Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-27T00:25:48.242Z Has data issue: false hasContentIssue false
  • English
  • Français

On the computation of resonant tidal dissipation in the liquid layers of planets and stars

Published online by Cambridge University Press:  16 October 2024

Jérémy Rekier Open the ORCID record for Jérémy Rekier [Opens in a new window]  and
Santiago A. Triana
Jérémy Rekier*
Affiliation:
Royal Observatory of Belgium, 3 avenue circulaire, 1180 Brussels, Belgium Dpt. of Earth & Planetary Science, University of California, Berkeley, California 94720, USA
Santiago A. Triana
Affiliation:
Royal Observatory of Belgium, 3 avenue circulaire, 1180 Brussels, Belgium
*
email: jeremy.rekier@observatory.be
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Planets and stars have liquid layers that can support internal gravity waves and inertial waves respectively restored by the buoyancy and Coriolis forces. Both types of waves are excited by tides, leading to resonantly amplified dissipation. We review the theoretical formalism to compute these resonances and present some challenges and methods to overcome them.

Keywords

liquid layersbuoyancyCoriolistidesresonances
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S382: Complex Planetary Systems II: Latest Methods for an Interdisciplinary Approach , December 2022 , pp. 167 - 173
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Chandrasekhar, S. (1987). Ellipsoidal Figures of Equilibrium. Dover Books on Mathematics. Dover.Google Scholar
Dahlen, F. A. and Tromp, J. (1998). Theoretical Global Seismology. Princeton University Press.Google Scholar
De Boeck, I., Van Hoolst, T., and Smeyers, P. (1992). The subseismic approximation for low-frequency modes of the Earth applied to low-degree, low-frequency g-modes of non-rotating stars. Astronomy and Astrophysics, 259:167–174.Google Scholar
Dintrans, B. and Rieutord, M. (2001). A comparison of the anelastic and subseismic approximations for low-frequency gravity modes in stars. Monthly Notices of the Royal Astronomical Society, 324(3):635–642.CrossRefGoogle Scholar
Greenspan, H. P. (1968). The Theory of Rotating Fluids. Cambridge Monographs on Mechanics and Applied Mathematics. Cambridge U.P, London.Google Scholar
Hubbard, W. B. (2013). Concentric Maclaurin Spheroid Models Of Rotating Liquid Planets. ApJ, 768(1):43.CrossRefGoogle Scholar
Ogilvie, G. I. (2014). Tidal dissipation in stars and giant planets. Annual Review of Astronomy and Astrophysics, 52(1):171–210.CrossRefGoogle Scholar
Rekier, J., Trinh, A., Triana, S. A., and Dehant, V. (2019). Inertial modes in near-spherical geometries. Geophysical Journal International, 216(2):777–793.CrossRefGoogle Scholar
Triana, S. A., Dumberry, M., Cébron, D., Vidal, J., Trinh, A., Gerick, F., and Rekier, J. (2021). Core Eigenmodes and their Impact on the Earth’s Rotation. Surv Geophys.Google Scholar