The structure and stability of Fe4+xS3 and its potential to form a Martian inner core

Lianjie Man (), Xiang Li, Tiziana Boffa Ballaran, Wenju Zhou, Julien Chantel, Adrien Néri, Ilya Kupenko, Georgios Aprilis, Alexander Kurnosov, Olivier Namur, Michael Hanfland, Nicolas Guignot, Laura Henry, Leonid Dubrovinsky and Daniel. J. Frost
Additional contact information
Lianjie Man: Universität Bayreuth
Xiang Li: European Synchrotron Radiation Facility
Tiziana Boffa Ballaran: Universität Bayreuth
Wenju Zhou: University of Bayreuth
Julien Chantel: UMR 8207—UMET—Unité Matériaux et Transformations
Adrien Néri: Universität Bayreuth
Ilya Kupenko: European Synchrotron Radiation Facility
Georgios Aprilis: European Synchrotron Radiation Facility
Alexander Kurnosov: Universität Bayreuth
Olivier Namur: Earth and Environmental Sciences
Michael Hanfland: European Synchrotron Radiation Facility
Nicolas Guignot: L’Orme de Merisiers
Laura Henry: L’Orme de Merisiers
Leonid Dubrovinsky: Universität Bayreuth
Daniel. J. Frost: Universität Bayreuth

Nature Communications, 2025, vol. 16, issue 1, 1-9

Abstract: Abstract Seismic, geodetic and cosmochemical evidence point to Mars having a sulfur-rich liquid core. Due to the similarity between estimates of the core’s sulfur content and the iron–iron sulfide eutectic composition at core conditions, it has been concluded that temperatures are too high for Mars to have an inner core. Recent low density estimates for the core, however, appear consistent with sulfur contents that are higher than the eutectic composition, leading to the possibility that an inner core could form from a high-pressure iron sulfide phase. Here we report the crystal structure of a phase with the formula Fe4+xS3, the iron content of which increases with temperature, approaching the stoichiometry Fe5S3 under Martian inner core conditions. We show that Fe4+xS3 has a higher density than the liquid Martian core and that a Fe4+xS3 inner core would crystalize if temperatures fall below 1960 (±105) K at the center of Mars.

Date: 2025
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DOI: 10.1038/s41467-025-56220-2

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