Water-rich formation produces CH4- and CO2-rich atmospheres while water-poor formation produces carbon-depleted ones, with soot boosting methane; the H2O/CH4-MMW plane diagnoses formation environment for JWST targets.
The Earth’s core as a reservoir of water
3 Pith papers cite this work, alongside 107 external citations. Polarity classification is still indexing.
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Coupling Bern formation models with extended chemical equilibrium including S and N shows equilibration depletes atmospheric nitrogen, shifts C/O higher outside the ice line, generates Si species, and leaves sulfur abundances weakly dependent on formation location.
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
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Atmospheric diversity of sub-Neptunes from formation with rock, water, and soot
Water-rich formation produces CH4- and CO2-rich atmospheres while water-poor formation produces carbon-depleted ones, with soot boosting methane; the H2O/CH4-MMW plane diagnoses formation environment for JWST targets.
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The Role of Formation Location in Shaping Sulfur-, Nitrogen-, and Carbon-Bearing Species in Super-Earth and Sub-Neptune Atmospheres
Coupling Bern formation models with extended chemical equilibrium including S and N shows equilibration depletes atmospheric nitrogen, shifts C/O higher outside the ice line, generates Si species, and leaves sulfur abundances weakly dependent on formation location.
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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.