Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths

Horn, H. W.; Prakapenka, V.; Chariton, S.; Speziale, S.; Shim, S. -H.

doi:10.3847/PSJ/acab03

Title: Reaction between Hydrogen and Ferrous/Ferric Oxides at High Pressures and High Temperatures—Implications for Sub-Neptunes and Super-Earths

Journal Article · Mon Feb 13 00:00:00 EST 2023 · The Planetary Science Journal

DOI:https://doi.org/10.3847/PSJ/acab03· OSTI ID:1924376

; Prakapenka, V.; Chariton, S.; Speziale, S.;

Abstract Sub-Neptune exoplanets may have thick hydrogen envelopes and therefore develop a high-pressure interface between hydrogen and the underlying silicates/metals. Some sub-Neptunes may convert to super-Earths via massive gas loss. If hydrogen chemically reacts with oxides and metals at high pressures and temperatures ( P − T ), it could impact the structure and composition of the cores and atmospheres of sub-Neptunes and super-Earths. While H ₂ gas is a strong reducing agent at low pressures, the behavior of hydrogen is unknown at the P − T expected for sub-Neptunes’ interiors, where hydrogen is a dense supercritical fluid. Here we report experimental results of reactions between ferrous/ferric oxides and hydrogen at 20–40 GPa and 1000–4000 K utilizing the pulsed laser-heated diamond-anvil cell combined with synchrotron X-ray diffraction. Under these conditions, hydrogen spontaneously strips iron off the oxides, forming Fe-H alloys and releasing oxygen to the hydrogen medium. In a planetary context where this reaction may occur, the Fe-H alloy may sink to the metallic part of the core, while released oxygen may stabilize as water in the silicate layer, providing a mechanism to ingas hydrogen to the deep interiors of sub-Neptunes. Water produced from the redox reaction can also partition to the atmosphere of sub-Neptunes, which has important implications for understanding the composition of their atmospheres. In addition, super-Earths converted from sub-Neptunes may contain a large amount of hydrogen and water in their interiors (at least a few wt% H ₂ O). This is distinct from smaller rocky planets, which were formed relatively dry (likely a few hundredths wt% H ₂ O).

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Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Argonne National Laboratory (ANL), Argonne, IL (United States). Advanced Photon Source (APS)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA); National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); USDOE Office of Science (SC), Basic Energy Sciences (BES). Chemical Sciences, Geosciences & Biosciences Division (CSGB)

Grant/Contract Number:: FG02-94ER14466; AC52-07NA27344; AC02-06CH11357; 80NSSC18K0353; AST-2108129; EAR-1921298; EAR-1634415

OSTI ID:: 1924376

Alternate ID(s):: OSTI ID: 1972040

Report Number(s):: LLNL-JRNL-842010

Journal Information:: The Planetary Science Journal, Journal Name: The Planetary Science Journal Vol. 4 Journal Issue: 2; ISSN 2632-3338

Publisher:: American Astronomical SocietyCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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