Secular Evolution of Planetary Systems in Binaries

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Scientific paper

Currently, 20% of extrasolar systems are associated with one or more stellar companions. Most of them are hierarchical systems in which the ratio of the planet's semimajor axis (apl) to the binary semimajor axis (ab) is small (apl / ab < 40°) with respect to the binary plane. Consequently, the planetary eccentricity and inclination oscillate on secular timescales while the semimajor axis remains nearly constant.
We investigate the evolution of hierarchical four-body systems in which two planets orbit a component of a wide stellar binary. With the presence of the other planet and a stellar companion, orbital precession is caused either by the Kozai oscillation (dv/dt|Koz) or the secular planet-planet interaction (dv/dt|PP). Kozai oscillations are suppressed when the timescale of the secular interaction between planets is shorter than the Kozai precession rate, i.e., (dv/dt|PP) / (dv/dt|Koz) < 1. However, when the two precession frequencies are comparable, the orbital elements of the planets evolve in a highly chaotic manner. When the planets can maintain the Hill stability throughout their evolutions, the outer planet with secularly oscillating eccentricity typically locks the inner planet into synchronized eccentricity oscillations. In such synchronized oscillations the outer planet propagates the torque from the stellar companion and excites the eccentricity of the inner planet on a timescale shorter than the direct perturbation by the companion star.

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