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Physics and Chemistry of Minerals

, Volume 40, Issue 8, pp 647–657 | Cite as

Phase relations in the carbon-saturated C–Mg–Fe–Si–O system and C and Si solubility in liquid Fe at high pressure and temperature: implications for planetary interiors

  • Suguru TakahashiEmail author
  • Eiji Ohtani
  • Hidenori Terasaki
  • Yoshinori Ito
  • Yuki Shibazaki
  • Miho Ishii
  • Ken-ichi Funakoshi
  • Yuji Higo
Original Paper

Abstract

The phase and melting relations of the C-saturated C–Mg–Fe–Si–O system were investigated at high pressure and temperature to understand the role of carbon in the structure of the Earth, terrestrial planets, and carbon-enriched extraterrestrial planets. The phase relations were studied using two types of experiments at 4 GPa: analyses of recovered samples and in situ X-ray diffractions. Our experiments revealed that the composition of metallic iron melts changes from a C-rich composition with up to about 5 wt.% C under oxidizing conditions (ΔIW = −1.7 to −1.2, where ΔIW is the deviation of the oxygen fugacity (fO2) from an iron-wüstite (IW) buffer) to a C-depleted composition with 21 wt.% Si under reducing conditions (ΔIW < −3.3) at 4 GPa and 1,873 K. SiC grains also coexisted with the Fe–Si melt under the most reducing conditions. The solubility of C in liquid Fe increased with increasing fO2, whereas the solubility of Si decreased with increasing fO2. The carbon-bearing phases were graphite, Fe3C, SiC, and Fe alloy melt (Fe–C or Fe–Si–C melts) under the redox conditions applied at 4 GPa, but carbonate was not observed under our experimental conditions. The phase relations observed in this study can be applicable to the Earth and other planets. In hypothetical reducing carbon planets (ΔIW < −6.2), graphite/diamond and/or SiC exist in the mantle, whereas the core would be an Fe–Si alloy containing very small amount of C even in the carbon-enriched planets. The mutually exclusive nature of C and Si may be important also for considering the light elements of the Earth’s core.

Keywords

Carbon-enriched planet Oxygen fugacity Solubility Core composition Deep carbon cycle 

Notes

Acknowledgments

We thank S. Kamada, K. Nishida, T. Sakai, M. Miyahara, A. Suzuki, and M. Murakami for useful suggestions and discussions. We also thank Prof. Masanori Matsui for the editorial handling and anonymous reviewers for their constructive comments. The in situ X-ray diffraction experiments were performed with the approval of the Japan Synchrotron Radiation Research Institute (JASRI) (Proposal No. 2010A1530 and 2011A1546). This work was supported by a Grant-in-Aid for Scientific Research from the Ministry of Education, Culture, Science, Sport, and Technology of Japan (No. 18104009 and 22000002) to E. Ohtani. This work was conducted as part of the Global COE Program at Tohoku University, “Global Education and Research Center for Earth and Planetary Dynamics”.

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Copyright information

© Springer-Verlag Berlin Heidelberg 2013

Authors and Affiliations

  • Suguru Takahashi
    • 1
    Email author
  • Eiji Ohtani
    • 1
  • Hidenori Terasaki
    • 1
    • 2
  • Yoshinori Ito
    • 1
  • Yuki Shibazaki
    • 1
    • 3
  • Miho Ishii
    • 1
  • Ken-ichi Funakoshi
    • 4
  • Yuji Higo
    • 4
  1. 1.Department of Earth and Planetary Material SciencesTohoku UniversitySendaiJapan
  2. 2.Department of Earth and Space ScienceOsaka UniversityToyonakaJapan
  3. 3.Geophysical LaboratoryCarnegie Institution of WashingtonWashingtonUSA
  4. 4.Japan Synchrotron Radiation Research InstituteSayoJapan

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