Surface tide on a rapidly rotating body. (arXiv:1902.00859v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wei_X/0/1/0/all/0/1">Xing Wei</a>
By solving Laplace’s tidal equations with friction terms we study the surface
tide on a rapidly rotating body. When $epsilon=Omega^2 R/g$, the square of
the ratio of dynamical timescale to rotational timescale, is very small for the
Earth the asymptotic result was derived. When it is not so small, e.g. a
rapidly rotating star or planet, we perform numerical calculations. It is found
that when rotation is sufficiently fast ($epsilon$ reaches $0.1$) 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 cannot completely suppress them at fast rotation. The thickness
of fluid layer can change tidal resonances but this change becomes weaker at
faster rotation. This result is of help to understanding the tides in the
atmosphere of a rapidly rotating star or planet or in the ocean of a neutron
star.
By solving Laplace’s tidal equations with friction terms we study the surface
tide on a rapidly rotating body. When $epsilon=Omega^2 R/g$, the square of
the ratio of dynamical timescale to rotational timescale, is very small for the
Earth the asymptotic result was derived. When it is not so small, e.g. a
rapidly rotating star or planet, we perform numerical calculations. It is found
that when rotation is sufficiently fast ($epsilon$ reaches $0.1$) 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 cannot completely suppress them at fast rotation. The thickness
of fluid layer can change tidal resonances but this change becomes weaker at
faster rotation. This result is of help to understanding the tides in the
atmosphere of a rapidly rotating star or planet or in the ocean of a neutron
star.
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