arXiv 1107.45612011-07-22astro-ph.GA

银河系尘埃的形成与演化。II。太阳附近

Formation and Evolution of the Dust in Galaxies. II. The Solar Neighbourhood

L. Piovan, C. Chiosi, E. Merlin, T. Grassi, R. Tantalo, U. Buonomo, L. P. Cassarà

备注：: 37 pages, 18 figures and 5 tables

摘要：

在过去的十年中，新一代的化学模型已经将粉尘纳入ISM的处理中。这一重大成就是由越来越多的关于高度模糊的高z宇宙和太阳邻域（SoNE）有趣的局部性质的数据所推动的。我们在这里提出了一个新的模型，能够模拟的形成和演变的灰尘在ISM。该模型遵循16种元素的演变，特别注意那些同时存在于气体和尘埃的形式，如C，N，O，Mg，Si，S，Ca和Fe。在这项研究中，我们专注于SoNe和MW磁盘作为一个整体，这被认为是实验室来测试的物理成分的灰尘演变。原始气体的侵入，恒星的诞生和死亡，物质在相邻壳层之间的径向流动，中心棒的存在，SNae和AGB恒星的星尘排放，尘埃的破坏和吸积都被考虑在内。该模型再现了气体中元素的局部耗尽，同时满足从观测中获得的其他约束。气体和尘埃中元素丰度的演变已经很好地再现了参数的合理选择。特别是Mg/Si比驱动硅酸盐的形成。我们发现，对于大部分的MW的演变，尘埃富集的主要过程是在ISM的寒冷地区的吸积。SNae在进化的早期阶段占主导地位。我们已经研究了控制时间窗口的主要因素，在该窗口中，SNAE管理的尘埃预算在低和高恒星形成环境。讨论了AGB星所起的作用。我们发现，IMF的范围内的大质量恒星的定期斜率更好地再现所观察到的耗尽。SoNe获得的结果使我们能够安全地扩展模型。

英文摘要：

Over the past decade a new generation of chemical models have included the dust in the treatment of the ISM. This major accomplishment has been spurred by the growing amounts of data on the highly obscured high-z Universe and the intriguing local properties of the Solar Neighbourhood (SoNE). We present here a new model able to simulate the formation and evolution of dust in the ISM. The model follows the evolution of 16 elemental species, with particular attention to those that are simultaneously present in form of gas and dust, e.g. C, N, O, Mg, Si, S, Ca and Fe. In this study we focus on the SoNe and the MW Disk as a whole which are considered as laboratories to test the physical ingredients governing the dust evolution. Infall of primordial gas, birth and death of stars, radial flows of matter between contiguous shells, presence of a central bar, star-dust emission by SNae and AGB stars, dust destruction and accretion are taken into account. The model reproduces the local depletion of the elements in the gas, and simultaneously satisfies other constraints obtained from the observations. The evolution of the element abundances in the gas and dust has been well reproduced for plausible choices of the parameters. The Mg/Si ratio, in particular, drives the formation of silicates. We show that for most of the evolution of the MW, the main process for dust enrichment is the accretion in the cold regions of the ISM. SNae dominate in the early phases of the evolution. We have examined the main factors controlling the temporal window in which SNae govern the dust budget both in low and high star forming environments. The role played by AGB stars is discussed. We find that IMFs with regular slope in the range of massive stars better reproduce the observed depletions. The results obtained for the SoNe lead us to safely extend the model.

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英文摘要：

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