AI 中文总结
研究紧密双星和恒星-行星系统中潮汐相互作用的能量转移，采用新型三层对流箱和外部周期性强迫量化潮汐耗散效率，得出单位质量潮汐功率随潮汐频率标度更浅等结果，还研究了旋转影响并讨论局限性与意义。
AI 中文摘要
对于紧密双星和恒星-行星系统，潮汐相互作用介导轨道运动与相关天体内部流动之间的能量转移，在其演化中起核心作用。对于平衡潮汐，相关能量转移通常通过作用于潮汐流的有效粘性建模。然而，粘性耗散效率随潮汐频率ω_T的标度仍有争议，特别是当ω_T大大超过对流涡旋周转频率ω_c时。以往数值研究通过使湍流对流流动受模拟平衡潮汐的振荡背景剪切来解决此问题。本文采用一种新型三层对流箱，由外部周期性强迫驱动，旨在代表夹在两个稳定层之间的恒星对流区。我们通过稳态下对流动的强迫功率量化潮汐耗散效率。结果表明，单位质量潮汐功率随ω_T的标度比早期剪切流模拟报道的更浅。这种标度与Terquem2021的预测一致，表明有效湍流粘性仅微弱依赖于ω_T，尽管我们的模拟限于ω_T≤10ω_c。此外，我们未发现反向能量转移（或“负粘性”）的证据，这一现象在一些先前剪切流模拟中观察到。我们还在同一局部框架内研究了旋转的影响。慢旋转（Ω≤ω_T）倾向于增强潮汐功率，而快旋转（Ω≥ω_T）显著抑制它。我们讨论了方法的局限性和研究结果的更广泛意义。
英文摘要
For close binaries and star-planet systems, tidal interactions mediate the energy transfer between the orbital motion and the internal flows of the bodies involved, thus playing a central role in their evolution. For equilibrium tides, the associated energy transfer is commonly modeled through an effective viscosity acting on the tidal flow. However, the scaling of viscous dissipation efficiency with tidal frequency $ω_\text{T}$ remains debated, particularly when $ω_\text{T}$ greatly exceeds the convective eddy turnover frequency $ω_\text{c}$. Previous numerical studies have addressed this issue by subjecting a turbulent convective flow to an oscillating background shear mimicking equilibrium tides. In this work, we adopt a novel three-layered convective box -- designed to represent a stellar convection zone sandwiched between two stable layers -- driven by an external periodic forcing. We quantify tidal dissipation efficiency by the forcing power on the flow in steady state. Our results yield a shallower scaling of tidal power per unit mass with $ω_\text{T}$ than reported in earlier shear-flow simulations. This scaling is consistent with the prediction by \cite{Terquem2021}, suggesting that the effective turbulent viscosity depends only weakly on $ω_\text{T}$, although our simulations are restricted to $ω_\text{T}\lesssim 10ω_\text{c}$. Moreover, we find no evidence of inverse energy transfer (or ``negative viscosity''), a phenomenon observed in some prior shear-flow simulations. We further investigate the influence of rotation within the same local framework. Slow rotation ($Ω\lesssim ω_\text{T}$) tends to enhance the tidal power, whereas fast rotation ($Ω\gtrsimω_\text{T}$) significantly suppresses it. We discuss the limitations of our approach and the broader implications of our findings.
Comments14 pages, 7 figures
