The atmosphere of TOI-1130b shows high metallicity, low C/O, and elevated mean molecular weight consistent with ex-situ formation beyond the water ice line.
Title resolution pending
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
fields
astro-ph.EP 6years
2026 6representative citing papers
Direct imaging reveals enhanced metallicity and aligned orbit in 29 Cyg b, supporting protoplanetary disk formation near the deuterium burning limit.
Coupled thermal-chemical models indicate that sub-Neptunes formed outside the water-ice line exhibit high atmospheric CH4, H2O, and C/O ratios while those formed inside show suppressed CH4 and low C/O.
DALI modeling with updated warm chemistry finds C2H2/H2O IR flux ratio in T Tauri disks is sensitive to C/O, total O/H, and small-grain abundance, with JWST data suggesting sub-unity C/O and common enhanced O/H.
ML regressors trained on APOGEE DR17 red giants predict C, O, Mg, Si abundances from kinematics and [Fe/H] more accurately than [Fe/H] baseline, with external validation on HARPS FGK dwarfs and reproduction of Galactic chemical evolution trends.
An optimal Stokes number window of 0.01-0.03 allows streaming instability to form planetesimals and pebble accretion to build all three main planet classes, with cold gas giants needing the lowest turbulence and largest discs.
citing papers explorer
-
JWST unveils a high mean molecular weight atmosphere for mini-Neptune TOI-1130b: Evidence for formation beyond the water ice line
The atmosphere of TOI-1130b shows high metallicity, low C/O, and elevated mean molecular weight consistent with ex-situ formation beyond the water ice line.
-
Direct Images of CO2 Absorption in the Atmosphere of a Super-Jupiter: Enhanced Metallicity Suggestive of Formation in a Disk
Direct imaging reveals enhanced metallicity and aligned orbit in 29 Cyg b, supporting protoplanetary disk formation near the deuterium burning limit.
-
Coupled Thermal-Chemical Evolution Models of Sub-Neptunes Reveal Atmospheric Signatures of Their Formation Location
Coupled thermal-chemical models indicate that sub-Neptunes formed outside the water-ice line exhibit high atmospheric CH4, H2O, and C/O ratios while those formed inside show suppressed CH4 and low C/O.
-
Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties
DALI modeling with updated warm chemistry finds C2H2/H2O IR flux ratio in T Tauri disks is sensitive to C/O, total O/H, and small-grain abundance, with JWST data suggesting sub-unity C/O and common enhanced O/H.
-
Inferring stellar metallicity and elemental abundances from kinematic and spectroscopic data using machine learning -- Implications for exoplanet host stars
ML regressors trained on APOGEE DR17 red giants predict C, O, Mg, Si abundances from kinematics and [Fe/H] more accurately than [Fe/H] baseline, with external validation on HARPS FGK dwarfs and reproduction of Galactic chemical evolution trends.
-
Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
An optimal Stokes number window of 0.01-0.03 allows streaming instability to form planetesimals and pebble accretion to build all three main planet classes, with cold gas giants needing the lowest turbulence and largest discs.