Scattering cold Jupiters disrupt inner mean-motion resonances via secular perturbations from their orbital history, driving resonance circulation in most 2:1 and 3:2 configurations and explaining the Kepler period ratio distribution.
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B., Matsumura, S., & Rasio, F
17 Pith papers cite this work. Polarity classification is still indexing.
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2026 17representative citing papers
First obliquity measurement in an M dwarf binary shows alignment, with tentative evidence that aligned orbits around cool stars and wide separations also hold for brown dwarfs and binaries.
Bi-CFM learns bidirectional mappings between initial and final state distributions to solve ill-posed inverse problems in chaotic systems, reporting metric improvements and speedups on Lorenz variants plus conservation-respecting results on three-body and globular cluster data.
GW190814 is proposed to originate from a collapsar-disk fragment merging with the central black hole, potentially preceded by SN2019npv ~60 days earlier, yielding H0 = 70.5 (+9.2, -6.4) km/s/Mpc.
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
Dynamical tides exciting f-modes during high-eccentricity migration produce the hot Jupiter pile-up, Neptune ridge, and Neptune desert via orbital circularization and selective atmospheric mass loss.
A new wide-binary coordinate system in REBOUND's TRACE integrator produces qualitatively correct results for planet-planet scattering, stellar flybys, and ZLK oscillations where prior hybrid integrators fail, while matching IAS15 accuracy at up to 9x speed.
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.
N-body simulations show that 14 Herculis's orbital architecture requires primordial ejection of an additional massive planet.
TOI-1710 b has a true obliquity of 149 degrees indicating retrograde motion, favoring high-eccentricity migration via planet-planet scattering and Kozai-Lidov cycles for this tidally detached super-Neptune.
A transit search on TESS Cycle 1 full-frame images produced 10,091 new planet candidates down to T=16 mag, more than doubling the known TESS total, with one hot Jupiter confirmed by radial velocity.
Archival RV and astrometric data plus three-body simulations constrain an unseen outer perturber in the GJ 436 system to sub-Jovian masses at a_c ≳ 6.8 AU, supporting Kozai-Lidov migration as the source of the hot Neptune's polar eccentric orbit.
N-body simulations demonstrate long-term dynamical stability of the HD 20794 system across a range of inclinations, with planet d identified as the lowest-mass high-eccentricity HZ-crossing planet.
Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.
TOI-159 b is confirmed as the hottest known eccentric hot Jupiter (e = 0.24) with a 13-sigma Keplerian detection around a young gamma Doradus star, including a preliminary low-resolution transmission spectrum.
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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Impact of Cold Jupiter Scattering on the Mean-Motion Resonance of Inner Small Planets
Scattering cold Jupiters disrupt inner mean-motion resonances via secular perturbations from their orbital history, driving resonance circulation in most 2:1 and 3:2 configurations and explaining the Kepler period ratio distribution.
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An Aligned Very-Low-Mass Star Orbiting an M dwarf and Obliquity Patterns Across Giant Planets, Brown Dwarfs, and Binary Stars
First obliquity measurement in an M dwarf binary shows alignment, with tentative evidence that aligned orbits around cool stars and wide separations also hold for brown dwarfs and binaries.
-
Solving Inverse Problems of Chaotic Systems with Bidirectional Conditional Flow Matching
Bi-CFM learns bidirectional mappings between initial and final state distributions to solve ill-posed inverse problems in chaotic systems, reporting metric improvements and speedups on Lorenz variants plus conservation-respecting results on three-body and globular cluster data.
-
A Collapsar-Disk Origin for GW190814
GW190814 is proposed to originate from a collapsar-disk fragment merging with the central black hole, potentially preceded by SN2019npv ~60 days earlier, yielding H0 = 70.5 (+9.2, -6.4) km/s/Mpc.
-
Planet-Planet Secular Migration Predicts a Stellar Obliquity-Period Anti-Correlation
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
-
Dynamical Tides during High-Eccentricity Migration produces the Hot Jupiter Pile-up, Neptune Ridge, and Neptune Desert
Dynamical tides exciting f-modes during high-eccentricity migration produce the hot Jupiter pile-up, Neptune ridge, and Neptune desert via orbital circularization and selective atmospheric mass loss.
-
A Coordinate System for Dynamical Instabilities in Hierarchical Systems in REBOUND
A new wide-binary coordinate system in REBOUND's TRACE integrator produces qualitatively correct results for planet-planet scattering, stellar flybys, and ZLK oscillations where prior hybrid integrators fail, while matching IAS15 accuracy at up to 9x speed.
-
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 Architecture of the 14 Herculis System Suggests Primordial Ejection of a Massive Planet
N-body simulations show that 14 Herculis's orbital architecture requires primordial ejection of an additional massive planet.
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A tidally detached super Neptune on a strongly misaligned retrograde orbit
TOI-1710 b has a true obliquity of 149 degrees indicating retrograde motion, favoring high-eccentricity migration via planet-planet scattering and Kozai-Lidov cycles for this tidally detached super-Neptune.
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Observational and Dynamical Constraints on an Unseen Outer Perturber in the GJ 436 Hot Neptune System
Archival RV and astrometric data plus three-body simulations constrain an unseen outer perturber in the GJ 436 system to sub-Jovian masses at a_c ≳ 6.8 AU, supporting Kozai-Lidov migration as the source of the hot Neptune's polar eccentric orbit.
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Dynamical Stability and Habitability in the HD 20794 System
N-body simulations demonstrate long-term dynamical stability of the HD 20794 system across a range of inclinations, with planet d identified as the lowest-mass high-eccentricity HZ-crossing planet.
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An Outer Giant Planet or Brown Dwarf in the 51 Pegasi System?
Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.
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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.