MORIA pipeline applied to HST data for KMT-2019-BLG-0253 halves the number of viable solutions and measures a 0.65 solar-mass host with a 7-9 Earth-mass planet at 2.64 kpc.
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10 Pith papers cite this work. Polarity classification is still indexing.
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Scattering between close-in super-Earths and secularly perturbed cold planets can launch some planets into free-floating orbits.
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.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
Simulations require 2000 Earth masses of pebbles to match observed disc gaps, but this produces mostly gas giants and few super-Earths, contradicting exoplanet data.
Three new planets detected via 2023 KMTNet microlensing with mass ratios log q ~ -1.9, -2.0, -2.6; overall 2023 sample of 25 planets matches prior mass-ratio distribution.
A new HST wide-field survey of the Galactic Bulge supplies high-angular-resolution data to enhance Roman exoplanet detections and serve as a community legacy dataset for stellar populations and dynamics.
An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
The Bern Model has incorporated MHD disk evolution, pebble accretion, and improved interiors, yielding quantitative matches to exoplanet mass functions, radius distributions, and system architectures.
citing papers explorer
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You Shall Not Pass (Without Modeling): High-Resolution Analysis of KMT-2019-BLG-0253 using MORIA
MORIA pipeline applied to HST data for KMT-2019-BLG-0253 halves the number of viable solutions and measures a 0.65 solar-mass host with a 7-9 Earth-mass planet at 2.64 kpc.
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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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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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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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Are the observed gaps in protoplanetary discs caused by growing planets?
Simulations require 2000 Earth masses of pebbles to match observed disc gaps, but this produces mostly gas giants and few super-Earths, contradicting exoplanet data.
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Mass Production of 2023 KMTNet Microlensing Planets. III: Three Planets from the Subprime Field
Three new planets detected via 2023 KMTNet microlensing with mass ratios log q ~ -1.9, -2.0, -2.6; overall 2023 sample of 25 planets matches prior mass-ratio distribution.
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An HST Wide Field Survey of the Galactic Bulge: Overview, Strategy, and First Results
A new HST wide-field survey of the Galactic Bulge supplies high-angular-resolution data to enhance Roman exoplanet detections and serve as a community legacy dataset for stellar populations and dynamics.
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Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.
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Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
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The formation of planetary systems: physics, populations, and architectures
The Bern Model has incorporated MHD disk evolution, pebble accretion, and improved interiors, yielding quantitative matches to exoplanet mass functions, radius distributions, and system architectures.