Hostname: page-component-cd9895bd7-q99xh Total loading time: 0 Render date: 2024-12-25T16:59:26.239Z Has data issue: false hasContentIssue false
  • English
  • Français

On the equilibrium rotation of Hot Jupiters in eccentric and excited orbits

Published online by Cambridge University Press:  10 November 2011

Alexandre C. M. Correia
Alexandre C. M. Correia*
Affiliation:
Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal email: [email protected] Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR 8028, 77 Avenue Denfert-Rochereau, 75014 Paris, France
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.

Hot-Jupiters are a common sub-class of exoplanets, which are enough close to the star to undergo tidal dissipation. The continuous action of tides modify the rotation of the planets until an equilibrium situation is reached. It is often assumed that synchronous motion is the most probable outcome of tidal evolution, since synchronous rotation is observed for the majority of the satellites in the Solar System. This is true for circular orbits, but when the orbits are eccentric, tidal effects are stronger when the planets are closer to the star, and therefore, the rotation rate tends to equalize the orbital speed rate at the pericenter (which is faster than synchronous rotation). An additional complication arises if the eccentricity is not constant and undergoes periodic perturbations from an external companion. Here we obtain an expression for the equilibrium rotation of Hot-Jupiters undergoing tidal dissipation and planetary perturbations. We show that for these planets, the equilibrium rotation rate is faster than for non-perturbed eccentric orbits.

Keywords

planetary systemscelestial mechanicsmethods: analytical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 287 - 294
Copyright
Copyright © International Astronomical Union 2011

References

Correia, A. C. M. & Laskar, J. 2004, Nature, 429, 848CrossRefGoogle Scholar
Correia, A. C. M. & Laskar, J. 2010, Icarus, 205, 338Google Scholar
Correia, A. C. M., Laskar, J., & Néron de Surgy, O. 2003, Icarus, 163, 1Google Scholar
Correia, A. C. M., Levrard, B., & Laskar, J. 2008, A&A 488, L63Google Scholar
Jacobson, R. A. 2001, BAAS, 33, 1039Google Scholar
Laskar, J. 1988, A&A, 198, 341Google Scholar
Mignard, F. 1979, Moon and Planets, 20, 301Google Scholar
Veras, D. & Ford, E. B. 2010, ApJ, 715, 803CrossRefGoogle Scholar
Wisdom, J., Peale, S. J., & Mignard, F. 1984, Icarus, 58, 137Google Scholar
Wright, J. T., Upadhyay, S., Marcy, G. W., et al. 2009, ApJ, 693, 1084CrossRefGoogle Scholar