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U, Th, and K partitioning between metal, silicate, and sulfide and implications for Mercury’s structure, volatile content, and radioactive heat production

  • Asmaa Boujibar EMAIL logo , Mya Habermann , Kevin Righter , D. Kent Ross , Kellye Pando , Minako Righter , Bethany A. Chidester and Lisa R. Danielson
Published/Copyright: August 28, 2019
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American Mineralogist
From the journal American Mineralogist Volume 104 Issue 9

Abstract

The distribution of heat-producing elements (HPE) potassium (K), uranium (U), and thorium (Th) within planetary interiors has major implications for the thermal evolution of the terrestrial planets and for the inventory of volatile elements in the inner solar system. To investigate the abundances of HPE in Mercury’s interior, we conducted experiments at high pressure and temperature (up to 5 GPa and 1900 °C) and reduced conditions (IW-1.8 to IW-6.5) to determine U, Th, and K partitioning between metal, silicate, and sulfide (Dmet/sil and Dsulf/sil). Our experimental data combined with those from the literature show that partitioning into sulfide is more efficient than into metal and that partitioning is enhanced with decreasing FeO and increasing O contents of the silicate and sulfide melts, respectively. Also, at low oxygen fugacity (log fO2 < IW-5), U and Th are more efficiently partitioned into liquid iron metal and sulfide than K. Dmet/sil for U, Th, and K increases with decreasing oxygen fugacity, while DUmet/sil and DKmet/sil increase when the metal is enriched and depleted in O or Si, respectively. We also used available data from the literature to constrain the concentrations of light elements (Si, S, O, and C) in Fe metal and sulfide. We calculated chemical compositions of Mercury’s core after core segregation, for a range of fO2 conditions during its differentiation. For example, if Mercury differentiated at IW-5.5, its core would contain 49 wt% Si, 0.02 wt% S, and negligible C. Also if core-mantle separation happened at a fO2 lower than IW-4, the bulk Mercury Fe/Si ratio is likely to be chondritic. We calculated concentrations of U, Th, and K in the Fe-rich core and possible sulfide layer of Mercury. Bulk Mercury K/U and K/Th were calculated taking all U, Th, and K reservoirs into account. Without any sulfide layer, or if Mercury’s core segregated at a higher fO2 than IW-4, bulk K/U and K/Th would be similar to those measured on the surface, confirming more elevated volatile K concentration than previously expected for Mercury. However, Mercury could fall on an overall volatile depletion trend where K/U increases with the heliocentric distance if core segregation occurred near IW-5.5 or more reduced conditions, and with a sulfide layer of at least 130 km thickness. At these conditions, the bulk Mercury K/Th ratio is close to Venus’s and Earth’s values. Since U and Th become more chalcophile with decreasing oxygen fugacity, to a higher extent than K, it is likely that at an fO2 close to, or lower than, IW-6 both K/U and K/Th become lower than values of the other terrestrial planets. Therefore, our results suggest that the elevated K/U and K/Th ratios of Mercury’s surface should not be exclusively interpreted as the result of a volatile enrichment in Mercury, but could also indicate a sequestration of more U and Th than K in a hidden iron sulfide reservoir, possibly a layer present between the mantle and core. Hence, Mercury could be more depleted in volatiles than Mars with a K concentration similar to or lower than the Earth’s and Venus’s, suggesting volatile depletion in the inner solar system. In addition, we show that the presence of a sulfide layer formed between IW-4 and IW-5.5 decreases the total radioactive heat production of Mercury by up to 30%.

Keywords: Core formation; Mercury; oxygen fugacity; partitioning, metal-silicate; sulfides; Volatile Elements in Differentiated Planetary Interiors

† Special collection papers can be found online at http://www.minsocam.org/MSA/AmMin/special-collections.html

Acknowledgments and Funding

This work was conducted at NASA JSC and funded by a NASA Postdoctoral Program fellowship awarded to A.B. and RTOPs from the NASA Cosmochemistry and LASER programs to K.R. M.H. was supported by a LPI summer internship. We acknowledge Anne Peslier, Loan Lee, and Thomas Lapen for support with electron microprobe, sample preparation, and ICPMS analysis, respectively. We thank Tim McCoy, Cari Corrigan, and other anonymous reviewers from earlier versions of the manuscript for their constructive comments. This article benefitted from discussions with Peter Driscoll, Larry Nittler, Conel Alexander, and Francis McCubbin.

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Received: 2019-02-14
Accepted: 2019-06-06
Published Online: 2019-08-28
Published in Print: 2019-09-25

© 2019 Walter de Gruyter GmbH, Berlin/Boston

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https://doi.org/10.2138/am-2019-7000
Keywords for this article
Core formation; Mercury; oxygen fugacity; partitioning, metal-silicate; sulfides; Volatile Elements in Differentiated Planetary Interiors

Articles in the same Issue

  1. Highlights and Breakthroughs
  2. Seeking the most hydrous, primitive arc melts: The glass is half full
  3. Hydrous LABZ beneath a subduction zone was reconstructed for the first time
  4. U, Th, and K partitioning between metal, silicate, and sulfide and implications for Mercury’s structure, volatile content, and radioactive heat production
  5. Valleyite: A new magnetic mineral with the sodalite-type structure
  6. An analysis of the magnetic behavior of olivine and garnet substitutional solid solutions
  7. Pyrite trace-element and sulfur isotope geochemistry of paleo-mesoproterozoic McArthur Basin: Proxy for oxidative weathering
  8. Compressional behavior and spin state of δ-(Al,Fe)OOH at high pressures
  9. Reconstruction of the lithosphere-asthenosphere boundary zone beneath Ichinomegata maar, Northeast Japan, by geobarometry of spinel peridotite xenoliths
  10. High-pressure phase stability and elasticity of ammonia hydrate
  11. A multi-methodological study of kurnakovite: A potential B-rich aggregate
  12. Identification of the occurrence of minor elements in the structure of diatomaceous opal using FIB and TEM-EDS
  13. Nixonite, Na2Ti6O13, a new mineral from a metasomatized mantle garnet pyroxenite from the western Rae Craton, Darby kimberlite field, Canada
  14. Goldschmidtite, (K,REE,Sr)(Nb,Cr)O3: A new perovskite supergroup mineral found in diamond from Koffiefontein, South Africa
  15. Edscottite, Fe5C2, a new iron carbide mineral from the Ni-rich Wedderburn IAB iron meteorite
  16. Letter
  17. The stability of Fe5O6 and Fe4O5 at high pressure and temperature
  18. New Mineral Names
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