Chromium on Mercury: New Results From the MESSENGER X‐Ray Spectrometer and Implications for the Innermost Planet's Geochemical Evolution

Abstract

Abstract Mercury, the innermost planet, formed under highly reduced conditions, based mainly on surface Fe, S, and Si abundances determined from MESSENGER mission data. The minor element Cr may serve as an independent oxybarometer but only very limited Cr data have been previously reported for Mercury. We report Cr/Si abundances across Mercury's surface based on MESSENGER X‐Ray Spectrometer data throughout the spacecraft's orbital mission. The heterogeneous Cr/Si ratio ranges from 3.6 × 10 −5 in the Caloris Basin to 0.0012 within the high‐magnesium region, with an average southern hemisphere value of 0.0008 (corresponding to about 200 ppm Cr). Absolute Cr/Si values have systematic uncertainty of at least 30%, but relative variations are more robust. By combining experimental Cr partitioning data along with planetary differentiation modeling, we find that if Mercury formed with bulk chondritic Cr/Al, Cr must be present in the planet's core and differentiation must have occurred at log f O 2 in the range of IW‐6.5 to IW‐2.5 in the absence of sulfides in its interior and a range of IW‐5.5 to IW‐2 with an FeS layer at the core‐mantle boundary. Models with large fractions of Mg‐Ca‐rich sulfides in Mercury's interior are more compatible with moderately reducing conditions (IW‐5.5 to IW‐4) owing to the instability of Mg‐Ca‐rich sulfides at elevated f O 2 . These results indicate that if Mercury differentiated at a log f O 2 lower than IW‐5.5, the presence of sulfides whether in the form of a FeS layer at the top of the core or Mg‐Ca‐rich sulfides within the mantle would be unlikely.