Three accelerating stars yield one stellar companion at 166 AU, one 45 Jupiter-mass object at ~18 AU, and one 9.5 Jupiter-mass object at 6.4 AU that is 65% likely to be a planet.
Science276(5320), 1836–1839 (1997)
7 Pith papers cite this work. Polarity classification is still indexing.
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TOI-5882, a lithium-enriched subgiant with a brown dwarf companion, shows enrichment consistent with engulfment of a super-Earth to Neptune-mass planet.
Atmospheric retrievals yield C/O = 0.57±0.01, [M/H] = 0.18±0.05, and 12CO/13CO ≈ 95 for 2MASS J0249-0557 c, matching benchmark brown dwarfs and favoring star-like gravitational collapse over disk accretion.
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.
TOI-7154b is a 71.7 M_J brown dwarf in an 8.86-day eccentric orbit around a G star, with eccentricity and age suggesting stellar-like fragmentation origins.
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.
citing papers explorer
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Gaia Exoplanet Orbits, Demographics, and Evolution Survey (GEODES): Characteristics of Three Long-Period Companions Accelerating their Host Stars
Three accelerating stars yield one stellar companion at 166 AU, one 45 Jupiter-mass object at ~18 AU, and one 9.5 Jupiter-mass object at 6.4 AU that is 65% likely to be a planet.
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Lithium Enrichment in a Subgiant Star with a Brown Dwarf Companion: A Planetary Engulfment Candidate
TOI-5882, a lithium-enriched subgiant with a brown dwarf companion, shows enrichment consistent with engulfment of a super-Earth to Neptune-mass planet.
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Chemistry and Isotope Ratios of Substellar Atmospheres in the $\beta$ Pictoris Young Moving Group
Atmospheric retrievals yield C/O = 0.57±0.01, [M/H] = 0.18±0.05, and 12CO/13CO ≈ 95 for 2MASS J0249-0557 c, matching benchmark brown dwarfs and favoring star-like gravitational collapse over disk accretion.
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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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TOI-7154b: A Close-in Massive Brown Dwarf in an Eccentric Orbit
TOI-7154b is a 71.7 M_J brown dwarf in an 8.86-day eccentric orbit around a G star, with eccentricity and age suggesting stellar-like fragmentation origins.
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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.