SIMBAD references

By solving Laplace's tidal equations with friction terms, we study the surface tide on a rapidly rotating body. When ε= Ω²R/g (i.e. the square of the ratio of the dynamical time-scale to the rotational time-scale) is very small for the Earth, the asymptotic result is derived. When it is not so small (e.g. for a rapidly rotating star or planet), we perform numerical calculations. It is found that when rotation is sufficiently fast (εreaches 0.1), a great amount of tidal resonances appear. To generate the same level of tide, a faster rotation corresponds to a lower tidal frequency. Friction suppresses tidal resonances but it cannot completely suppress them at fast rotation. The thickness of the fluid layer can change tidal resonances but this change becomes weaker at faster rotation. This result can help us to understand tides in the atmosphere of a rapidly rotating star or planet, or in the ocean of a neutron star.