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.
Three‐dimensional Interaction between a Planet and an Isothermal Gaseous Disk. I. Corotation and Lindblad Torques and Planet Migration
8 Pith papers cite this work, alongside 873 external citations. Polarity classification is still indexing.
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representative citing papers
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.
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by prolonging the lifetime of the circumprimary disc against truncation and photoevaporation.
Turbulent torques modeled as a Gaussian around the linear torque can push gas-induced dephasing in LISA EMRIs above the detection threshold for Eddington ratios above 0.3 and sufficient turbulence strength.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
Two migrating super-Earths in low-viscosity disks trigger narrow and broad dust substructures with high dust-to-gas ratios favorable for planetesimal formation.
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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$\alpha\beta q_\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
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A formation pathway for giant planets in S-type discs of {\gamma}-Cephei-like compact binaries
Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by prolonging the lifetime of the circumprimary disc against truncation and photoevaporation.
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Chaotic migration of LISA Extreme Mass Ratio Inspirals in a turbulent accretion disk: effect on waveform de-phasing
Turbulent torques modeled as a Gaussian around the linear torque can push gas-induced dephasing in LISA EMRIs above the detection threshold for Eddington ratios above 0.3 and sufficient turbulence strength.
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Constructing Earth Formation History Using Deep Mantle Noble Gas Reservoirs
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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On the Dust Substructures Triggered by Two Super-Earths Migrating in Low-viscosity Disks
Two migrating super-Earths in low-viscosity disks trigger narrow and broad dust substructures with high dust-to-gas ratios favorable for planetesimal formation.
- Eccentricity as a signature of hierarchical subsolar-mass mergers in collapsar disks