Secular dynamics of planetesimals in tight binary systems: application to \gamma-Cephei

GIUPPONE, C. A. ; LEIVA, A. M.; CORREA-OTTO, J. Y BEAUGE, C.

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Año: 2011 vol. 230 p. 103 - 113

0004-6361

Context. The secular dynamics of small planetesimals in tight binary systems play a fundamental role in establishing the possibility ofaccretional collisions in such extreme cases. The most important secular parameters are the forced eccentricity and secular frequency,which depend on the initial conditions of the particles, as well as on the mass and orbital parameters of the secondary star.Aims. We construct a second-order theory (with respect to the masses) for the planar secular motion of small planetasimals and deducenew expressions for the forced eccentricity and secular frequency. We also reanalyze the radial velocity data available for γ-Cepheiand present a series of orbital solutions leading to residuals compatible with the best fits. Finally, we discuss how different orbitalconfigurations for γ-Cephei may affect the dynamics of small bodies in circumstellar motion.Methods. The secular theory is constructed using a Lie series perturbation scheme restricted to second order in the small parameter.The orbital fits were analyzed with a minimization code that employs a genetic algorithm for a preliminary solution plus a simulatedannealing for the fine tuning.Results. For γ-Cephei, we find that the classical first-order expressions for the secular frequency and forced eccentricity lead to largeinaccuracies \sim 50% for semimajor axes larger than one tenth the orbital separation between the stellar components. Low eccentricitiesand/or masses reduce the importance of the second-order terms. The dynamics of small planetesimals only show a weak dependencewith the orbital fits of the stellar components, and the same result is found including the effects of a nonlinear gas drag. Thus, thepossibility of planetary formation in this binary system largely appears insensitive to the orbital fits adopted for the stellar components,and any future alterations in the system parameters (due to new observations) should not change this picture. Finally, we show thatplanetesimals migrating because of gas drag may be trapped in mean-motion resonances with the binary, even though the migrationis divergent.