On the X-ray emission from massive star clusters and their evolving superbubbles – II. Detailed analytics and observational effects     

G. A. Añorve-Zeferino  G. Tenorio-Tagle  S. Silich 《Monthly notices of the Royal Astronomical Society》2009,394(3):1284-1306

In this work, we present a comprehensive X-ray picture of the interaction between a super star cluster and the interstellar medium. In order to do that, we compare and combine the X-ray emission from the superwind driven by the cluster with the emission from the wind-blown bubble. Detailed analytical models for the hydrodynamics and X-ray luminosity of fast polytropic superwinds are presented. The superwind X-ray luminosity models are an extension of the results obtained in Paper I. Here, the superwind polytropic character allows us to parametrize a wide variety of effects, for instance, radiative cooling. Additionally, X-ray properties that are valid for all bubble models taking thermal evaporation into account are derived. The final X-ray picture is obtained by calculating analytically the expected surface brightness and weighted temperature of each component. All of our X-ray models have an explicit dependence on metallicity and admit general emissivities as functions of the hydrodynamical variables. We consider a realistic X-ray emissivity that separates the contributions from hydrogen and metals. The paper ends with a comparison of the models with observational data.  相似文献   

Radiative bubbles blown by slow stellar winds     

Christopher D. Matzner  Ruben Krasnopolsky 《Monthly notices of the Royal Astronomical Society》2008,386(2):903-908

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Hydrodynamical simulations of Galactic fountains – I. Evolution of single fountains     

C. Melioli  F. Brighenti  A. D'Ercole  E. M. de Gouveia Dal Pino 《Monthly notices of the Royal Astronomical Society》2008,388(2):573-586

The ejection of the gas out of the disc in late-type galaxies is related to star formation and is due mainly to Type II supernovae. In this paper, we studied in detail the development of the Galactic fountains in order to understand their dynamical evolution and their influence on the redistribution of the freshly delivered metals over the disc. To this aim, we performed a number of 3D hydrodynamical radiative cooling simulations of the gas in the Milky Way where the whole Galaxy structure, the Galactic differential rotation and the supernova explosions generated by a single OB association are considered. A typical fountain powered by 100 Type II supernovae may eject material up to ∼2 kpc which than collapses back mostly in the form of dense, cold clouds and filaments. The majority of the gas lifted up by the fountains falls back on the disc remaining within a radial distance  Δ R = 0.5 kpc  from the place where the fountain originated. This localized circulation of disc gas does not influence the radial chemical gradients on large scale, as required by the chemical models of the Milky Way which reproduce the metallicity distribution without invoking large fluxes of metals. Simulations of multiple fountains fuelled by Type II supernovae of different OB associations will be presented in a companion paper.  相似文献   

长英质岩浆中不混溶流体的运移机理——兼论成矿作用发生的条件   总被引：2，自引：0，他引：2  

朱永峰 《地学前缘》1994,1(4):0-0

与岩浆作用有关的热液矿床的形成,在一定程度上是岩浆体系内富含挥发分流体的组成、压力及性质演变的结果。长英质岩浆中无水硅酸盐矿物的结晶导致挥发性组分以气泡形式存在。气泡的体积随岩浆演化程度增强而不断增大,由于两不混溶流体之密度差而产生的力的作用使气泡相对硅酸盐熔体（＋晶体）超前向上迁移,最终到达岩浆房顶部。长英质岩浆中富含挥发分流体的迁移运动是通过气泡的上浮实现的。气泡能否上浮主要取决于气泡的体积大小和受力的强度。只有体积较大的气泡才可能迅速迁移并到达岩浆房顶部。修正后的Ｄａｒｃｙ定律对气泡（岩浆体系中的流体）的上述运动特征给予了物理学方法的描述。  相似文献   

An experimental study on microscopic characteristics of gas-bearing sediments under different gas reservoir pressures     

Zhenqi Guo  Tao Liu  Lei Guo  Xiuting Su  Yan Zhang  Sanpeng Li 《海洋学报(英文版)》2021,40(10):144-151

Gas-bearing sediments are widely distributed in five continents all over the world. Most of the gases exist in the soil skeleton in the form of discrete large bubbles. The existence of gas-phase may increase or decrease the strength of the soil skeleton. So far, bubbles’ structural morphology and evolution characteristics in soil skeleton lack research, and the influence of different gas reservoir pressures on bubbles are still unclear. The micro characteristics of bubbles in the same sediment sample were studied using an industrial CT scanning test system to solve these problems. Using the image processing software, the micro variation characteristics of gas-bearing sediments in gas reservoir pressure change are obtained. The results show that the number and volume of bubbles in different equivalent radius ranges will change regularly under different gas reservoir pressure. With the increase of gas reservoir pressure, the number and volume of tiny bubbles decrease. In contrast, the number and volume of large bubbles increase, and the gas content in different positions increases and occupies a dominant position, driving the reduction of pore water and soil skeleton movement.  相似文献   

DISCUSSION: ‘HYDROLOGICAL MODEL OF PEAT-MOUND FORM WITH VERTICALLY VARYING HYDRAULIC CONDUCTIVITY’ BY ADRIAN C. ARMSTRONG     

ANDREW J. BAIRD  SIMON W. GAFFNEY 《地球表面变化过程与地形》1996,21(8):765-767

In this comment we argue that the premise on which the peat mound model developed by Armstrong (Earth Surface Process and Landforms, 1995, 20 , 473–477) is based, that hydraulic conductivity shows an exponential decline with depth in bog peats, is unsound. Empirical evidence in the literature for such an exponential decline is less sound than Armstrong suggests. In addition, Armstrong's suggestion that the hypothesis of Baird and Gaffney (Earth Surface Processes and Landforms, 1995, 20 , 561–566) supports an exponential decline is shown to be erroneous.  相似文献   

基于单波束测深资料的海底冷泉动力学特征反演方法研究     

华志励  刘波 《海洋科学》2019,43(9):94-103

为了准确理解冷泉水体中甲烷气体的分布规律,综合运用单波束测深数据和冷泉水体流场数据,建立了冷泉气泡上升、溶解速率的定量反演方法,利用现场海试资料对反演方法进行了验证,并对海试区域的冷泉气体溢出、溶解通量以及冷泉水体的甲烷浓度进行了估算。计算结果表明,考察船航向与冷泉水体流向的差异会对声学探测结果产生影响,当航向与流向的夹角大于±60°时,声学成像中冷泉倾角的误差将超过50%。同时,冷泉气泡上升速率的衰减与溢出口水深显著相关,相关系数可达0.9,并且冷泉上升流对上升速率的提升效果明显。水合物稳定带的分布对冷泉气泡的收缩速率影响显著,稳定带内、外收缩速率的差异可达3～4倍。冷泉气体通量的计算结果表明,调查区域内冷泉的溢出强度整体较大,同时溶解通量与水深之间呈现明显的分段效应。根据冷泉气体溶解通量估算的冷泉水体甲烷浓度与色谱分析结果具有较好的一致性。相关研究有助于实现对冷泉水体中甲烷气体分布的定量评估,为潜在海底冷泉区的圈划和海域天然气水合物的调查提供技术支撑。  相似文献   

Nitrogen, Oxygen and Argon Dissolved in the Northern North Pacific in Early Summer     

Noriko Nakayama  Shuichi Watanabe  Shizuo Tsunogai 《Journal of Oceanography》2002,58(6):775-785

Major gases dissolved in seawater were accurately determined with a shipboard gas chromatographic method. The standard deviations were 0.28, 0.34 and 0.36% for N₂, O₂ and Ar, respectively. The method was applied to water from the northwestern North Pacific Ocean collected in May to June 2000. We got 127 duplicate seawater samples from the surface 200 m layer at 11 stations. The O₂ concentrations obtained by this method agreed with those given by the Winkler method. All the seawater samples from the surface 200 m, especially those from the upper 30 m, were supersaturated with respect to atmospheric N₂ and Ar concentrations. In the topmost 30 m layer, the degrees of supersaturation in the inventory were 2.7–4.3% for N₂ (ΔN₂) and 1.7–2.6% for Ar (ΔAr), and their ratios, ΔN₂/ΔAr, ranged from 1.53 to 1.81. This supersaturation seems to be chiefly due to air bubbles injected into the water and dissolved due to the water pressure, because the N₂/Ar ratio of the air is around 2. The amounts of air bubbles dissolved in the upper 30 m water were relatively large, with mean value of 0.41 ml/kg or 18.4 μmol/kg. The ΔN₂, ΔAr and ΔN₂/ΔAr values were all positively well correlated with the wind velocities averaged for the last 24 hours prior to sampling, allowing the conclusion to be drawn that the weaker the wind velocity, the dissolved gas composition approaches in equilibrium with the air; while the stronger the wind velocity, it approaches in the air composition. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

X‐ray computed tomography of peat soils: measuring gas content and peat structure     

Nicholas Kettridge  Andrew Binley 《水文研究》2008,22(25):4827-4837

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Hydrodynamics of Supernova Evolution in the Winds of Massive Stars     

Vikram V. Dwarkadas 《Astrophysics and Space Science》2007,307(1-3):153-158

Core-Collapse supernovae arise from stars greater than 8 M_⊙. These stars lose a considerable amount of mass during their lifetime, which accumulates around the star forming wind-blown bubbles. Upon the death of the star in a spectacular explosion, the resulting SN shock wave will interact with this modified medium. We study the evolution of the shock wave, and investigate the properties of this interaction. We concentrate on the evolution of the SN shock wave in the medium around a 35 solar mass star. We discuss the hydrodynamics of the resulting interaction, the formation and growth of instabilities, and deviations from sphericity.  相似文献