碳和锰的宇宙起源
The cosmic origin of carbon and manganese
摘要：
[摘要]我们已经确定了51颗矮星的碳丰度和95颗矮星的锰丰度，这两个不同的、定义明确的恒星星族是银河系的薄盘和厚盘。由于这两个种群有不同的化学历史，我们已经能够，通过差分丰度分析使用高分辨率光谱，限制在银河系盘（S）的碳和锰的形成地点。碳的分析是基于872.7 nm处的禁[C I]线，这是一种对恒星大气参数误差不敏感的丰度指标。结合这些数据与我们以前发表的氧丰度，基于630.0 nm处的禁[O I]线，我们可以形成非常强大的[C/O]比，然后我们用来研究碳的起源和银河系薄盘和厚盘的化学演化。我们对丰度趋势的解释是，负责银河系薄盘和厚盘中碳富集的来源在时间尺度上的运作与负责Fe和Y富集的来源非常相似（即，SNIa和AGB星）。对于锰，当比较我们的锰丰度与O丰度相同的恒星，我们发现，在恒星的丰度趋势与运动学典型的厚盘可以解释的金属丰度依赖于产量从SN II。此外，晕中的[Mn/O]对[O/H]趋势是平坦的。我们的结论是，我们的数据的最简单的解释是，锰最有可能是产生在SN II和锰产量等SNAE必须是金属丰度依赖。
英文摘要：
[ABRIDGED] We have determined carbon abundances for 51 dwarf stars and manganese abundances for 95 dwarf stars in two distinct and well defined stellar populations - the Galactic thin and thick disks. As these two populations have different chemical histories we have been able to, through a differential abundance analysis using high-resolution spectra, constrain the formation sites for carbon and manganese in the Galactic disk(s). The analysis of carbon is based on the forbidden [C I] line at 872.7 nm which is an abundance indicator that is insensitive to errors in the stellar atmosphere parameters. Combining these data with our previously published oxygen abundances, based on the forbidden [O I] line at 630.0 nm, we can form very robust [C/O] ratios that we then used to investigate the origin of carbon and the chemical evolution of the Galactic thin and thick disks..... Our interpretation of our abundance trends is that the sources that are responsible for the carbon enrichment in the Galactic thin and thick disks have operated on a time-scale very similar to those that are responsible for the Fe and Y enrichment (i.e., SNIa and AGB stars, respectively). For manganese, when comparing our Mn abundances with O abundances for the same stars we find that the abundance trends in the stars with kinematics typical of the thick disk can be explained by metallicity dependent yields from SN II. Furthermore, the [Mn/O] versus [O/H] trend in the halo is flat. We conclude that the simplest interpretation of our data is that manganese most likely is produced in SN II and that the Mn yields for such SNae must be metallicity dependent.
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