标题： 海洋潮汐在围绕低质量恒星运行的异步自转行星上 显示英文标题

标题： Ocean Tides on Asynchronously Rotating Planets Orbiting Low-mass Stars

摘要： 行星在低质量恒星的液态水宜居带内会经历大的潮汐力，是地球上的$10^3$到$10^4$倍，这是由于宜居带与恒星之间的距离较小。 因此，这些行星上的固体内潮、海洋潮汐和大气潮汐可能比地球上的强得多，但很少有研究明确模拟海洋潮汐。 在这里，我们首次进行了全球海洋潮汐模拟，并表明自转不同步且偏心率较大的行星上的海洋潮汐高度可达$\mathcal{O}(1000)\,\mathrm{m}$，流速可达$\mathcal{O}(10)\,\mathrm{m\,s^{-1}}$。 潮汐与海底地形之间的相互作用可以引起大的能量耗散，平均而言为$\sim\mathcal{O}(100)\,\mathrm{W\,m^{-2}}$。 这种潮汐能量耗散可以通过1到2个数量级显著加速轨道演化。 然而，对于偏心率较小的行星，海洋潮汐要弱得多，但仍与现代地球相当。 我们的结果表明，围绕低质量恒星运行的偏心行星上的海洋潮汐比地球上的强大几个数量级，可以显著影响地表地理和轨道演化。 显示英文摘要

摘要： Planets in the liquid-water habitable zone of low-mass stars experience large tidal forces, $10^3$ to $10^4$ times those on Earth, due to the small distance between the habitable zone and the host stars. Therefore, interior solid tides, ocean tides and atmospheric tides on these planets could be much stronger than that on Earth, but rare work has been done to explicitly simulate the ocean tides. Here, for the first time, we perform global ocean tide simulations and show that ocean tides on asynchronously rotating planets with large eccentricities can reach $\mathcal{O}(1000)\,\mathrm{m}$ in height and $\mathcal{O}(10)\,\mathrm{m\,s^{-1}}$ in flow speed. Interactions between tide and bottom topography can induce large energy dissipation, $\sim\mathcal{O}(100)\,\mathrm{W\,m^{-2}}$ in global mean. This tidal energy dissipation can strongly accelerate orbital evolution by 1-2 orders of magnitude. However, for planets with small eccentricities, the ocean tides are much weaker but still comparable to that on modern Earth. Our results suggest that ocean tides on eccentric planets orbiting low-mass stars are orders of magnitude more powerful than those on Earth and can dramatically influence surface geography and orbital evolution.