论文标题
宇宙学对\ textit {r} -process-hehanced星星的早期积聚。 I. Lamost J1109+0754的全面化学动力分析
Cosmological Insights into the Early Accretion of \textit{r}-Process-Enhanced stars. I. A Comprehensive Chemo-dynamical Analysis of LAMOST J1109+0754
论文作者
论文摘要
这项研究对Lamost J1109 +0754，Bright（V = 12.8）进行了全面的化学分析分析，极度金属罚款（\ abund {fe} {h} {h} = $ -3.17 $）恒星，具有强的\ textit \ textit {r} {r} -process -process -process-process-process-process-process-process-process-process增强（\ abund $ $ pmund $} { 0.12）。我们的结果基于由$ GAIA $提供的7-D测量以及源自高分辨率（$ r \ sim 110,000 $），高信噪比（$ s/n \ sim 60）$ 2.4 \获得的光谱，由2.4 \，M自动化的Planet Finders telescope在Lick Compervator中获得。我们获得了31个元素的化学丰度（从锂到or）。光元素（z $ \ leqslant 30 $）的丰度比（\ abund {x} {fe}）表明在13.4-29.5 \，m $ _ $ _ \ odot $质量范围内有大量人口\，iii祖细胞。重型元素（$ 30 <$ z $ \ leqslant 90 $）J1109+075的丰度模式与Scaled-Solar \ textit {r} - 程序签名非常吻合。 We have developed a novel approach to trace the kinematic history and orbital evolution of J1109+0754 with a c\textbf{O}smologically de\textbf{RI}ved tim\textbf{E}-varyi\textbf{N}g Galactic po\textbf{T}ential (the ORIENT) constructed from snapshots of a simulated从\ texttt {Illustris-tng}仿真中获取的乳白色模拟。这个类似银河系的星系中的轨道进化以及化学丰富的模式意味着J1109+0754可能起源于位于银河中心的$ \ sim $ 60 \ kpc的低质量矮人星系中，该中心是银河系中心的，它被带来了$ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ \ sim $ 6-7 \ gyr，属于那个属于那个星系，现在属于恒星，现在属于星系。
This study presents a comprehensive chemo-dynamical analysis of LAMOST J1109+0754, a bright (V = 12.8), extremely metal-poor (\abund{Fe}{H} = $-3.17$) star, with a strong \textit{r}-process enhancement (\abund{Eu}{Fe} = +0.94 $\pm$ 0.12). Our results are based on the 7-D measurements supplied by $Gaia$ and the chemical composition derived from a high-resolution ($R\sim 110,000$), high signal-to-noise ratio ($S/N \sim 60)$ optical spectrum obtained by the 2.4\,m Automated Planet Finder Telescope at Lick Observatory. We obtain chemical abundances of 31 elements (from lithium to thorium). The abundance ratios (\abund{X}{Fe}) of the light-elements (Z $\leqslant 30$) suggest a massive Population\,III progenitor in the 13.4-29.5\,M$_\odot$ mass range. The heavy-element ($30 <$ Z $\leqslant 90$) abundance pattern of J1109+075 agrees extremely well with the scaled-Solar \textit{r}-process signature. We have developed a novel approach to trace the kinematic history and orbital evolution of J1109+0754 with a c\textbf{O}smologically de\textbf{RI}ved tim\textbf{E}-varyi\textbf{N}g Galactic po\textbf{T}ential (the ORIENT) constructed from snapshots of a simulated Milky-Way analog taken from the \texttt{Illustris-TNG} simulation. The orbital evolution within this Milky Way-like galaxy, along with the chemical-abundance pattern implies that J1109+0754 likely originated in a low-mass dwarf galaxy located $\sim$ 60\,kpc from the center of the Galaxy, which was accreted $\sim$ 6 - 7\,Gyr ago, and that the star now belongs to the outer-halo population.
