A self-consistent weak friction model for the tidal evolution of circumbinary planets

LEIVA, A. M.; BEAUGÉ, C.; ZOPPETTI, F. A.; FOLONIER, H.; LEIVA, A. M.; BEAUGÉ, C.; ZOPPETTI, F. A.; FOLONIER, H.

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Año: 2019 vol. 627

0004-6361

We present a self-consistent model for the tidal evolution of circumbinary planets that is easily extensible to any other three-bodyproblem. Based on the weak-friction model, we derive expressions of the resulting forces and torques considering complete tidalinteractions between all the bodies of the system. Although the tidal deformation suffered by each extended mass must take intoaccount the combined gravitational effects of the other two bodies, the only tidal forces that have a net effect on the dynamic arethose that are applied on the same body that exerts the deformation, as long as no mean-motion resonance exists between the masses.As a working example, we applied the model to the Kepler-38 binary system. The evolution of the spin equations shows that theplanet reaches a stationary solution much faster than the stars, and the equilibrium spin frequency is sub-synchronous. The binarycomponents, on the other hand, evolve on a longer timescale, reaching a super-synchronous solution very close to that derived for thetwo-body problem. The orbital evolution is more complex. After reaching spin stationarity, the eccentricity was damped in all bodiesand for all the parameters analysed here. A similar effect is noted for the binary separation. The semimajor axis of the planet, on theother hand, may migrate inwards or outwards, depending on the masses and orbital parameters. In some cases the secular evolutionof the system may also exhibit an alignment of the pericenters, requiring the inclusion of additional terms in the tidal model. Finally,we derived analytical expressions for the variational equations of the orbital evolution and spin rates based on low-order ellipticalexpansions in the semimajor axis ratio α and the eccentricities. These are found to reduce to the well-known two-body case whenα → 0 or when one of the masses is taken as equal to zero. This model allows us to find a closed and simple analytical expression forthe stationary spin rates of all the bodies, as well as predicting the direction and magnitude of the orbital migration.