Understanding high-density matter through analysis of surface spectral lines and burst oscillations from accreting neutron stars

We discuss millisecond period brightness oscillations and surface atomic spectral lines observed during type I X-ray bursts from a neutron star in a low mass X-ray binary system. We show that modeling of these phenomena can constrain models of the dense cold matter at the cores of neutron stars. We demonstrate that, even for a broad and asymmetric spectral line, the stellar radius-to-mass ratio can be inferred to better than 5%. We also fit our theoretical models to the burst oscillation data of the low mass X-ray binary XTE J1814-338, and find that the 90% confidence lower limit of the neutron star’s dimensionless radius-to-mass ratio is 4.2.     

基于贝叶斯动态模型的自相关控制图

传统控制图应用的假设前提是从过程得到的观测值彼此独立.但许多过程存在自相关现象,并且这种自相关现象对控制图性能有严重影响.从工程实际出发,对AR(1) 过程模型提出了基于贝叶斯动态模型的自相关控制图,阐明了此自相关控制图的原理和方法;并将该控制图与基于过程模型的自相关控制图的性能进行比较.此控制图借助贝叶斯先验估计,建模迅速,不以时间序列模型为基础,对强自相关模型具有很好的性能.对强自相关过程,并要求迅速建立过程控制时,可以使用此自相关控制图,进行过程监视.      

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.     

Cosmological Shock Waves

Large-scale structure formation, accretion and merging processes, AGN activity produce cosmological gas shocks. The shocks convert a fraction of the energy of gravitationally accelerated flows to internal energy of the gas. Being the main gas-heating agent, cosmological shocks could amplify magnetic fields and accelerate energetic particles via the multi-fluid plasma relaxation processes. We first discuss the basic properties of standard single-fluid shocks. Cosmological plasma shocks are expected to be collisionless. We then review the plasma processes responsible for the microscopic structure of collisionless shocks. A tiny fraction of the particles crossing the shock is injected into the non-thermal energetic component that could get a substantial part of the ram pressure power dissipated at the shock. The energetic particles penetrate deep into the shock upstream producing an extended shock precursor. Scaling relations for postshock ion temperature and entropy as functions of shock velocity in strong collisionless multi-fluid shocks are discussed. We show that the multi-fluid nature of collisionless shocks results in excessive gas compression, energetic particle acceleration, precursor gas heating, magnetic field amplification and non-thermal emission. Multi-fluid shocks provide a reduced gas entropy production and could also modify the observable thermodynamic scaling relations for clusters of galaxies.     

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.     

腐蚀结构分析中腐蚀坑的随机布置和计算机模拟

针对老龄化飞机安全评估分析中结构表面存在广布随机不等直径腐蚀坑这一现状,采用蒙特卡罗(MonteCarlo)方法分析并编制了计算机程序,完成了由结构腐蚀原况到计算模型的映射,从而实现了利用计算机模拟再现结构腐蚀损伤,为定量研究腐蚀损伤对老龄飞机结构的剩余强度和寿命影响提供可能。     

Alfvén waves in the context of solar-like star formation: accretion columns and disks

In this work we examine the damping of Alfvén waves as a source of plasma heating in disks and magnetic funnels of young solar like stars, the T Tauri stars. We apply four different damping mechanisms in this study: viscous-resistive, collisional, nonlinear and turbulent, exploring a wide range of wave frequencies, from 10⁻⁵Ω_i to 10⁻¹Ω_i (where Ω_i is the ion-cyclotron frequency). The results show that Alfvénic heating can increase the ionization rate of accretion disks and elevate the temperature of magnetic funnels of T Tauri stars opening possibilities to explain some observational features of these objects. This revised version was published online in August 2006 with corrections to the Cover Date.     

30CrMnSiNi2A和GC4（40CrMnSiMoVA）钢裂纹扩展性能比较分析研究

在分析30CrMnSiNi2A和GC4力学性能的基础上,在相同裂纹长度条件下,对两种材料的裂纹扩展寿命和裂纹扩展速率的统计特性进行了统计研究。经比较分析后认为,由于30CrMnSiNi2A钢的裂纹扩展速率较慢,故裂纹扩展寿命较长,但由于其分散性较大,在裂纹长度较大时,99.9%的安全寿命尽管仍比GC4钢大,但两者已很接近。     

高周疲劳曲线的等效应力法

对散点法试验获得的高周疲劳数据,提出了用等效应力法处理中值S-N曲线、用修正的三参数幂函数法或修正的等效应力法处理统计值P-S-N曲线的方法。该方法与用传统的标准方法试验和数据处理相比,不仅可节省试样,而且还可以通过模型内插获得未曾试验应力比下的S-N曲线,更适于工程应用。     

三维地形的计算机模拟生成技术

三维地形的生成是许多模拟器中的一项关键技术。文中给出了地形基准数据库的基本概念和一般的建立方法,并给出了形成计算机模拟三维地形的统计特性和产生方法。最后通过大量的计算仿真试验,对三维地形在不同地形条件下的变化进行了仿真评估。仿真结果为三维地形技术在实际的模拟器中的应用提供了依据。