论文标题
通过非单调初始最终质量关系所见，碳恒星形成
Carbon star formation as seen through the non-monotonic initial-final mass relation
论文作者
论文摘要
初始质量关系（IFMR）将恒星的出生质量与死亡时剩下的紧凑型残留物联系起来。尽管普遍承认IFMR在天体物理学中的相关性，但并非所有细节都得到了解决。对银河系的旧开放簇中的一些碳氧气白色矮人进行了新的分析，这使我们在IFMR中识别位于一系列初始质量的IFMR中的扭结，$ 1.65 \ sillesim m _ {\ rm i}/m _}/m _ {\ odot} \ odot} \ silysim 2.10 $。 $ \ $ \ $ \的扭结峰值大约0.70-0.75 \，m _ {\ odot} $由$ m _ {\ rm i} \ simeq 1.8-1.9 \，m _ {\ odot} $产生的星星产生。有趣的是，该峰值与低质量恒星之间的初始质量限制一致，该恒星在中央氢耗尽后发展出退化的氦芯和避免电子退化的中间质量恒星。我们将IFMR扭结解释为以银河系的签名。这一发现对于限制低质量恒星的进化和化学富集至关重要，及其对星系分光光度计特性的影响。
The initial-final mass relation (IFMR) links the birth mass of a star to the mass of the compact remnant left at its death. While the relevance of the IFMR across astrophysics is universally acknowledged, not all of its fine details have yet been resolved. A new analysis of a few carbon-oxygen white dwarfs in old open clusters of the Milky Way led us to identify a kink in the IFMR, located over a range of initial masses, $1.65 \lesssim M_{\rm i}/M_{\odot} \lesssim 2.10$. The kink's peak in WD mass of $\approx 0.70-0.75 \, M_{\odot}$ is produced by stars with $M_{\rm i} \simeq 1.8 - 1.9 \, M_{\odot}$, corresponding to ages of about $1.8 - 1.7 $ Gyr. Interestingly, this peak coincides with the initial mass limit between low-mass stars that develop a degenerate helium core after central hydrogen exhaustion, and intermediate-mass stars that avoid electron degeneracy. We interpret the IFMR kink as the signature of carbon star formation in the Milky Way. This finding is critical to constraining the evolution and chemical enrichment of low-mass stars, and their impact on the spectrophotometric properties of galaxies.
