Rotation and figure evolution in the creep tide theory: a new approach and application to Mercury

Autor(es)

Gomes, G. O. ^[1] ; Folonier, H. A. ^[1] ; Ferraz-Mello, S. ^[1]

Afiliação do(s) autor(es)

^[1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, SP - Brazil

• Tipo de documento: Artigo Científico
• Fonte: CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY; v. 131, n. 12 DEC 2019.
• Citações Web of Science: 0

Resumo

This paper deals with the rotation and figure evolution of a planet near the 3/2 spin-orbit resonance and the exploration of a new formulation of the creep tide theory (Folonier et al. in Celest Mech Dyn Astron 130:78, 2018). This new formulation is composed by a system of differential equations for the figure and the rotation of the body simultaneously (which is the same system of equations used in Folonier et al. 2018), different from the original one (Ferraz-Mello in Celest Mech Dyn Astron 116:109-140, 2013; Celest Mech Dyn Astron 122:359-389, 2015a. ) in which rotation and figure were considered separately. The time evolution of the figure of the body is studied for both the 3/2 and 2/1 spin-orbit resonances. Moreover, we provide a method to determine the relaxation factor gamma of non-rigid homogeneous bodies whose endpoint of rotational evolution from tidal interactions is the 3/2 spin-orbit resonance, provided that (i) an initially faster rotation is assumed and (ii) no permanent components of the flattenings of the body existed at the time of the capture in the 3/2 spin-orbit resonance. The method is applied to Mercury, since it is currently trapped in a 3/2 spin-orbit resonance with its orbital motion and we obtain 4.8x10-8. The equatorial prolateness and polar oblateness coefficients obtained for Mercury's figure with such range of values of gamma are the same as the ones given by the Darwin-Kaula model (Matsuyama and Nimmo in J Geophys Res 114, E01010, 2009). However, comparing the values of the flattenings obtained for such range of gamma with those obtained from MESSENGER's measurements (Perry et al. in Geophys. Res. Lett. 42, 6951-6958, 2015), we see that the current values for Mercury's equatorial prolateness and polar oblateness are 2-3 orders of magnitude larger than the values given by the tidal theories. (AU)

• Processo FAPESP: 17/25224-0 - Aplicação da teoria das marés planetárias a exoplanetas e satélites planetários
• Beneficiário: Gabriel de Oliveira Gomes
• Modalidade de apoio: Bolsas no Brasil - Doutorado Direto
• Processo FAPESP: 16/20189-9 - Evolução dinâmica devida à maré em exoplanetas e satélites diferenciados
• Beneficiário: Hugo Alberto Folonier
• Modalidade de apoio: Bolsas no Brasil - Pós-Doutorado
• Processo FAPESP: 16/13750-6 - O Brasil no espaço: Astrofísica e Engenharia
• Beneficiário: Eduardo Janot Pacheco
• Modalidade de apoio: Auxílio à Pesquisa - Projetos Especiais