AI 中文总结
通过对可观测的共包层后双星正向建模，系统测试共包层演化形式体系，对比α、两阶段和SCATTER形式体系预测结果，发现基于能量的形式体系最准确，更多观测可限制复合能量贡献及结果随供体质量的变化。
AI 中文摘要
我们通过对可观测的共包层后双星进行正向建模，对共包层演化的形式体系进行了系统测试。我们将α形式体系、两阶段形式体系和SCATTER形式体系的预测结果与观测到的共包层后双星进行了比较，包括具有超大质量白矮星的宽双星和行星状星云的中心双星。基于角动量的SCATTER形式体系即使调整参数也无法预测出与观测到的完整样本相匹配的样本。我们认为这表明使用轨道角动量平衡来预测共包层结果存在根本挑战。基于能量的α形式体系和混合两阶段形式体系都能很好地复制观测到的样本。αCE~0.2-0.3可以匹配当前的观测结果，与之前的研究一致。复合能量是必要的，但只有一小部分（~10-40%）能够贡献，以便在正确的轨道周期预测出具有超大质量白矮星的IK Peg类双星。我们的工作表明，基于能量的形式体系在预测共包层结果方面仍然是最准确的，但更多的观测可以限制复合能量的贡献以及这些结果如何随供体质量系统地变化。
英文摘要
We present a systematic test of formalisms for common envelope evolution by forward-modelling observable post-common envelope binaries. We compare predictions from the $α$-formalism, and the Two-stage and SCATTER formalisms against observed post-common envelope binaries, including wide binaries with ultra-massive white dwarfs and central binaries of planetary nebulae. The angular momentum-based SCATTER formalism does not predict populations which match the complete observed population, even with adjustments to its parameters. We take this as indicative of fundamental challenges with using the orbital angular momentum balance to predict common envelope outcomes. The energy-based $α$ and hybrid Two-stage formalisms both well-replicate the observed population. $α_{\rm CE} \sim 0.2\text{--}0.3$ can match current observations, in agreement with previous works. Recombination energy is necessary, but only a fraction of it ($\sim\! 10\text{--}40\%$) can contribute in order to predict IK Peg-like binaries with ultra-massive white dwarfs at the correct orbital periods. Our work suggests energy-based formalisms remain the most accurate for predicting common envelope outcomes, but more observations can constrain the recombination contribution and how these outcomes systematically vary with the donor mass.
Comments30 pages, 14 (8+6) figures. Accepted at ApJ; updated version. Thanks to all for pre-print comments
