Milky Way chemo-dynamics in the era of Gaia
Milky Way chemo-dynamics in the era of Gaia
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DOI：
10.1002/asna.201612404
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发表时间：
2016-01
影响因子：
0.9
通讯作者：
I. Minchev;C. Chiappini;M. Martig
中科院分区：
文献类型：
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作者：
I. Minchev;C. Chiappini;M. Martig
银河考古学的主要目标是了解银河系基本组成部分的形成和演变。这需要复杂的化学动力学建模，其中椎间盘不对称性（例如，来自中央棒、螺旋臂和下落卫星的扰动）和非平衡过程自洽地考虑在内。在这里，我们讨论了目前的现状，银河系化学动力学模型，并专注于最近的混合技术，这有助于规避传统的化学富集和星星的形成遇到完全自洽的宇宙学simulation.We表明，这个模型可以解释在银河系的化学运动学关系的数量。此外，本发明还提供了一种方法，我们证明：（1）我们的模型与观测到的年龄-[α/Fe]和年龄-[Fe/H]关系相吻合;（2）年龄-[Fe/H]关系中的离散不能简单地用模糊来解释（位于apo和近心点的恒星访问太阳附近），但有显著的径向迁移（恒星诞生在其他地方，但由于引导半径的变化而最终出现在今天的太阳附近）是必要的。我们强调准确的恒星年龄的重要性，如通过星震学获得的CoRoT和开普勒任务，打破不同的银河系演化方案之间的简并。
The main goal of Galactic Archaeology is understanding the formation and evolution of the basic Galactic components. This requires sophisticated chemo-dynamical modeling, where disc asymmetries (e.g., perturbations from the central bar, spirals arms, and infalling satellites) and non-equilibrium processes are taken into account self-consistently. Here we discuss the current status of Galactic chemo-dynamical modeling and focus on a recent hybrid technique, which helps circumvent traditional problems with chemical enrichment and star formation encountered in fully self-consistent cosmological simulations.We show that this model can account for a number of chemo-kinematic relations in the Milky Way. In addition, we demonstrate that (1) our model matches well the observed age-[α/Fe] and age-[Fe/H] relations and (2) that the scatter in the age-[Fe/H] relation cannot be simply explained by blurring (stars on apo- and pericenters visiting the solar vicinity) but significant radial migration (stars born elsewhere but ending up at the solar vicinity today because of a change in guiding radius) is needed. We emphasize the importance of accurate stellar ages, such as those obtained through asteroseismology by the CoRoT and Kepler missions, for breaking the degeneracy among different Galactic evolution scenarios.