AI 中文总结
研究恒星潮汐场中行星大气逃逸率，通过三维流体动力学模拟与一维模型对比，发现常用一维模型局限性，进而开发基于物理的混合模型，能准确预测质量损失率，优于含潮汐修正的一维模型。
AI 中文摘要
热驱动的大气逃逸，包括光蒸发和核心驱动的质量损失，在塑造近距离系外行星的演化中起关键作用，但当前多数模型依赖简化的一维大气逃逸描述。本文对嵌入太阳型主星引力势中的木星大小行星的大气外流进行三维流体动力学模拟，并与一维模型比较。通过改变洛希瓣填充程度和外流热状态探索多种构型。发现潮汐影响弱和高温风的系统产生近球形和各向同性外流，而更多洛希瓣填充和较冷风形成强各向异性和双尾结构。常用的一维帕克风模型仅在弱潮汐区表现良好，包含潮汐修正能合理估计质量损失率并捕捉所有区域的平均径向密度剖面，但无法再现外流从球形到潮汐结构尾过渡时本质的三维、角度相关特性。基于此结果，开发了一个基于物理的混合模型，经三维模拟校准，能准确预测所探索参数空间的质量损失率，且优于含潮汐修正的一维模型。
英文摘要
Thermally driven atmospheric escape, including photo-evaporation and core-powered mass-loss, plays a key role in shaping the evolution of close-in exoplanets, yet most current models rely on simplified one-dimensional descriptions of atmospheric escape. In this work, we perform 3D hydrodynamic simulations of atmospheric outflows from a Jupiter-sized planet embedded in the gravitational potential of a solar-type host star, and compare these results with 1D models to identify the regimes where they perform well and where they break down. We explore a range of configurations by varying the degree of Roche-lobe filling and the thermal state of the outflow. We find that systems with weak tidal influence and high-temperature winds produce nearly spherical and isotropic outflows, whereas more Roche-lobe-filling and cooler winds develop strong anisotropy and form two-tailed structures. We show that the commonly used 1D Parker wind model performs well only in the weak-tides regime, while including tidal corrections yields reasonable estimates of mass-loss rates and captures the mean radial density profile across all regimes, but fails to reproduce the intrinsically three-dimensional, angle-dependent nature of the flow as the outflow transitions from spherical to tidally structured tails. Motivated by these results, we develop a physically informed Mixture Model, calibrated using our 3D simulations, that accurately predicts mass-loss rates across the parameter space explored and outperforms 1D model with tidal corrections.
CommentsAccepted for publication in ApJ
