Tidal interactions shape period ratios in planetary systems with three-body resonant chains

Charalambous, C.; Teyssandier, J.; Libert, A.-S.

doi:10.1051/0004-6361/202345852

Cited by 5 publications

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

The nature of the Laplace resonance between the Galilean moons

Lari,

Saillenfest

2024

Celest Mech Dyn Astron

View full text Add to dashboard Cite

The Laplace resonance is a mean-motion resonance that involves the three inner Galilean moons of Jupiter. However, its true nature is in part unclear; in particular, different views can be found in the literature on whether the Laplace resonance is a pure three-body resonance or a mere superposition of two-body resonances. To settle this question, we conduct a thorough analysis of the many resonances involved, starting from the two-body 2:1 commensurabilities of the couples Io–Europa and Europa–Ganymede, and ending with the three-body 4:2:1 commensurability between the three moons. By artificially varying the parameters of the system and monitoring its fundamental frequencies, we cartography all resonances involved and their interactions. From the analysis of the individual 2:1 commensurabilities, we find that despite the oscillation of the resonant angles they are not genuine resonances, as the trajectory of the system in the phase space is not enclosed by separatrices. On the contrary, as suggested by previous works, we show that the only current true mean-motion resonance is the pure three-body resonance between all three satellites. Moreover, we find that the current values of the moons’ orbital elements make the Laplace resonance sufficiently separated from the individual two-body 2:1 resonances, preventing chaotic effects from appearing.

show abstract

The nature of the Laplace resonance between the Galilean moons

Lari,

Saillenfest

2024

Celest Mech Dyn Astron

View full text Add to dashboard Cite

show abstract

Dynamical stability of the Laplace resonance

Pucacco

2024

Celest Mech Dyn Astron

View full text Add to dashboard Cite

Searching for the grand tack in exoplanetary data

Cridland

2024

A&A

View full text Add to dashboard Cite

The grand tack model, more generally called the Masset and Snellgrove mechanism, is a planetary migration model whereby two giant planets via interactions with their natal disk migrated to larger orbital radii. While its relevance in our own Solar System remains in question, the fact that the Masset and Snellgrove mechanism is a general hydrodynamical effect implies that it may have occurred in another planetary system. In this study I searched through exoplanet data for evidence of the Masset and Snellgrove mechanism, which requires that (1) the inner of the two planets is more massive than the outer planet; (2) the planets are sufficiently massive that their gravity-induced gap overlaps; and (3) they orbit at sufficiently close radii that their co-rotation regions also overlap. The last two requirements are met when the planets orbit with a 3:2 mean motion resonance. I do not find conclusive evidence for a grand tack-like system, but find some evidence for planet formation at the edge of a planet-induced protoplanetary disk gap in three systems.

show abstract

Tidal interactions shape period ratios in planetary systems with three-body resonant chains

Cited by 5 publications

References 52 publications

The nature of the Laplace resonance between the Galilean moons

The nature of the Laplace resonance between the Galilean moons

Dynamical stability of the Laplace resonance

Searching for the grand tack in exoplanetary data

Contact Info

Product

Resources

About