发表机构
Yunnan Observatories, Chinese Academy of Sciences; International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research; University of Chinese Academy of Sciences; Lund Observatory, Division of Astrophysics, Department of Physics, Lund University; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院云南天文台; 超新星国际中心（ICESUN），云南省超新星研究重点实验室; 中国科学院大学; 隆德大学物理系天体物理学部隆德天文台; 中国科学院国家天文台光学天文重点实验室）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究针对公共包层演化中恒星束缚能的不确定性，引入包层质量残余的改进束缚能，基于绝热质量损失模型重新计算λ参数，发现晚期红巨星和渐近巨星分支阶段λ可增一至两个数量级，并提供插值网格和拟合公式。
AI 中文摘要
公共包层演化（CEE）是密近双星系统演化的关键过程。许多重要的天体物理对象和演化阶段与CEE密切相关，包括白矮双星、热亚矮星以及引力波并合事件。在CEE的标准能量形式中，供体包层的束缚能起着至关重要的作用，因为它直接影响CEE后的最终轨道周期，并且是双星族合成研究中的关键物理参数。然而，目前采用的束缚能存在较大的不确定性，主要原因是巨星分支星的包层束缚能在氦核边界附近变化剧烈。此外，CEE期间恒星的膨胀也会影响束缚能。为了解决这些问题，我们引入了针对包层质量残余的改进束缚能。基于绝热质量损失模型，我们重新计算了不同质量和不同演化阶段恒星的CEE束缚能参数λ的分布，并分析了包层质量残余和绝热膨胀的影响。由于包层质量残余，一些供体在红巨星分支晚期和渐近巨星分支阶段的λ可以增加一到两个数量级。此外，我们为这些结果提供了插值网格和拟合公式，可方便地应用于各种双星族合成代码。
英文摘要
Common-envelope evolution (CEE) is a key process in the evolution of close binary systems. Many important astrophysical objects and evolutionary stages are closely related to CEE, including white dwarf binaries, hot subdwarfs, and gravitational wave mergers. In the standard energy formalism of CEE, the binding energy of the donor envelope plays a crucial role, as it directly affects the final orbital period after CEE and serves as a key physical parameter in binary population synthesis studies. However, the currently adopted binding energy suffers from large uncertainties, mainly because the envelope binding energy of giant-branch stars varies strongly near the helium-core boundary. In addition, the expansion of the star during CEE can also affect the binding energy. To address these issues, we introduce an improved binding energy for the envelope mass residual. Based on adiabatic mass loss models, we recalculate the distribution of the CEE binding-energy parameter lambda for stars with different masses and at different evolutionary stages, and we analyse the effects of envelope mass residual and adiabatic expansion. Due to the envelope mass residual, the lambdas of some donors can increase by one to two orders of magnitude at the late red giant branch and asymptotic giant branch stages. Furthermore, we provide interpolation grids and fitting formulae for these results, which can be readily applied to various binary population synthesis codes.
Comments15 pages, 9 figures
