银河系球状星团、晕子结构及卫星星系的静力学与爆发性α元素化学丰度
Hydrostatic and explosive $α$-element chemical abundances of Milky Way globular clusters, halo substructures, and satellite galaxies
AI总结：
本文基于APOGEE数据对比银河系球状星团、晕子结构及卫星星系的静力学与爆发性α元素丰度比，发现球状星团与晕子结构hex ratio相似且高于矮卫星星系，并揭示其随金属丰度和年龄的变化趋势。
摘要：
恒星大气元素丰度比保留了其诞生条件的信息，有助于阐明其起源和性质。本文利用APOGEE巡天数据，对大量银河系球状星团（GCs）、晕子结构、卫星星系以及银河系高/低α盘样本的静力学与爆发性α元素丰度比及其二者之比（hex ratio）进行了分析与对比。结果表明：i）银河系球状星团和晕子结构在广泛的[Fe/H]范围内表现出定性相似的hex ratio，且高于相似[Fe/H]的矮卫星星系；ii）对于所研究的所有恒星族群，hex ratio随[Fe/H]呈现趋势；iii）银河系球状星团的hex ratio随年龄存在弱趋势，但与初始或最终球状星团质量无关；iv）原位形成的球状星团与被标记为吸积形成的球状星团之间在hex ratio上没有差异。
英文摘要：
Stellar atmospheric element abundance ratios of stars retain information about their birth conditions, helping elucidate their origin and nature. In this letter, we analyse and contrast the hydrostatic and explosive $α$-element abundance ratios, and the ratio of the two (the hex ratio), for a large sample of Galactic globular clusters (GCs), halo substructures, satellite galaxies, and the Milky Way high-/low-$α$ discs using data from the $APOGEE$ survey. Our results show that: $i$) Milky Way GCs and halo substructures appear to have qualitatively similar hex ratios across a broad range of [Fe/H], that are higher than that of dwarf satellite galaxies of similar [Fe/H]; $ii$) for all stellar populations studied, there is a trend in the hex ratio with [Fe/H]; $iii$) there is a weak trend in the hex ratio with respect to age for Galactic GCs, but not with initial or final GC mass; $iv$) there are no differences in the hex ratio between GCs formed $in$ $situ$ versus those labelled as accreted.
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