论文标题
galah调查中对富含李的巨人和普通巨人的丰富分析
Abundance analyses of Li-enriched and normal giants in the GALAH survey
论文作者
论文摘要
比较了Galah调查中富含锂和正常巨人的组成。除LI外，从碳到Europium的富含锂富集和正常巨人之间的唯一可检测到的丰度差异是碳的发生。在（li）= 1.8至3.1的Li-igh巨人中，C缺陷与正常巨人（（li）$ <$ 1.8）的报道非常相似，其中第一次挖掘起来引起了轻微的C缺乏。碳在超级富含li的巨人中的碳含量超过a（li）= 3.2的碳中略有略有较高的含量。文献中的$^{12} $ c/$^{13} $ c的$^{12} $ c/$^{13} $ c的比例表明，添加Li来创建一个Li-rich的巨人可能独立于第一次挖掘的丰度变化。然而，随着CN-cycle的额外转换C到N。成为li富裕的巨人的可能性大约独立于一颗恒星的质量，尽管发现大多数富含李的巨人的质量是低质量（$ M \ m \ leq $ 2 m $ $ _ $ _ \ odot $），但它的创建似乎与恒星的质量无关。正常巨人中富含李的巨人的发生频率约为百分之一，并且略微依赖于金属性（[Fe/h]）。发现富含液化的巨人和正常的巨人具有相似的投影旋转速度，这表明巨人的富集与诸如合并之类的场景和二进制恒星之间的潮汐相互作用无关。
Compositions of lithium-enriched and normal giants among the GALAH survey are compared. Except for Li, the only detectable abundance difference between lithium-enriched and normal giants among the investigated elements from carbon to europium occurs for carbon. Among Li-rich giants with A(Li) = 1.8 to 3.1, the C deficiency is very similar to that reported for the normal giants (with A(Li) $<$ 1.8) where the slight C deficiency arises from the first dredge-up. Carbon is slightly under abundant relative to normal giants among the super Li-rich giants where the Li abundance exceeds A(Li) = 3.2. The C abundance as well as the $^{12}$C/$^{13}$C ratios from the literature suggest that addition of Li to create a Li-rich giant may occur independently of the abundance changes wrought by the first dredge-up. Creation of a super Li-rich giant, however, appears to occur with additional CN-cycle conversion of C to N. The probability of becoming a Li-rich giant is approximately independent of a star's mass, although the majority of the Li-rich giants are found to be low mass ($M \leq$ 2 M$_\odot$). The frequency of occurrence of Li-enriched giants among normal giants is about one percent and slightly dependent on metallicity ([Fe/H]). Li-enriched and normal giants are found to have similar projected rotational velocity which suggest that Li-enrichment in giants is not linked to scenarios such as mergers and tidal interaction between binary stars.
