论文标题
巨大恒星中的supernova前风能在高红移时用氮气富含星际培养基吗？
Can pre-supernova winds from massive stars enrich the interstellar medium with nitrogen at high redshift?
论文作者
论文摘要
了解氮的核合成起源以及星际培养基中N/O比的演化对于高降射时星系化学进化的全面图景至关重要，因为大多数观察金属性（O/H）估计值隐含地取决于N/O比率。在高红移处观察到的N/O显示出O/H的总体恒定性，尽管散布较大。我们表明，这些迄今无法解释的功能可以通过旋转巨大恒星的前风（m $ \ gtrsim 10 \，\ mathrm {m} _ \ odot $，$ v/v _ {\ rm {crit}} \ gtrsim 0.4 $ 0.4 $）来解释。我们的模型自然会产生观察到的N/O高原以及低O/H处的散射。我们发现散射是由于不同的恒星形成效率而产生的。但是，具有超新星占主导地位的模型在低O/H时与观察到的N/O的拟合度较差。低O/H处的这种特殊的丰度模式表明，矮星系最有可能没有SNE的产量，并且主要由Supernova前风丰度富集。
Understanding the nucleosynthetic origin of nitrogen and the evolution of the N/O ratio in the interstellar medium is crucial for a comprehensive picture of galaxy chemical evolution at high-redshift because most observational metallicity (O/H) estimates are implicitly dependent on the N/O ratio. The observed N/O at high-redshift shows an overall constancy with O/H, albeit with a large scatter. We show that these heretofore unexplained features can be explained by the pre-supernova wind yields from rotating massive stars (M$\gtrsim 10 \, \mathrm{M}_\odot$, $v/v_{\rm{crit}} \gtrsim 0.4$). Our models naturally produce the observed N/O plateau, as well as the scatter at low O/H. We find the scatter to arise from varying star formation efficiency. However, the models that have supernovae dominated yields produce a poor fit to the observed N/O at low O/H. This peculiar abundance pattern at low O/H suggests that dwarf galaxies are most likely to be devoid of SNe yields and are primarily enriched by pre-supernova wind abundances.
