Secular dynamics of planetesimals in tight binary systems: Application to Gamma-Cephei

TL;DR

This paper develops a second-order secular theory for small planetesimals in tight binary systems, applies it to Gamma-Cephei, and finds that planetary formation likelihood is robust against orbital uncertainties.

Contribution

It introduces a second-order analytical model for secular dynamics in binary systems and reassesses Gamma-Cephei's orbital configurations affecting planetesimal evolution.

Findings

Second-order theory improves accuracy over first-order for large semimajor axes.

Planetary formation in Gamma-Cephei is insensitive to orbital fit variations.

Planetesimals can be trapped in mean-motion resonances during divergent migration.

Abstract

The secular dynamics of small planetesimals in tight binary systems play a fundamental role in establishing the possibility of accretional 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. We construct a second-order theory (with respect to the masses) for the planar secular motion of small planetasimals and deduce new expressions for the forced eccentricity and secular frequency. We also reanalyze the radial velocity data available for Gamma-Cephei and present a series of orbital solutions leading to residuals compatible with the best fits. Finally, we discuss how different orbital configurations for Gamma-Cephei may affect the dynamics of small bodies in circunmstellar motion. For Gamma-Cephei, we find that the classical first-order expressions for the secular frequency and forced eccentricity lead to large inaccuracies around 50 % for semimajor axes larger than one tenth the orbital separation between the stellar components. Low eccentricities and/or masses reduce the importance of the second-order terms. The dynamics of small planetesimals only show a weak dependence with the orbital fits of the stellar components, and the same result is found including the effects of a nonlinear gas drag. Thus, the possibility 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 that planetesimals migrating because of gas drag may be trapped in mean-motion resonances with the binary, even though the migration is divergent.