On the Efficacy of Ocean Formation with a Primordial Hydrogen Atmosphere
arXiv:2506.10417 · doi:10.1029/2024JE008786
Abstract
It has been suggested that Earth's present water budget formed from oxidation reactions between its initial hydrogen-rich primordial atmosphere and its magma ocean. Here we examine this hypothesis by building a comprehensive atmosphere-magma ocean model. We find that water formation is unlikely for two reasons. First, any water formed from oxidation reactions in the magma ocean would quickly outgass because of the water-poor atmosphere above. Second, the top boundary layer of the magma ocean becomes stable against convection because the oxidation reactions produce metallic iron, which sinks to the core of a growing Earth. This iron loss makes the top boundary layer significantly more buoyant than the rest of the magma, thus becoming stable against mixing. Our results suggest that hydrogen dissolution is unlikely to play a major role in the formation of Earth's oceans.
arXiv commentAccepted for publication in the Journal of Geophysical Research - Planets
References in corpus (45)
- Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
- Protoplanetary Disks and Their Evolution
- Rapid planetesimal formation in turbulent circumstellar discs
- Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks
- The origins and concentrations of water, carbon, nitrogen and noble gases on Earth
- Accretion Disks around Young Objects. I. The Detailed Vertical Structure
- Dynamics of Protoplanetary Disks
- Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets
- Making other Earths: Dynamical Simulations of Terrestrial Planet Formation and Water Delivery
- The locality of transport in self-gravitating accretion discs
- Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
- Atmospheres of protoplanetary cores: critical mass for nucleated instability
- The origin of the Moon within a terrestrial synestia
- Solar System Abundances of the Elements
- Analytical protostellar disk models 1: the effect of internal dissipation and surface irradiation on the structure of disks and the location of the snow line around Sun-like stars
- Constraints on the mass of a habitable planet with water of nebular origin
- Melting and Mixing States of the Earth's Mantle after the Moon-Forming Impact
- Hydrodynamics of Embedded Planets' First Atmospheres. II. A Rapid Recycling of Atmospheric Gas
- Ab Initio Equation of State for Hydrogen-Helium Mixtures with Recalibration of the Giant-Planet Mass-Radius Relation
- Steady-State Size Distributions for Collisional Populations: Analytical Solution with Size-Dependent Strength
- Vertical structure models of T Tauri and Herbig Ae/Be disks
- On the Evolution of the Snow Line in Protoplanetary Discs
- Terrestrial planet formation from lost inner solar system material
- Earth shaped by primordial H atmospheres
- Infrared Signatures of Protoplanetary Disk Evolution
- Exploring the conditions required to form giant planets via gravitational instability in massive protoplanetary discs
- The effects of opacity on gravitational stability in protoplanetary discs
- Revised Estimates of Ocean Surface Drag in Strong Winds
- The mass-radius relation of exoplanets, revisited
- Solubility of water in peridotite liquids and the prevalence of steam atmospheres on rocky planets
- On the evolution of the snow line in protoplanetary discs II: Analytic approximations
- Pebbles versus planetesimals: the outcomes of population synthesis models
- Measuring the Dust Masses of Protoplanetary Disks in Lupus with ALMA: Evidence that Disks can be Optically Thick at 3 mm
- The influence of infall on the properties of protoplanetary discs
- The Maximum Mass Solar Nebula and the early formation of planets
- Determining Dust Properties in Protoplanetary Disks: SED-derived Masses and Settling With ALMA
- Role of magma oceans in controlling carbon and oxygen of sub-Neptune atmospheres
- Delivery of water and volatiles to the terrestrial planets and the Moon
- Structure of Passive Circumstellar Disks: Beyond the Two-Temperature Approximation
- The three regimes of atmospheric evaporation for super-Earths and sub-Neptunes
- Rapid solidification of Earth's magma ocean limits early lunar recession
- The fate of particles in a volumetrically heated convective fluid at high Prandtl number
- Orbital Divergence and Relaxation in the Gravitational N-Body Problem
- Exploring Super-Earth Surfaces: Albedo of Near-Airless Magma Ocean Planets and Topography
- Maximum Temperatures in Evolving Protoplanetary Discs and Composition of Planetary Building Blocks