Abstract
The slow deformation of terrestrial orbits in the medium range, subject to lunisolar resonances, is well approximated by a family of Hamiltonian flow with $2.5$ degree-of-freedom. The action variables of the system may experience chaotic variations and large drift that we may quantify. Using variational chaos indicators, we compute high-resolution portraits of the action space. Such refined meshes allow to reveal the existence of tori and structures filling chaotic regions. Our elaborate computations allow us to isolate precise initial conditions near specific zones of interest and study their asymptotic behaviour in time. Borrowing classical techniques of phase- space visualisation, we highlight how the drift is mediated by the complement of the numerically detected KAM tori.
Highlights
Various groups of scientists have become enchanted anew by the lunisolar resonances affecting the dynamics of terrestrial orbits
The Hamiltonian flow obtained under the simplest assumptions for the disturbing effects of the perturbers, Moon and Sun, encapsulates all the details of the dynamics in which we are interested [7]
One method of choice to design effective dynamics relies on the Lagrangian averaging principle [21,22,23, 36], which has a long-lasting tradition in Celestial Mechanics
Summary
Various groups of scientists have become enchanted anew by the lunisolar resonances affecting the dynamics of terrestrial orbits. Later rebranded by Rossi [4] in the context of the medium-Earth orbits (MEOs), the study of their long-term dynamics, and in particular their eccentricity growths in the elliptic domain [5], represent current deep motivations for the community. The Hamiltonian flow obtained under the simplest assumptions for the disturbing effects of the perturbers (i.e., a development restricted to its lowest order and averaged over fast variables), Moon and Sun, encapsulates all the details of the dynamics in which we are interested [7]. We focus rather on (i) the physical consequences in terms of transport in the phase space and (ii) on the visualization of these excursions via double sections in the action-like phase space.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
