Binary neutron star mergers (BNSMs) are currently the most promising source of r -process thanks to the detection of GW170817. The estimated occurring frequency and the amount of mass ejected per merger indicate that BNSMs by themselves can account for all the r -process enrichment in the Galaxy. However, the decreasing trend of [Eu/Fe] versus [Fe/H] of disk stars for [Fe/H] ≳ −1 in the solar neighborhood is inconsistent with the flat trend expected from BNSMs with a standard delay time distribution(DTD) ∝ t −1 . This has led to the suggestion that either additional sources or modification to the DTD of BNSMs is required to match the observations. We investigate the effects of natal kicks received during the birth of neutron star binaries on the chemical evolution of r -process element Eu in the Milky Way by combining the results from the galactic dynamics code galpy with a one-zone Galactic chemical evolution model

中文翻译：

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中子星合并是r过程的主要来源：纳塔尔踢和救援的由内而外的演变

由于发现了GW170817，二元中子星合并（BNSM）是当前最有希望的r过程来源。估计的合并发生频率和每次合并排出的质量数量表明，BNSM本身可以解释银河系中所有r过程富集。然而，太阳附近[Fe / H]≳-1的盘状恒星[Eu / Fe]相对于[Fe / H]的下降趋势与标准延迟时间分布（DTD）的BNSM预期的平坦趋势不一致。 ）t −1。这导致提出这样的建议，即需要BNSM的DTD的其他来源或修改以匹配观察结果。