LAMOST J1109+7459的起源

Nour Aldein Almusleh, Yazan Khrais, Ali Taani
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引用次数: 0

摘要

我们对LAMOST J1109+0754进行了全面的化学动力学分析,这是一颗相对明亮(V = 12.8),极贫金属([Fe/H] = $-3.17$),顺行($J_\phi$和$V_\phi$$> 0$)的恒星,具有很强的\textit{r-}过程增强([Eu/Fe] = $+$ 0.94 $\pm$ 0.12, [Ba/Fe] = $-$ 0.52 $\pm$ 0.15)。得到了31种化学丰度(从锂到钍)。我们提出一个可能的祖恒星质量为13.4-29.5 M $_\odot$。我们认为J1109+0754是主要r-\textit{过程}组分的代表,因为它与尺度太阳能r-过程\textit{组分具有良好的一致性}。我们{\it基于从Illustris-TNG模拟中提取的银河系模拟模型,分析了这颗恒星在随时间变化的银河系势}中的轨道历史。利用\texttt{这个模型,我们}对J1109+0754在年轻宇宙年龄时的相空间坐标进行了统计估计。总的来说,计算出的运动、推导出的化学物质以及宇宙学模拟的结果表明,LAMOST J1109+0754最有可能形成于一个低质量矮星系,属于银河系外晕群。
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The Origin of LAMOST J1109+7459
We report a comprehensive Chemo-dynamical analysis of LAMOST J1109+0754, a relatively bright (V = 12.8), extremely metal-poor ([Fe/H] = $-3.17$), and prograde ($J_\phi$ and $V_\phi$ $> 0$) star, with a strong \textit{r}-process enhancement ([Eu/Fe] = $+$0.94 $\pm$ 0.12, [Ba/Fe] = $-$0.52 $\pm$ 0.15). 31 chemical abundances (from Lithium to Thorium) were derived. We suggest a possible progenitor with stellar mass of 13.4-29.5 M$_\odot$. We argue that J1109+0754 is representative of the main \textit{r}-process component due to the well agreement with the scaled-solar \textit{r}-process component. We analyze the orbital history of this star in a {\it time-varying Galactic potential}, based on a Milky-Way analogue model extracted from \texttt{Illustris-TNG} simulations. Using this model, we carry out a statistical estimation of the phase-space coordinates of J1109+0754 at a young cosmic age. Collectively, the calculated motions, the derived chemistry, and the results from the cosmological simulations suggest that LAMOST J1109+0754 most likely formed in a low-mass dwarf galaxy, and belongs to the Galactic outer-halo population.
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