论文标题
中子星合并作为R-Process的主要来源：Natal踢和内而外的进化
Neutron Star Mergers as the Main Source of R-process: Natal Kicks And Inside-Out Evolution to The Rescue
论文作者
论文摘要
由于GW170817的检测，二进制中子星星合并（BNSMS）当前是\ textsl {r} - 过程中最有希望的来源。估计的发生频率和每次合并的质量弹出量表明，BNSM本身可以解释银河系中的所有\ textsl {r} - 过程富集。但是，太阳邻域[Fe/h] $ \ gtrsim -1 $的[EU/FE]与[Fe/H]的[Fe/H]的趋势与具有标准延迟时间分布（DTD）$ \ propto $ \ propto t^{ - 1} $的平坦趋势不一致。这导致了这样的建议，即需要对BNSM的DTD进行其他源或修改以匹配观测值。我们通过将银河系动力学代码\ textsc {galpy}的结果与一个区域的银河化学进化模型\ textsc \ textsc \ emega}相结合，调查了中子星二进制期间在中子恒星二进制诞生期间收到的纳塔尔踢的影响。我们表明，当从内而外磁盘演化的模拟中进行关键输入与出生踢结合时，BNSM自然可以在太阳能邻域中使用[eu/fe/h]的[eu/fe/h]的下降趋势，而无需对DTD进行修改或其他\ textsl {r} -process sources。
Binary neutron star mergers (BNSMs) is currently the most promising source of \textsl{r}-process thanks to the detection of GW170817. The estimated occurring frequency and the amount of mass ejected per merger indicate that BNSMs by itself can account for all the \textsl{r}-process enrichment in the Galaxy. However, the decreasing trend of [Eu/Fe] vs [Fe/H] of disk stars for [Fe/H]$\gtrsim -1$ in the solar neighborhood is inconsistent with the flat trend expected from BNSMs with a standard delay time distribution (DTD) $\propto t^{-1}$. 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 \textsl{r}-process element Eu in the Milky Way by combining the results from the galactic dynamics code \textsc{galpy} with a one-zone Galactic chemical evolution model \textsc{omega}. We show that when key inputs from simulations of the inside-out disk evolution are combined with natal kicks, BNSMs can naturally reproduce the observed decreasing trend of [Eu/Fe] with [Fe/H] in the solar neighborhood without the need for modification to the DTD or additional \textsl{r}-process sources.
