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Title:
Dynamical analysis of the Gliese-876 Laplace resonance
Authors:
Martí, J. G.; Giuppone, C. A.; Beaugé, C.
Affiliation:
AA(Universidad Nacional de Córdoba, Observatorio Astronómico, IATE, Laprida 854, X5000BGR Córdoba, Argentina; ), AB(Universidad Nacional de Córdoba, Observatorio Astronómico, IATE, Laprida 854, X5000BGR Córdoba, Argentina; Departamento de Física, I3N, Universidade de Aveiro, Campus de Santiago, P-3810-193 Aveiro, Portugal), AC(Universidad Nacional de Córdoba, Observatorio Astronómico, IATE, Laprida 854, X5000BGR Córdoba, Argentina)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 433, Issue 2, p.928-934 (MNRAS Homepage)
Publication Date:
08/2013
Origin:
OUP
Astronomy Keywords:
techniques: radial velocities, celestial mechanics, planets and satellites: formation
Abstract Copyright:
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stt765
Bibliographic Code:
2013MNRAS.433..928M

Abstract

The number of multiple-planet systems known to be involved in mean motion conmensurabilities has increased significantly since the Kepler mission. Although most correspond to two-planet resonances, multiple resonances have also been found. The Laplace resonance is a particular case of a three-body resonance in which the period ratio between consecutive pairs is n1/n2 ˜ n2/n3 ˜ 2/1. It is not clear how this triple resonance acts to stabilize (or not) the system.

The most reliable extrasolar system located in a Laplace resonance is GJ 876, because it has two independent confirmations. However, best-fit parameters were obtained without previous knowledge of resonance structure, and not all possible stable solutions for the system have been explored.

In the present work we explore the various configurations allowed by the Laplace resonance in the GJ 876 system by varying the planetary parameters of the third outer planet. We find that in this case the Laplace resonance is a stabilization mechanism in itself, defined by a tiny island of regular motion surrounded by (unstable) highly chaotic orbits. Low-eccentricity orbits and mutual inclinations from -20° to 20° are compatible with observations. A definite range of mass ratio must be assumed to maintain orbital stability. Finally, we provide constraints on the argument of pericentres and mean anomalies to ensure stability for this kind of system.

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