Scaling laws to understand tidal dissipation in fluid planetary layers and stars

TL;DR

This paper develops scaling laws to understand how viscous friction in fluid layers of stars and planets affects tidal dissipation, influencing the evolution of planetary systems.

Contribution

It introduces general scaling laws for tidal dissipation in fluid layers, emphasizing the effects of internal parameters and tidal frequency on dissipation behavior.

Findings

Dissipation sensitivity to tidal frequency

Impact of rotation, stratification, viscosity, and thermal diffusivity

Qualitative overview of fluid tidal wave behaviors

Abstract

Tidal dissipation is known as one of the main drivers of the secular evolution of planetary systems. It directly results from dissipative mechanisms that occur in planets and stars' interiors and strongly depends on the structure and dynamics of the bodies. This work focuses on the mechanism of viscous friction in stars and planetary layers. A local model is used to study tidal dissipation. It provides general scaling laws that give a qualitative overview of the different possible behaviors of fluid tidal waves. Furthermore, it highlights the sensitivity of dissipation to the tidal frequency and the roles played by the internal parameters of the fluid such as rotation, stratification, viscosity and thermal diffusivity that will impact the spins/orbital architecture in planetary systems.