ENERGY DISSIPATION IN TIDAL ESTUARIES

Rías and Tidal-sea Estuaries

Tidal dissipation in Mars: where and how?

Introduction: The orbit of Phobos is secularly decaying at a rate which implies that Mars is highly dissipative; even more so than Earth’s mantle. Most tidal dissipation on Earth occurs within the oceans. Where and how the tidal energy dissipation occurs within Mars is not presently well constrained. We examine several alternatives, including a uniformly warm mantle, a partial melt zone within ...

Tidal Dissipation in Rotating Solar-type Stars

We calculate the excitation and dissipation of low-frequency tidal oscillations in uniformly rotating solar-type stars. For tidal frequencies smaller than twice the spin frequency, inertial waves are excited in the convective envelope and are dissipated by turbulent viscosity. Enhanced dissipation occurs over the entire frequency range rather than in a series of very narrow resonant peaks, and ...

Asymptotic behavior of tidal damping in alluvial estuaries

[1] Tidal wave propagation can be described analytically by a set of four implicit equations, i.e., the phase lag equation, the scaling equation, the damping equation, and the celerity equation. It is demonstrated that this system of equations has an asymptotic solution for an infinite channel, reflecting the balance between friction and channel convergence. Subsequently, explicit expressions f...

Tidal dissipation in rotating giant planets

Many extrasolar planets orbit sufficiently close to their host stars that significant tidal interactions can be expected, resulting in an evolution of the spin and orbital properties of the planets. The accompanying dissipation of energy can also be an important source of heat, leading to the inflation of short-period planets and even mass loss through Roche-lobe overflow. Tides may therefore p...