Artigo
Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology
Registro en:
Astronomy &astrophysics. Les Ulis Cedex A: Edp Sciences S A, v. 571, p. 1-16, 2014.
0004-6361
10.1051/0004-6361/201424211
WOS:000345282600061
Autor
Correia, Alexandre C. M.
Bouee, Gwenacl
Laskar, Jacques
Rodrieguez, Adrian [UNESP]
Resumen
In this paper we present a new approach to tidal theory. Assuming a Maxwell viscoelastic rheology, we compute the instantaneous deformation of celestial bodies using a differential equation for the gravity field coefficients. This method allows large eccentricities and it is not limited to quasi-periodic perturbations. It can take into account an extended class of perturbations, including chaotic motions and transient events. We apply our model to some already detected eccentric hot Jupiters and super-Earths in planar configurations. We show that when the relaxation time of the deformation is larger than the orbital period, spin-orbit equilibria arise naturally at half-integers of the mean motion, even for gaseous planets. In the case of super-Earths, these equilibria can be maintained for very low values of eccentricity. Our method can also be used to study planets with complex internal structures and other rheologies. PNP-CNRS CS of Paris Observatory France-Portugal program FCT-Portugal Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014 Paris, France Departamento de Física, I3N, Universidade de Aveiro, Campus de Santiago, 3810-193 Aveiro, Portugal. Instituto de Geociências e Ciências Exatas, UNESP, Av. 24-A 1515, CEP 13506-900, Rio Claro, SP, Brazil France-Portugal program: PICS05998 FCT-Portugal: PEst-C/CTM/LA0025/2011 FAPESP: 2009/16900-5 FAPESP: 2012/13731-0