Breaking Giant Chains: Early-Stage Instabilities in Long-Period Giant Planet Systems
arxiv(2024)
摘要
Orbital evolution is a critical process that sculpts planetary systems,
particularly during their early stages where planet-disk interactions are
expected to lead to the formation of resonant chains. Despite the theoretically
expected prominence of such configurations, they are scarcely observed among
long-period giant exoplanets. This disparity suggests an evolutionary sequence
wherein giant planet systems originate in compact multi-resonant
configurations, but subsequently become unstable, eventually relaxing to wider
orbits–a phenomenon mirrored in our own solar system's early history. In this
work, we present a suite of N-body simulations that model the
instability-driven evolution of giant planet systems, originating from resonant
initial conditions, through phases of disk-dispersal and beyond. By comparing
the period ratio and normalized angular momentum deficit distributions of our
synthetic aggregate of systems with the observational census of long-period
Jovian planets, we derive constraints on the expected rate of orbital
migration, efficiency of gas-driven eccentricity damping, and typical initial
multiplicity. Our findings reveal a distinct inclination towards densely-packed
initial conditions, weak damping, and high giant planet multiplicities.
Furthermore, our models indicate that resonant chain origins do not facilitate
the formation of Hot Jupiters via the coplanar high-eccentricity pathway at
rates high enough to explain their observed prevalence.
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