AI 中文总结
研究银河系金属丰度下II型超新星前身星，用ComBinE代码发现约40%源于主序后星与主序伴星合并。合并产物有更重富氢包层且富含氦，会影响IIP型光变曲线，利用相关设施约束比例有助于了解双星演化物理。
AI 中文摘要
在塑造核心坍缩超新星的前身星群体中，双星相互作用预计起着主要作用，尤其是在深度、高频率瞬态巡天时代。使用ComBinE（一种将表格化恒星结构模型与基于物理的质量转移稳定性标准相结合的快速双星群体合成代码），我们发现银河系金属丰度下约40%的II型超新星前身星源自主序后恒星与主序伴星在不稳定质量转移后的合并。与具有相同氦核质量的单星前身星相比，这些合并产物有更重的富氢包层和更宽的包层质量分布。它们的包层富含氦，相对增强高达80%，氦质量分数达到0.4。这些差异预计会影响IIP型光变曲线，应在未来的前身星和爆炸模型中予以考虑。利用LSST、罗曼太空望远镜和极大望远镜等设施来约束合并诱导的IIP型比例，将有助于深入了解双星演化物理。
英文摘要
Binary interactions are expected to play a major role in shaping the progenitor population of core-collapse supernovae, particularly in the era of deep, high-cadence transient surveys. Using ComBinE, a rapid binary population synthesis code combining tabulated stellar structure models with physically motivated mass-transfer stability criteria, we find that ~40% of Type II supernova progenitors at Milky Way metallicity originate from mergers between a post-main-sequence star and a main-sequence companion following unstable mass transfer. Compared to single-star progenitors with the same helium-core mass, these merger products have more massive hydrogen-rich envelopes and broader envelope-mass distributions. Their envelopes are helium-enriched, with relative enhancements of up to 80% and helium mass fractions reaching 0.4. These differences are expected to affect Type IIP light curves and should be considered in future progenitor and explosion models. Constraining the merger-induced Type IIP fraction with facilities such as LSST, Roman, and the ELT will provide insights into binary evolution physics.
Comments5 pages, 3 figures, submitted to the proceedings of IAU Symposium 406: Future landscape of astrophysical transients
