Abstract
Since 22 years, more than 3600 exoplanets have now been discovered in 2700 planetary systems, among which 610 host several planets. These discoveries reveal us a large diversity of planets, from super-Earths to hot Jupiters, orbiting host stars of different masses, ages, and metallicities. Moreover, the detected exoplanetary systems present a broad variety of orbital architectures that shows that the solar system is not typical. In addition, some of the detected telluric planets orbit within the habitable zone of their host stars. This challenges our understanding of the formation, the evolution, and the stability of planetary systems. In this context, tidal interactions should be coherently modeled taking advantage of the different observational signatures they have in our Earth-Moon system, in the solar system, and in exoplanetary systems. They reveal how tidal dissipation in celestial bodies varies strongly as a function of their internal structure and dynamics. In this chapter, we make a complete review of the physical mechanisms driving tidal friction in stars, giant planets, and telluric planets. For each type of celestial bodies, we discussed in details the state of the art of their modeling and how the resulting predictions compare to observations. We show the importance to adopt a stellar and planetary physicist perspective when studying tidal dissipation in planetary systems.
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Stéphane Mathis acknowledges funding by the European Research Council through ERC grant SPIRE 647383 and thanks ISSI for its support to the Encelade 200 team.
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Mathis, S. (2018). Tidal Star-Planet Interactions: A Stellar and Planetary Perspective. In: Deeg, H., Belmonte, J. (eds) Handbook of Exoplanets . Springer, Cham. https://doi.org/10.1007/978-3-319-55333-7_24
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