An intercomparison of planetary evolution codes finds Earth magma oceans solidify in about 4 million years while Venus scenarios show more varied prolonged stages up to 50 million years, with outcomes sensitive to initial volatile budgets and model-specific treatments.
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Numerical model of C outgassing shows CC planetesimals deplete >50% carbon while NCs deplete <50% for typical sizes and formation times, favoring NC bodies as the main C source for terrestrial planets.
Young M dwarf flares exert greater chemical stress on primordial exo-Earth atmospheres than previous models, with potential for lasting changes in mixing ratios especially for low-abundance species.
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.
citing papers explorer
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Coupled atmospHere Interior modeL Intercomparison (CHILI). I. Evolutionary Modelling -- Primordial Magma Oceans of Earth and Venus
An intercomparison of planetary evolution codes finds Earth magma oceans solidify in about 4 million years while Venus scenarios show more varied prolonged stages up to 50 million years, with outcomes sensitive to initial volatile budgets and model-specific treatments.
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Modeling carbon outgassing from chondritic planetesimals
Numerical model of C outgassing shows CC planetesimals deplete >50% carbon while NCs deplete <50% for typical sizes and formation times, favoring NC bodies as the main C source for terrestrial planets.
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Stellar flare-driven evolution of primordial early exo-Earth atmospheres: Insights from a Young M Dwarf Flare model
Young M dwarf flares exert greater chemical stress on primordial exo-Earth atmospheres than previous models, with potential for lasting changes in mixing ratios especially for low-abundance species.
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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.