大质量恒星中双星星团质量转移的化学指纹
Chemical fingerprints of binary mass transfer in massive stars
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中文总结 AI 辅助
本研究通过大质量双星演化模型发现表面化学丰度的系统性趋势，开发不依赖特定模型的分析框架，结合表面丰度约束双星质量转移，应用于γ Columbae等OB星并解释其演化历史。
中文摘要 AI 辅助
大多数大质量恒星诞生于密近双星系统，恒星随年龄增长会膨胀，质量转移甚至与伴星并合不可避免。然而，多数双星相互作用产物表现为单星，其过往经历的主要证据已丢失。在一套 comprehensive 的详细大质量双星演化模型网格中，我们发现了表面化学丰度的系统性趋势，可用于识别过往的质量吸积星。我们开发了一种不依赖特定演化模型的分析框架，通过观测到的表面丰度来限制吸积物质的数量和组成，这为大质量双星中不确定的质量转移物理提供了严格约束，还能重建原双星系统的过往演化历史。该方法经证实也可约束双星并合（例如SN 1987A），已应用于目前研究最充分的一些O型、B型恒星（OB星）。对于被认为是包层剥离星的γ Columbae，我们证明它是一颗质量吸积星，其伴星可能形成了包层剥离型超新星。我们的结果凸显了表面丰度测量作为强大工具，可增进对演化向超新星及致密天体双星的大质量双星系统的理解。
英文摘要
The majority of massive stars are born in close binary systems. As stars expand when they age, mass transfer or even a merger with their companion is inevitable. However, most binary interaction products appear as single stars, such that the main evidence of their exciting past is lost. In a comprehensive grid of detailed massive binary evolution models we find systematic trends in chemical surface abundances that allow identifying the past mass gainers. We develop an analytic framework which is independent of specific evolutionary models, to constrain the amount and composition of the accreted material from their observed surface abundances. This yields tight constraints on the uncertain mass transfer physics in massive binary stars and allows us to reconstruct the past evolutionary history of the progenitor binary system. This method, which is shown to also constrain binary mergers (for example, SN 1987A), is applied to some of the best-studied OB stars so far. For γ Columbae, suggested to be an envelope-stripped star, we show that it is a mass gainer instead, whose companion star likely formed a stripped-envelope supernova. Our results highlight surface abundance measurements as a powerful tool to improve our understanding of massive binary systems evolving towards supernovae and compact object binaries.
