Convection and spin-up during common envelope evolution: the formation of short-period double white dwarfs
Convection and spin-up during common envelope evolution: the formation of short-period double white dwarfs
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DOI：
10.1093/mnras/staa2088
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发表时间：
2020-06
影响因子：
4.8
通讯作者：
E. Wilson;J. Nordhaus;J. Nordhaus
中科院分区：
文献类型：
--
作者：
E. Wilson;J. Nordhaus;J. Nordhaus
双白色矮人（DWD）的形成通道和预测的人群很重要，因为子集将演变为IA型超新星的重力波源和/或祖细胞。鉴于观察到的短期DWD的群体，我们计算包括对流效应时的共同包膜（CE）演变的结果。对于DWD系统中的每个观察到的白矮人（WD），我们从全面的恒星演化模型套件中鉴定出所有具有等效原始WD核心质量的祖细胞。在第二个将WD视为同伴的情况下，我们计算对流可以随着轨道衰变而释放的能量的条件，包括（如有必要）在CE阶段必须旋转多少信封。预测的CE后最终分离密切跟踪观察到的DWD轨道参数空间，进一步增强了对流是CE进化中的关键成分的观点。
The formation channels and predicted populations of double white dwarfs (DWDs) are important because a subset will evolve to be gravitational-wave sources and/or progenitors of Type Ia supernovae. Given the observed population of short-period DWDs, we calculate the outcomes of common envelope (CE) evolution when convective effects are included. For each observed white dwarf (WD) in a DWD system, we identify all progenitor stars with an equivalent proto-WD core mass from a comprehensive suite of stellar evolution models. With the second observed WD as the companion, we calculate the conditions under which convection can accommodate the energy released as the orbit decays, including (if necessary) how much the envelope must spin-up during the CE phase. The predicted post-CE final separations closely track the observed DWD orbital parameter space, further strengthening the view that convection is a key ingredient in CE evolution.