潮汐锁定熔岩星球的海洋环流 第一部分：一个理想化二维数值模型
Ocean Circulation on Tide-locked Lava Worlds, Part I: An Idealized 2D Numerical Model
AI总结：
本研究针对潮汐锁定熔岩星球，利用自主开发的理想化二维模型模拟其海洋环流与深度，发现岩浆洋深度远浅于传统对流假设的预测，且海洋环流对热相位曲线的观测影响极小。
摘要：
若表面温度超过典型地壳的熔融温度，潮汐锁定行星的昼侧预计会存在岩浆洋。作为詹姆斯·韦伯空间望远镜（JWST）的高优先级观测目标，熔岩行星的表面与大气相关信息很快将被获取。以往多数熔岩行星研究通常假设该系统处于强对流且等熵的状态，这意味着由绝热线和熔融曲线决定的岩浆洋深度可达$O$($10^4$--$10^5$)米。本研究中，我们利用作者开发的理想化二维（x-z）模型，模拟潮汐锁定熔岩星球的海洋环流与海洋深度。模拟结果显示，在内部热源为零或较小的情况下，最大纬向流速范围为0.1--1.0米每秒，岩浆洋深度保持在$O$(100)米量级，比完全对流系统预测的深度浅100倍以上。我们证实，海洋热输送辐散始终比恒星入射辐射小1--2个数量级。因此，观测中海洋环流对潮汐锁定熔岩星球热相位曲线的影响极小。
英文摘要：
A magma ocean is expected to exist on the dayside of tide-locked planets if surface temperature exceeds the melting temperature of typical crust. As highly prioritized targets for the James Webb Space Telescope (JWST), more information about the surface and atmosphere of lava planets will soon be available. In most previous studies of lava planets, the system is typically assumed to be vigorously convecting and isentropic. This implies a magma ocean depth reaching $O$($10^4$--$10^5$) m, determined by the adiabats and melting curves. In this study, we aim to simulate ocean circulation and ocean depth on tidally locked lava worlds using an idealized 2D (x-z) model developed by the authors. Our simulation results show that under zero or a small internal source, the maximum zonal current speed ranges from 0.1--1.0 m s$^{-1}$ and the magma ocean depth remains $O$(100) m, being more than 100 times shallower than that predicted in a fully convecting system. We demonstrate that the ocean heat transport divergence is consistently smaller than the stellar insolation by 1--2 orders of magnitude. Consequently, the impact of ocean circulation on the thermal phase curve of tidally locked lava worlds is minimal in observations.
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