在早期沸腾流失背景下评估核心驱动的质量流失：亚海王星群体的极小长期质量流失
Assessing Core-Powered Mass Loss in the Context of Early Boil-Off: Minimal Long-Lived Mass Loss for the Sub-Neptune Population
AI总结：
本文开发了结合早期沸腾流失与长期核心驱动质量流失的亚海王星演化模型，发现核心驱动逃逸对小行星人口特征影响极小，仅能移除0.1%的H/He质量，且沸腾流失无法单独形成观测到的半径间隙。
摘要：
我们开发了一个基于 Python 的最先进亚海王星演化模型，该模型结合了年轻阶段（年龄 ≤ 1 Myr）的形成后沸腾流失（boil-off）和内部冷却导致的长期核心驱动质量流失（约 Gyrs）。我们研究了初始 H/He 熵、核心光度、能量平流、辐射大气结构以及向 XUV 驱动质量流失阶段的转变所起的作用，着眼于行星质量流失和热演化的相关时间尺度。特别关注 H/He 包层的重新平衡过程，包括为流体动力学风提供能量的能量来源和能量传输时间尺度，我们发现沸腾流失和核心驱动逃逸主要由恒星全波段辐射驱动。我们进一步发现，沸腾流失和核心驱动逃逸都与热演化解耦。我们表明，在考虑了初始 H/He 质量分数和初始熵的沸腾流失阶段后，沸腾流失后的核心驱动逃逸对小行星的人口统计特征影响微乎其微，因为它最多只能移除 0.1% 的 H/He 质量分数。我们的数值结果直接与先前关于个别演化轨迹和小行星群体的分析核心驱动质量流失模型工作进行了比较。我们检查了先前研究中做出的若干假设，这些假设导致了与我们的发现相比的显著差异。我们发现，尽管沸腾流失能够完全剥离高度辐射（F ≥ 100 F⊕）且具有低质量核心（Mc ≤ 4M⊕）的行星的气体包层，但其本身无法形成在观测群体中看到的明显半径间隙。
英文摘要：
We develop a python-based state-of-the-art sub-Neptune evolution model that incorporates both the post-formation boil-off at young ages $\leq$ 1 Myr and long-lived core-powered mass loss ($\sim$ Gyrs) from interior cooling. We investigate the roles of initial H/He entropy, core luminosity, energy advection, radiative atmospheric structure, and the transition to an XUV-driven mass-loss phase, with an eye on relevant timescales for planetary mass loss and thermal evolution. With particular attention to the re-equilibration process of the H/He envelope, including the energy sources that fuel the hydrodynamic wind, and energy transport timescales, we find boil-off and core-powered escape are primarily driven by stellar bolometric radiation. We further find that both boil-off and core-powered escape are decoupled from the thermal evolution. We show that, with a boil-off phase that accounts for the initial H/He mass fraction and initial entropy, post-boil-off core-powered escape has an insignificant influence on the demographics of small planets, as it is only able to remove at most 0.1% of the H/He mass fraction. Our numerical results are directly compared to previous work on analytical core-powered mass loss modeling for individual evolutionary trajectories and populations of small planets. We examine a number of assumptions made in previous studies that cause significant differences compared to our findings. We find that boil-off, though able to completely strip the gaseous envelope from a highly irradiated ($F \geq 100 F_\oplus$) planet that has a low-mass core ($M_c \leq 4M_\oplus$), cannot by itself form a pronounced radius gap as is seen in the observed population.
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