Formation and evolution of the two 4/3 resonant giants planets in HD 200946

TL;DR

This paper investigates the formation and stability of two giant planets in the 4/3 mean-motion resonance around HD 200964, updating orbital parameters and proposing a formation scenario consistent with observed dynamics.

Contribution

It provides the first detailed formation scenario for two giant planets in the 4/3 resonance, matching observed orbital parameters and stability constraints.

Findings

Formation simulations reproduce the 4/3 resonance dynamics.

Stable evolution is sensitive to planetary masses and disk parameters.

Narrow stable region aligns with the best-fit orbital configuration.

Abstract

It has been suggested that HD 200964 is the first exoplanetary system with two Jovian planets evolving in the 4/3 mean- motion resonance. Previous scenarios to simulate the formation of two giant planets in the stable 4/3 resonance configuration have failed. Moreover, the orbital parameters available in the literature point out an unstable configuration of the planetary pair. The purpose of this paper is i) to determine the orbits of the planets from the RV measurements and update the value of the stellar mass (1.57 M), ii) to analyse the stability of the planetary evolution in the vicinity and inside the 4/3 MMR, and iii) to elaborate a possible scenario for the formation of systems in the 4/3 MMR. The results of the formation simulations are able to very closely reproduce the 4/3 resonant dynamics of the best-fit config- uration obtained in this paper. Moreover, the confidence interval of the fit matches well with the very narrow stable region of the 4/3 mean-motion resonance. The formation process of the HD 200964 system is very sensitive to the planetary masses and protoplanetary disk parameters. Only a thin, flat disk allows the embryo-sized planets to reach the 4/3 resonant configuration. The stable evolution of the resonant planets is also sensitive to the mass of the central star, because of overlapping high-order resonances inside the 4/3 resonance. Regardless of the very narrow domain of stable motion, the confidence interval of our fit closely matches the stability area.