Atomic-scale mixing between MgO and H2O in the deep interiors of water-rich planets
Abstract
Water-rich planets exist in our Solar System (Uranus and Neptune) and are found to be common in the extrasolar systems (some of the sub-Neptunes). In conventional models of these planets a thick water-rich layer is underlain by a separate rocky interior. In this work, we report experimental results on two rock-forming minerals, olivine ((Mg,Fe)2SiO4) and ferropericlase ((Mg,Fe) O), in water at the pressure and temperature conditions expected for the water-rich planets. Our data indicate a selective leaching of MgO, which peaks between 20 and 40 GPa and above 1,500 K. For water-rich planets with 1–6 Earth masses (>50 wt% H2O), the chemical reaction at the deep water–rock interface would lead to high concentrations of MgO in the H2O layer. For Uranus and Neptune, the top ~3% of the H2O layer would have a large storage capacity for MgO. If an early dynamic process enables the rock–H2O reaction, the topmost H2O layer may be rich in MgO, possibly affecting the thermal history of the planet.
- Authors:
-
[1];
[2];
[3];
[6];
[1]
- Yonsei Univ., Seoul (Korea, Republic of)
- Univ. of Chicago, IL (United States)
- Deutsches Elektronen-Synchrotron (DESY), Hamburg (Germany)
- Univ. of Illinois, Chicago, IL (United States)
- Helmholtz-Zentrum Potsdam (HZP), (Germany). German Research Centre for GeoSciences
- Arizona State Univ., Tempe, AZ (United States)
- Publication Date:
- Research Org.:
- Univ. of Illinois, Chicago, IL (United States)
- Sponsoring Org.:
- USDOE National Nuclear Security Administration (NNSA), Office of Defense Programs (DP); USDOE Office of Science (SC), Basic Energy Sciences (BES); Korean Ministry of Science; National Science Foundation (NSF); National Aeronautics and Space Administration (NASA)
- OSTI Identifier:
- 1785537
- Grant/Contract Number:
- NA0003975; SC0012704; FG02-94ER14466; FC03-03N00144; AC02-06CH11357; NRF-2018R1A3B1052042; NRF-2019K1A3A7A09033395; EAR1338810; EAR-1634415; EAR 11-57758; 80NSSC18K0353
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Nature Astronomy
- Additional Journal Information:
- Journal Volume: 5; Journal ID: ISSN 2397-3366
- Publisher:
- Springer Nature
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS
Citation Formats
Kim, Taehyun, Chariton, Stella, Prakapenka, Vitali, Pakhomova, Anna, Liermann, Hanns-Peter, Liu, Zhenxian, Speziale, Sergio, Shim, Sang-Heon, and Lee, Yongjae. Atomic-scale mixing between MgO and H2O in the deep interiors of water-rich planets. United States: N. p., 2021.
Web. doi:10.1038/s41550-021-01368-2.
Kim, Taehyun, Chariton, Stella, Prakapenka, Vitali, Pakhomova, Anna, Liermann, Hanns-Peter, Liu, Zhenxian, Speziale, Sergio, Shim, Sang-Heon, & Lee, Yongjae. Atomic-scale mixing between MgO and H2O in the deep interiors of water-rich planets. United States. https://doi.org/10.1038/s41550-021-01368-2
Kim, Taehyun, Chariton, Stella, Prakapenka, Vitali, Pakhomova, Anna, Liermann, Hanns-Peter, Liu, Zhenxian, Speziale, Sergio, Shim, Sang-Heon, and Lee, Yongjae. Mon .
"Atomic-scale mixing between MgO and H2O in the deep interiors of water-rich planets". United States. https://doi.org/10.1038/s41550-021-01368-2. https://www.osti.gov/servlets/purl/1785537.
@article{osti_1785537,
title = {Atomic-scale mixing between MgO and H2O in the deep interiors of water-rich planets},
author = {Kim, Taehyun and Chariton, Stella and Prakapenka, Vitali and Pakhomova, Anna and Liermann, Hanns-Peter and Liu, Zhenxian and Speziale, Sergio and Shim, Sang-Heon and Lee, Yongjae},
abstractNote = {Water-rich planets exist in our Solar System (Uranus and Neptune) and are found to be common in the extrasolar systems (some of the sub-Neptunes). In conventional models of these planets a thick water-rich layer is underlain by a separate rocky interior. In this work, we report experimental results on two rock-forming minerals, olivine ((Mg,Fe)2SiO4) and ferropericlase ((Mg,Fe) O), in water at the pressure and temperature conditions expected for the water-rich planets. Our data indicate a selective leaching of MgO, which peaks between 20 and 40 GPa and above 1,500 K. For water-rich planets with 1–6 Earth masses (>50 wt% H2O), the chemical reaction at the deep water–rock interface would lead to high concentrations of MgO in the H2O layer. For Uranus and Neptune, the top ~3% of the H2O layer would have a large storage capacity for MgO. If an early dynamic process enables the rock–H2O reaction, the topmost H2O layer may be rich in MgO, possibly affecting the thermal history of the planet.},
doi = {10.1038/s41550-021-01368-2},
journal = {Nature Astronomy},
number = ,
volume = 5,
place = {United States},
year = {Mon May 17 00:00:00 EDT 2021},
month = {Mon May 17 00:00:00 EDT 2021}
}
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