Sharp migration-rate gradients in protoplanetary disks quench resonant overstability when the dimensionless steepness parameter β exceeds the ratio of semi-major axis to eccentricity evolution timescales.
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Planetesimal disks with 1-4% of the planetary mass disrupt resonant Neptune chains, triggering instabilities that scatter planets to ~0.1 au orbits and enable hot Neptune formation on 10-100 Myr timescales.
Giant planet multiplicity is low, with 10.6% and 15.8% of Sun-like stars hosting at least one giant planet within 10 au across the two surveys, mostly as singles, inconsistent with scattering models.
citing papers explorer
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Suppression of Resonant Overstability at Sharp Migration Gradients
Sharp migration-rate gradients in protoplanetary disks quench resonant overstability when the dimensionless steepness parameter β exceeds the ratio of semi-major axis to eccentricity evolution timescales.
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Planetesimal-Driven Instabilities in Resonant Chains of Cold Neptunes and Their Dynamical Outcomes
Planetesimal disks with 1-4% of the planetary mass disrupt resonant Neptune chains, triggering instabilities that scatter planets to ~0.1 au orbits and enable hot Neptune formation on 10-100 Myr timescales.
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The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method. II. Constraints on Giant Planet Multiplicity from Different Surveys
Giant planet multiplicity is low, with 10.6% and 15.8% of Sun-like stars hosting at least one giant planet within 10 au across the two surveys, mostly as singles, inconsistent with scattering models.