Narrow-ring accretion models for terrestrial planets cannot reproduce bulk silicate Earth composition because embryos mix reduced and oxidized planetesimals early, requiring segregated reservoirs and late oxidized delivery.
Earth and Planetary Science Letters 271, 181–191
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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.
Simulations indicate that order-of-magnitude changes in TiO2 and SiO2 abundances in lava melts produce distinguishable TiO, SiO, and SiO2 features in dry lava planet emission spectra, potentially observable with 12 JWST eclipses for the brightest targets.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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.
Mars provides a real-world case study of processes like volatile loss, climate evolution, and magnetism that determine habitability on small rocky planets at the edge of habitable conditions.
citing papers explorer
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Oxidation Constraints on Terrestrial Planet Formation from a Ring
Narrow-ring accretion models for terrestrial planets cannot reproduce bulk silicate Earth composition because embryos mix reduced and oxidized planetesimals early, requiring segregated reservoirs and late oxidized delivery.
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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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Sensitivity of Dry Lava Planet Atmospheric Emission Spectra to Changes in Lava Compositions
Simulations indicate that order-of-magnitude changes in TiO2 and SiO2 abundances in lava melts produce distinguishable TiO, SiO, and SiO2 features in dry lava planet emission spectra, potentially observable with 12 JWST eclipses for the brightest targets.
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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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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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Mars as an Exoplanet: Lessons from a Planet at the Edge of Habitability
Mars provides a real-world case study of processes like volatile loss, climate evolution, and magnetism that determine habitability on small rocky planets at the edge of habitable conditions.