AI 中文总结
通过分析狐狸座Z星的表面丰度，结合300多万个演化模型，揭示其经历近保守A类质量转移，明确需结合光谱丰度与恒星内部轮廓重建相互作用双星演化史。
AI 中文摘要
双星成员的光球丰度模式是探测大陵五型双星中质量与角动量转移的灵敏探针。为追溯大陵五型双星的演化历史并明确其质量转移效率，我们利用加那利群岛拉帕尔马岛的Mercator望远镜搭载的HERMES摄谱仪，获取了约12颗大陵五型双星的新高分辨率光谱。作为系列论文的首篇，本文呈现了对热大陵五型双星系统狐狸座Z星（Z Vul）的综合分析结果：我们推导了该系统成员星的恒星绝对参数与元素丰度。碳氮比（C/N）是热核反应过程与质量转移最灵敏的示踪剂，研究发现其符合吸积星的预期值，但供星（质量损失星）并未出现深度剥离恒星通常预期的严重C/N反转。我们使用剑桥STARS代码计算了包含300多万个演化模型的大规模网格，以确定最佳拟合模型与所有存活模型。来自氦和CNO丰度的约束表明，狐狸座Z星在其原质量更大的主序星阶段经历了近保守的质量转移事件（A类）。我们的详细化学标记证实，质量损失星的表面丰度代表了被精细剥离的外层，尚未触及富含CNO的核心，这强调了将高分辨率光谱丰度与恒星内部轮廓结合，以准确重建相互作用双星演化历史的必要性。
英文摘要
The photospheric abundance pattern of the components is a sensitive probe of mass and angular momentum transfer in Algols. With the aim to trace the evolutionary history and disclosed efficiency of mass transfer in Algols we collected new high-resolution spectra for about a dozen Algols with the {\sc hermes} spectrograph at the Mercator Telescope on La Palma, Canary Islands. In the present paper, which is the first in the series, we present the results of a comprehensive analysis of Z Vul, a hot Algol-type system. We derived the absolute stellar quantities and elemental abundances for the components. The carbon-to-nitrogen (C/N) ratio is the most sensitive tracer of thermonuclear processing and mass transfer. It is found to be within expected value for gainer but donor lacks the severe C/N inversion traditionally expected for a deeply stripped star. An extensive grid of over three million evolutionary models was calculated with the Cambridge \texttt{STARS} code which allows determination of the best-fitting and all surviving models. Constraints from the He and CNO abundances indicate that Z Vul underwent an episode of nearly conservative mass transfer during the Main Sequence life-time of the originally more massive component (Case A). Our detailed chemical tagging confirms that the surface abundances of the mass-losing component represent the delicately stripped outer layers still not reaching the CNO-rich core. This underscores the need of coupling high-resolution spectroscopic abundances with interior stellar profiles to accurately reconstruct the evolutionary history of interacting binaries.
CommentsAccepted in MNRAS
