Abstract
The Lagrange case of the three body problem interacting through gravitational forces was perturbed from the circular Lagrange motion around the center of mass, to the motion in a near orbit. The perturbation motion was supposed to occur in the same plane of the unperturbed Lagrange solution. The computations were performed using new sets of coordinates introduced recently for the general three body problem.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
References
E. Piña, Celestial Mechanics and Dynamical Astronomy 74 (1999), 163.
E. Pina and L. Jiménez-lara l, Celestial Mechanics and Dynamical Astronomy 82 (2002), 1.
E.T. Whittaker, Analytical Dynamics of Particles and Rigid Bodies, Cambridge University Press, (1965),403.
C.L. Slegel and J. K. Moser Lectures on Celestial Mechanics, Springer Verlag, 1971.
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 2004 Springer Science+Business Media New York
About this paper
Cite this paper
Piña, E., Jiménez-Lara, L. (2004). Perturbing the Lagrange Solution to the General Three Body Problem. In: Delgado, J., Lacomba, E.A., Llibre, J., Pérez-Chavela, E. (eds) New Advances in Celestial Mechanics and Hamiltonian Systems. Springer, Boston, MA. https://doi.org/10.1007/978-1-4419-9058-7_8
Download citation
DOI: https://doi.org/10.1007/978-1-4419-9058-7_8
Publisher Name: Springer, Boston, MA
Print ISBN: 978-1-4613-4778-1
Online ISBN: 978-1-4419-9058-7
eBook Packages: Springer Book Archive