Abundance ratios in the hot ISM of elliptical galaxies

Abundance ratios in the hot ISM of elliptical galaxies
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椭圆星系热ISM中的丰度比

DOI：
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
F. Matteucci
F. Matteucci
中科院分区：
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文献类型：
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作者：
A. Pipino;F. Matteucci

文献摘要

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约束提出的解决椭圆星系热星际介质中理论Fe差异的方案，同时解释[α/Fe]比。为了做到这一点，我们使用最新的理论nucleosynthetic产量，我们将灰尘，我们探索不同的SNIA祖方案通过一个自洽的化学演化模型再现的性质，在椭圆星系的恒星种群。模型与铁只有灰尘和/或较低的有效SNIa率实现了更好的协议与所观察到的铁丰度。然而，一个适当的修改SNIa产量相对于标准的W7模型需要完全匹配的丰度比模式。Maeda等人（2010年）的2D爆炸模型C-DDT是再现[Fe/H]和[alpha/Fe]比的有希望的候选模型。（A&A格式）
To constrain the recipes put forth to solve the theoretical Fe discrepancy in the hot interstellar medium of elliptical galaxies and at the same time explain the [alpha/Fe] ratios. In order to do so we use the latest theoretical nucleosynthetic yields, we incorporate the dust, we explore differing SNIa progenitor scenarios by means of a self-consistent chemical evolution model which reproduces the properties of the stellar populations in elliptical galaxies. Models with Fe-only dust and/or a lower effective SNIa rate achieve a better agreement with the observed Fe abundance. However, a suitable modification to the SNIa yield with respect to the standard W7 model is needed to fully match the abundance ratio pattern. The 2D explosion model C-DDT by Maeda et al. (2010) is a promising candidate for reproducing the [Fe/H] and the [alpha/Fe] ratios. (A&A format)