies retain all the metals produced by the stellar populations of the member galaxies. Most of these metals reside in the hot plasma which dominates the baryon content of clusters. This makes them excellent laboratories for the study of the nucleosynthesis and chemical enrichment history of the Universe. Here we review the history, current possibilities and limitations of the abundance studies, and the present observational status of X-ray measurements of the chemical composition of the intra-cluster medium. We summarise the latest progress in using the abundance patterns in clusters to put constraints on theoretical models of supernovae and we show how cluster abundances provide new insights into the star-formation history of the Universe.     

Observations of Extended Radio Emission in Clusters

We review observations of extended regions of radio emission in clusters; these include diffuse emission in ‘relics’, and the large central regions commonly referred to as ‘halos’. The spectral observations, as well as Faraday rotation measurements of background and cluster radio sources, provide the main evidence for large-scale intracluster magnetic fields and significant densities of relativistic electrons. Implications from these observations on acceleration mechanisms of these electrons are reviewed, including turbulent and shock acceleration, and also the origin of some of the electrons in collisions of relativistic protons by ambient protons in the (thermal) gas. Improved knowledge of non-thermal phenomena in clusters requires more extensive and detailed radio measurements; we briefly review prospects for future observations.     

Clusters of Galaxies: Beyond the Thermal View

We present the work of an international team at the International Space Science Institute (ISSI) in Bern that worked together to review the current observational and theoretical status of the non-virialised X-ray emission components in clusters of galaxies. The subject is important for the study of large-scale hierarchical structure formation and to shed light on the “missing baryon” problem. The topics of the team work include thermal emission and absorption from the warm-hot intergalactic medium, non-thermal X-ray emission in clusters of galaxies, physical processes and chemical enrichment of this medium and clusters of galaxies, and the relationship between all these processes. One of the main goals of the team is to write and discuss a series of review papers on this subject. These reviews are intended as introductory text and reference for scientists wishing to work actively in this field. The team consists of sixteen experts in observations, theory and numerical simulations.     

Non-Thermal Processes in Cosmological Simulations

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.     

Astrophysics in 2006

The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the Universe) and others of which there are always many, like meteors and molecules, black holes and binaries.     

复合推进剂力学性能与吸湿率的相关性研究

对复合推进剂试样进行了10℃、30℃、50℃三种温度、多种相对湿度条件下的湿老化,测量了不同条件的湿老化后推进剂试样的吸湿率和力学性能;分别利用线性模型、指数模型和Prony级数模型等3种数学模型表示了复合推进剂力学性能与吸湿率的相关性,并对模型的优劣及其误差进行了讨论。     

Measurements of the 12C/13C Ratio in Planetary Nebulae and Implications for Stellar Evolution

We present the results of a study aimed at determining the 12C/13C ratio in two samples of planetary nebulae (PNe) by means of mm-wave observations of 12CO and 13CO. The first group includes six PNe which have been observed in the 3He+ hyperfine transition; the other group consists of 23 nebulae with rich molecular envelopes. We have determined the isotopic ratio in 14 objects and the results indicate a range of values between 9 and 23. In particular, three PNe have ratios well below the value predicted by standard evolutionary models ( 20), indicating that some extra-mixing process has occurred in these stars. We briefly discuss the implications of our results for standard and nonstandard stellar nucleosynthesis.     

论民营中小企业的企业文化建设

近年来民营中小企业已经成为我国经济中的一支重要力量。然而民营中小企业文化建设现状却不容乐观,影响了非公有制经济的发展。文章阐述了企业文化建设在中小民营企业生存和发展中的重要作用,分析了我国中小民营企业文化建设的现状,提出了中小民营企业的文化建设应树立以人为本的理念、建设个性化的企业文化等建议。     

共振吸声结构在航空发动机上的应用进展

共振吸声结构是由穿孔面板、蜂窝及刚性背板形成的三明治夹层结构,该结构广泛应用于发动机消声短舱内,取得了良好的降噪效果。随着声学理论及制造工艺的不断进步,共振吸声结构从最初的单自由度逐步发展为多自由度甚至内嵌多自由度阶段,吸声效果也取得了较大进步。详细阐述共振吸声结构的吸声原理,并在此基础上介绍国内外发动机消声短舱的发展历程。指出发动机消声短舱的两个发展趋势及在进行短舱声衬结构的精细化设计时要考虑的细节问题,例如背景剪切流动、入射声压级、制造误差等。     

交互绘图软件(MTSCAD2.0)开发中的深层次问题探讨(1)

本文介绍了图形数据的设计和图形编辑的程序设计经验,用实例来说明图形变换的实质就是对图形数据的操作.程序举例用C语言表达,对重要的语句有注解,便于读者理解。     

可压缩混合层中的大尺度结构及其作用初探

利用粒子示踪图像流动显示技术和粒子图像测速技术(PIV技术)研究了对流马赫数Mc=0.38时可压缩混合层发展早期出现的大尺度结构的形状和特性,并将这些混合现象与湍流脉动场结合起来研究了这些大尺度结构对流动混合效率的作用.将粒子示踪图像和湍流脉动强度场对比以后发现:混合层流动中早期出现的大尺度结构沿着顺时针方向旋转着向前移动;该结构上的流体微元具有高涡量.由于该结构旋转和高涡量产生了较大的诱导速度,加上该结构的非定常性导致在这些大尺度结构频繁出现的区域具有很高的脉动强度,从而可能带来较高的混合效率.     

对RLC串联电路中通频带与RLC参数关系的讨论——从一道习题引起的问题

讨论了RLC串联电路中通频带与RLC参数的关系,说明在设计一个RLC串联谐振电路时,在给定谐振频率,电感量和频带宽度时,上下边界频率不能只满足通频带宽度而任意假定,还应满足通频带与RLC这些参数之间关系的表达式.     

论我国高师矩阵结构课程体系的有效性

本从结构、课程设置和课程内容等方面分析了我国高师现行课程体系存在的缺陷，进而提出横向模块、纵向两系列的高师矩阵结构课程体系的基本思路和组成框架。重点从理论上实践上的合理性和统一性等方面分析了矩阵结构课程体系的有效性。     

连续型和非连续型蜂窝芯材的共振吸声结构性能研究

以芳纶纸蜂窝、内嵌树脂隔板和微穿孔面板为原料,制备了连续和非连续双自由度共振吸声结构,对两种共振吸声结构的力学性能和吸声系数进行对比研究。结果表明：连续蜂窝芯材所制备共振吸声结构的压缩和拉伸性能高于非连续型共振吸声结构,其中非稳定型压缩强度和拉伸强度高19%,稳定型压缩强度高32%,稳定型压缩模量高43%,剪切性能基本相当;两层蜂窝芯材容易出现孔格错位（非连续型共振吸声结构）,引起错位区域的微孔堵塞,使该结构的共振吸收峰与理论值出现较大差异。     

The massive star distribution in the Galaxy and the Magellanic Clouds

The numbers and distribution of Population I O-type stars and Wolf-Rayet stars are reviewed. The numbers of known WR stars in the Galaxy, the LMC and the SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.