research_article
213-224
en
Our purpose is to build a model of rotation for a rigid Mercury, involving the planetary perturbations and the non-spherical shape of the planet. The approach is purely analytical, based on Hamiltonian formalism; we start with a first-order basic averaged resonant potential (including J2 and C22, and the first powers of the eccentricity and the inclination of Mercury). With this kernel model, we identify the present equilibrium of Mercury; we introduce local canonical variables, describing the motion around this 3:2 resonance. We perform a canonical untangling transformation, to generate three sets of action-angle variables, and identify the three basic frequencies associated to this motion. We show how to reintroduce the short-periodic terms, lost in the averaging process, thanks to the Lie generator; we also comment about the damping effects and the planetary perturbations. At any point of the development, we use the model SONYR to compare and check our calculations.
articles
2019-04-11T14:29
https://scigraph.springernature.com/explorer/license/
2006-05
The 3:2 spin-orbit resonant motion of Mercury
http://link.springer.com/10.1007%2Fs10569-006-9032-y
false
2006-05-01
Springer Nature - SN SciGraph project
Nicolas
Rambaux
readcube_id
8e55a8bfdc36efe8e4b2438d7f912e8c2e65cab7a9b9ca2c1188276535f00640
Psychology
University of Namur
Département de mathématique, FUNDP, Rempart de la Vierge, 8, 5000, Namur, Belgium
Psychology and Cognitive Sciences
Sandrine
D’Hoedt
Anne
Lemaitre
pub.1029877442
dimensions_id
10.1007/s10569-006-9032-y
doi
0923-2958
Celestial Mechanics and Dynamical Astronomy
0008-8714
95
1-4