AI 中文总结
该研究提出基于星团的框架重建白矮星+主序后共包层双星演化历史，以阿莱西12 - PCE双星验证此方法，测量相关参数，结合多种数据确定前身星情况，通过CE演化模型再现轨道分离，新框架可对共包层物理进行经验性约束。
AI 中文摘要
共包层（CE）演化是双星生命中的关键阶段，产生了Ia型超新星和引力波源的前身紧密双星。尽管其很重要，但由于具有受限的CE前后性质的系统稀缺，CE演化仍知之甚少。在此，我们提出了一个基于星团的框架来重建白矮星+主序（WD+MS）后CE双星的演化历史，其中星团成员身份可提供独立的年龄约束和/或排除WD的合并起源。我们用阿莱西12 - PCE验证了此方法，它是开放星团中首个具有精确确定的CE前后性质的此类双星。我们将伴星分类为M4V并测量出WD质量为$1.06 \pm 0.02 M_{\odot}$，使其成为与星团相关的最大质量WD+MS双星。通过径向速度监测确认在光变曲线中检测到的6.99小时周期性为双星轨道周期。结合WD质量、WD冷却年龄和阿莱西12星团年龄，恒星演化模型暗示一个$5.40 \pm 0.10 M_{\odot}$的WD前身在渐近巨星分支（AGB）进入了CE。对流是设定$\alpha_{\text{CE}}$的主导物理机制的CE演化模型在恰好两种情况下再现了观测到的轨道分离：要么是$\alpha_{\text{CE}}\approx0.99$的AGB中期相互作用，要么是$\alpha_{\text{CE}}\approx0.05$的AGB后期相互作用。我们的新框架适用于星团中的其他后CE双星，能够对仅从野外双星无法获得的CE物理进行经验性约束。
英文摘要
Common envelope (CE) evolution is a critical phase in the lives of binary stars, producing close binaries that are progenitors of type Ia supernovae and gravitational wave sources. Despite its importance, CE evolution remains poorly understood, largely due to the scarcity of systems with constrained pre- and post-CE properties. Here, we present a star cluster-based framework for reconstructing the evolutionary histories of white dwarf+main-sequence (WD+MS) post-CE binaries, where cluster membership can provide an independent age constraint and/or rule out a merger origin for the WD. We demonstrate this method with Alessi12-PCE, the first such binary in an open cluster with precisely determined pre- and post-CE properties. We classify the companion as an M4V and measure a WD mass of $1.06 \pm 0.02 M_{\odot}$, making it the most massive WD+MS binary associated with a cluster. A 6.99-hour periodicity detected in a light curve is confirmed as the binary orbital period via radial velocity monitoring. Combined with the WD mass, WD cooling age, and Alessi 12 cluster age, stellar evolution models imply a $5.40 \pm 0.10 M_{\odot}$ WD progenitor that entered a CE on the asymptotic giant branch (AGB). CE evolution models where convection is the dominant physical mechanism that sets $α_{\text{CE}}$ reproduce the observed orbital separation in exactly two scenarios: either a mid-AGB interaction with $α_{\text{CE}}\approx0.99$, or a late-AGB interaction with $α_{\text{CE}}\approx0.05$. Applicable to other post-CE binaries in star clusters, our new framework enables empirical constraints on CE physics inaccessible from field binaries alone.
Comments31 pages, 11 figures, 4 tables. Submitted to ApJ
