Evidence map›Paper›PMID 41455714›Full record

ArticleNature communications2025

Shock compression of FeOOH and implications for iron-water interactions in super-earth magma oceans.

Yanyao Zhang, Komal Bali, Caroline Dorn, Alessandra Ravasio, Hong Yang, Silvia Pandolfi, Amanda J Chen, Xuehui Wei, Lélia Libon, Qijun Che and 12 more

Abstract read
PubMed Full text at PMC Publisher
In one paragraph

Article in Nature communications, 2025. The graph could read no effect estimate from its abstract, so it casts no vote on the map. Not yet cited in PubMed.

0numbers the graph read from it
0cells of the map it votes in
0citing papers in PubMed
–field-weighted citation impact
1 · What the graph read from it

What it found

Each row is one number read from the abstract, on the scale the paper reported it, with its interval. Left of the dashed line favours the treatment, right favours the comparator. Under each row is the sentence it came from. New to these charts? A ten-minute tutorial.

The abstract states no effect estimate the extractor could read, or names no intervention and outcome on the map, so this paper lights no cell and moves no belief. It is still indexed, cited and linked below.

2 · The registry

The trial behind it

Trials whose registry record cites this paper, or whose number appears in the abstract. A trial that started after this paper was published is citing it as background, not reporting it.

Neither the registry nor the abstract names a trial number. If this is a trial report, that itself is worth knowing.

3 · Its place in the literature

Who cites it

0 citing papers in PubMed.

No citing paper in PubMed yet.

4 · The record

Corrections and comments

PubMed lists nothing against this paper. Absence here is not a guarantee, only a check that was made.

5 · Who and what money

Authors and funding

22 authors.

Yanyao ZhangEarth and Planetary Sciences, Stanford University, Stanford, CA, USA. yanyaozh@stanford.edu.ORCID http://orcid.org/0000-0002-3846-1131
Komal Bali *Institute for Particle Physics and Astrophysics, ETH Zürich, Zürich, Switzerland.
Caroline Dorn *Institute for Particle Physics and Astrophysics, ETH Zürich, Zürich, Switzerland. dornc@phys.ethz.ch.ORCID http://orcid.org/0000-0001-6110-4610
Alessandra RavasioLaboratoire LULI, CNRS - École Polytechnique - CEA - Sorbonne Université, Palaiseau Cedex, France.ORCID http://orcid.org/0000-0002-2077-6493
Hong Yang *Earth and Planetary Sciences, Stanford University, Stanford, CA, USA.ORCID http://orcid.org/0000-0003-0906-7562
Silvia Pandolfi *Sorbonne Université, Muséum National d'Histoire Naturelle, UMR CNRS 7590, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Paris, France.ORCID http://orcid.org/0000-0003-0855-9434
Amanda J Chen *Earth and Planetary Sciences, Stanford University, Stanford, CA, USA.ORCID http://orcid.org/0000-0002-9284-6024
Xuehui Wei *School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA.ORCID http://orcid.org/0000-0002-1556-9924
Lélia Libon *Sorbonne Université, Muséum National d'Histoire Naturelle, UMR CNRS 7590, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Paris, France.ORCID http://orcid.org/0000-0001-5806-5796
Qijun CheSLAC National Accelerator Laboratory, Menlo Park, CA, USA.ORCID https://orcid.org/0009-0008-5805-7727
Donghao ZhengDepartment of Geosciences, Princeton University, Princeton, NJ, USA.
Eglantine BoulardSorbonne Université, Muséum National d'Histoire Naturelle, UMR CNRS 7590, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Paris, France.
Alessandra Benuzzi-MounaixLaboratoire LULI, CNRS - École Polytechnique - CEA - Sorbonne Université, Palaiseau Cedex, France.
Hae Ja LeeSLAC National Accelerator Laboratory, Menlo Park, CA, USA.ORCID http://orcid.org/0000-0002-4035-5637
Eric GaltierSLAC National Accelerator Laboratory, Menlo Park, CA, USA.
Nicholas A CzaplaSLAC National Accelerator Laboratory, Menlo Park, CA, USA.
Dimosthenis SokarasSLAC National Accelerator Laboratory, Menlo Park, CA, USA.ORCID http://orcid.org/0000-0001-8117-1933
Roberto Alonso-MoriSLAC National Accelerator Laboratory, Menlo Park, CA, USA. robertoa@slac.stanford.edu.ORCID http://orcid.org/0000-0002-5357-0934
Arianna E GleasonEarth and Planetary Sciences, Stanford University, Stanford, CA, USA. ariannag@stanford.edu.ORCID http://orcid.org/0000-0002-7736-5118
Sang Heon ShimSchool of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA. shdshim@asu.edu.ORCID http://orcid.org/0000-0001-5203-6038
Guillaume MorardSorbonne Université, Muséum National d'Histoire Naturelle, UMR CNRS 7590, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Paris, France. guillaume.morard@cnrs.fr.ORCID http://orcid.org/0000-0002-4225-0767
Wendy L MaoEarth and Planetary Sciences, Stanford University, Stanford, CA, USA. wmao@stanford.edu.ORCID http://orcid.org/0000-0003-0595-7760

Funding

No grant is acknowledged in the PubMed record.

6 · The paper itself

Abstract

Iron(Fe)-water reactions in a magma ocean can influence water storage and density of planets. These reactions can form Fe-O-H phases, whose density, melting, and electronic properties at planetary interior conditions are important for informing planetary models. Here, we study natural goethite (α-FeOOH) that is shock-compressed along its principal Hugoniot. Analysis of our velocity interferometer system for any reflector (VISAR) results extends the equation of state to over 800 GPa. X-ray diffraction and VISAR reflectivity results indicate the onset of melting occurs at ~95 GPa with complete melting by 166 GPa, which may be relevant to low seismic velocity anomalies observed above the core-mantle boundary. Analysis of X-ray emission spectroscopy results up to 285 GPa shows the spin crossover of Fe, with dominantly low spin Fe above ~265 GPa in the melt, supporting formation of dense basal magma oceans in terrestrial planets. Using our measured FeOOH densities, we model planetary interiors up to 10 Earth masses. Assuming FeOOH forms via iron-water reactions, the radius decreases by up to 28%, while the density increases by up to 165% compared to the unreacted case, providing an avenue to investigate water storage and evolution in super-Earths and sub-Neptunes.

Identifiers

PMID41455714
PMCPMC12852173

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Read under generation 80e0d062 · epoch 390. Bibliography from PubMed, PubMed Central and OpenAlex; grants from NIH RePORTER; trial links from ClinicalTrials.gov; estimates, votes and beliefs from the OpenQuestion graph.