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The dilution peak, metallicity evolution, and dating of galaxy interactions and mergers

机译:稀释峰,金属性演变以及星系相互作用和合并的年代

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Strong inflows of gas from the outer disk to the inner kiloparsecsare induced during the interaction of disk galaxies. This inflow ofrelatively low-metallicity gas dilutes the metallicityof the circumnuclear gas. This process is critical for the galaxyevolution. We have investigated several aspects of the process as thetiming and duration of the dilution and its correlation with theinduced star formation. We analysed major(1:1) gas-richinteractions and mergers, spanning a range of initial orbitalcharacteristics. Star formation and metal enrichment from SNe areincludedin our model. Our results show that the strongest trend is between thestar formation rate and the dilution of the metals in the nuclearregion; i.e., the more intense the central burst of star formation, themore the gas is diluted. This trend comes from strong inflows ofrelatively metal-poor gas from the outer regions of both disks, whichfuels the intense star formation and lowers the overall metallicity fora time. The strong inflows happen on timescales of about 108yearsor less (i.e., on an internal dynamical time of the disk in thesimulations), and the most intense star formation and lowest gas phasemetallicities are seen generally after the first pericentre passage.Asthe star formation proceeds and the merger advances, thedilution reduces and enrichment becomes dominant- ultimatelyincreasing the metallicity of the circumnuclear gas to a level higherthan the initial metallicities of the merging galaxies. The``fly-bys''- pairs that interact but do not merge- alsocause some dilution. We even see some dilution early in the merger orin the ``fly-bys'' and thus do not observe a strong trend between thenuclear metallicities andseparation in our simulations until the merger is well advanced. Wealso analyse the O and Feenrichment of the ISM, and show that theevolution of the ratios, aswell as the dilution of the central gas metallicity, can be used as a clock for dating the interaction. Key words: galaxies: interactions - galaxies: formation - galaxies: evolution
机译:在盘星系相互作用期间,引起了从外盘到内千帕的强烈气体流入。相对低金属性的气体的这种流入稀释了周围核气体的金属性。这个过程对于星系进化至关重要。我们已经研究了该过程的几个方面,如稀释的时间和持续时间及其与诱导恒星形成的相关性。我们分析了主要的(1:1)富含气体的相互作用和合并,涵盖了一系列初始轨道特征。我们的模型包括SNe的恒星形成和金属富集。我们的结果表明,最强烈的趋势是在恒星形成率和核区域中金属的稀释之间;即,恒星形成的中央爆发越强烈,气体被稀释的程度就越高。这种趋势来自两个磁盘外部区域的大量相对贫金属气体的大量流入,这助长了强烈的恒星形成并暂时降低了总体金属性。强烈的流入发生在大约108年或更短的时间尺度上(即在模拟中磁盘的内部动力学时间上),通常在首次绕过中心后观察到最强烈的恒星形成和最低的气相金属性。合并的发展,稀释的减少和富集变得占主导地位,最终将周围核气体的金属性提高到比合并星系的初始金属性更高的水平。相互作用但不融合的``飞越''对也会造成一些稀释。我们甚至在合并早期或``飞越''中看到了一些稀释,因此在合并进行得很顺利之前,在我们的模拟中观察不到核金属和分离之间的强烈趋势。我们还分析了ISM的O和Feenrichment,表明比率的演变以及中心气体金属性的稀释可以用作确定相互作用的时标。关键词:星系:相互作用-星系:形成-星系:演化

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