SHARD is a collision-resolution framework that interpolates SPH results for remnants and clusters unresolved debris into N-body fragments while enforcing mass and water conservation for planet formation simulations.
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A new three-point inverse solution using the α-β model reconstructs meteoroid masses and bulk densities from limited fireball observations, achieving 88% convergence on the EN catalog and producing a continuous density range of 300-4000 kg m^{-3} instead of discrete PE categories.
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.
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.
Dynamical simulations show mm-sized meteoroids impacting Earth below 17 km/s are mostly asteroidal if released in the last 150-200 kyr, with cometary fraction rising above that speed and dominating above 27 km/s.
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.
Scattering between close-in super-Earths and secularly perturbed cold planets can launch some planets into free-floating orbits.
Simulations indicate EKL interactions excite TTV phases and disrupt resonances in a significant fraction of near-resonant super-Earth systems over 16 Myr.
Dust particles inspiraling under PR drag are temporarily trapped in MMRs, escape due to overstability of librations, then undergo stochastic scattering with predicted fractions for planetary collision, sublimation, or ejection via an analytic epicycle model and Monte Carlo method.
N-body simulations show that 14 Herculis's orbital architecture requires primordial ejection of an additional massive planet.
N-body simulations demonstrate that post-capture chaotic planet-planet interactions around pulsars can produce stable low-eccentricity orbits after ejections.
Viscous stirring via gravitational scattering produces lognormal inclination distributions that yield Lorentzian vertical density profiles, which relax to Gaussians after equipartition, enabling estimates of perturber masses in ARKS debris disks.
General relativity induces three regions of orbital instability for misaligned low-eccentricity test particles around binaries, extending to about 8 binary semimajor axes.
Detection and characterization of two eccentric warm Jupiters TOI-2147 b (P=26.2 d, e=0.29, M=116 M⊕) and TOI-6019 b (P=14.5 d, e=0.48, M=149 M⊕) with TESS and MaHPS data, showing mildly inflated radii consistent with tidal heating.
citing papers explorer
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Clustering SPH Debris into N-body Fragments: A Collisional Code for Planet Formation
SHARD is a collision-resolution framework that interpolates SPH results for remnants and clusters unresolved debris into N-body fragments while enforcing mass and water conservation for planet formation simulations.
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Consistency between dynamical modeling and photometrically derived masses of fireballs
A new three-point inverse solution using the α-β model reconstructs meteoroid masses and bulk densities from limited fireball observations, achieving 88% convergence on the EN catalog and producing a continuous density range of 300-4000 kg m^{-3} instead of discrete PE categories.
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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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The Dynamical Origin of Millimetre-Sized Sporadic Meteoroids
Dynamical simulations show mm-sized meteoroids impacting Earth below 17 km/s are mostly asteroidal if released in the last 150-200 kyr, with cometary fraction rising above that speed and dominating above 27 km/s.
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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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A Robust Launching Mechanism for Freely-Floating Planets from Host Stars with Close-in Planets
Scattering between close-in super-Earths and secularly perturbed cold planets can launch some planets into free-floating orbits.
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Resonant Super-Earths Dancing With EKL Oscillations: TTV Phase Excitation and Resonance Disruption by EKL Interactions between a Cold Jupiter and Stellar Companion
Simulations indicate EKL interactions excite TTV phases and disrupt resonances in a significant fraction of near-resonant super-Earth systems over 16 Myr.
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Resonance and Stochastic Dynamics of Interplanetary Dust
Dust particles inspiraling under PR drag are temporarily trapped in MMRs, escape due to overstability of librations, then undergo stochastic scattering with predicted fractions for planetary collision, sublimation, or ejection via an analytic epicycle model and Monte Carlo method.
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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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Viscously Stirring Particle Disks into Lorentzians and Gaussians to Infer Dynamical and Collisional Masses (ARKS XIII)
Viscous stirring via gravitational scattering produces lognormal inclination distributions that yield Lorentzian vertical density profiles, which relax to Gaussians after equipartition, enabling estimates of perturber masses in ARKS debris disks.
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Relativistic Effects on Circumbinary Orbit Stability
General relativity induces three regions of orbital instability for misaligned low-eccentricity test particles around binaries, extending to about 8 binary semimajor axes.
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TOI-2147 b and TOI-6019 b: Two eccentric warm Jupiters detected and characterized with TESS and MaHPS
Detection and characterization of two eccentric warm Jupiters TOI-2147 b (P=26.2 d, e=0.29, M=116 M⊕) and TOI-6019 b (P=14.5 d, e=0.48, M=149 M⊕) with TESS and MaHPS data, showing mildly inflated radii consistent with tidal heating.