Chemical evolution with radial mixing redux: a detailed model for formation and evolution of the Milky Way
Chemical evolution with radial mixing redux: a detailed model for formation and evolution of the Milky Way
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DOI：
10.1093/mnras/stad1568
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发表时间：
2022-04
影响因子：
4.8
通讯作者：
Boquan Chen;M. Hayden;Sanjib Sharma;J. Bland-Hawthorn;C. Kobayashi;A. Karakas
中科院分区：
文献类型：
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作者：
Boquan Chen;M. Hayden;Sanjib Sharma;J. Bland-Hawthorn;C. Kobayashi;A. Karakas
我们提出了一个多区银河系化学演化（GCE）模型，考虑到最近更新的主要核合成通道的产量。它结合了以前GCE模型中常见的物理过程，如超新星和星星形成的气体反馈，圆盘中气体的径向流动，新鲜气体的流入，沿着恒星散射过程，如径向迁移。我们单独分析了我们模型中不同物理过程对银河系观测特性的影响。圆盘中气体的径向流动在建立低[α/Fe]序列中[Fe/H]的径向梯度中起重要作用。我们的模型具有一个平滑的气体入口和恒定的星星形成效率，能够再现在不同的（R，|z|银河系的位置。我们的结果指出，Ia型超新星爆发后[α/Fe]的快速演化和高[α/Fe]序列形成过程中的高星星形成率是[α/Fe]双峰的起源。在我们的模型中，为了再现[α/Fe]能隙和盘中的化学扩散，不需要二次入流。此外，我们还比较了各种单丰度种群的中位年龄和不同（R，|z|）从我们的基准模型到观测值的位置。我们讨论了我们的结果与其他相关工作的细节。
We present a multizone galactic chemical evolution (GCE) model for the Milky Way that takes the most recently updated yields of major nucleosynthesis channels into account. It incorporates physical processes commonly found in previous GCE models like gas feedback from supernovae and star formation, the radial flow of gas in the disc, and the infall of fresh gas, along with stellar scattering processes like radial migration. We individually analyse the effect of different physical processes present in our model on the observed properties of the Galaxy. The radial flow of gas in the disc plays an important role in establishing the radial gradient for [Fe/H] in the low-[α/Fe] sequence. Our model with one episode of smooth gas infall and constant star formation efficiency is capable of reproducing the observed ([Fe/H], [α/Fe]) distribution of stars at different (R, |z|) positions in the Milky Way. Our results point to the rapid evolution of [α/Fe] after the onset of Type Ia supernovae and a high star formation rate during the formation of the high-[α/Fe] sequence as the origin of dual peaks in [α/Fe]. A secondary infall is unnecessary to reproduce the [α/Fe] gap and chemical spread in the disc in our model. We additionally compare the median age for various mono-abundance populations and the age–metallicity relation at different (R, |z|) positions from our fiducial model to observations. We discuss our results in relation to other related work in detail.