The composition of Mars

TL;DR

This paper proposes an alternative compositional model for Mars based on meteorite and spacecraft data, challenging the traditional CI chondrite assumption and providing new insights into Martian core composition and volatile element depletion.

Contribution

It introduces a new model for Mars's bulk composition that does not rely on CI chondrite analogs, using meteorite and spacecraft data to refine element abundances and core composition estimates.

Findings

Mars has 2.26 times higher refractory lithophile elements than CI chondrites.

Mars shows systematic depletion in moderately volatile lithophile elements.

The Martian core likely contains ≤7 wt% sulfur, lower than previous models.

Abstract

Comparing compositional models of the terrestrial planets provides insights into physicochemical processes that produced planet-scale similarities and differences. The widely accepted compositional model for Mars assumes Mn and more refractory elements are in CI chondrite proportions in the planet, including Fe, Mg, and Si, which along with O make up $>$90\% of the mass of Mars. However, recent improvements in our understandings on the composition of the solar photosphere and meteorites challenge the use of CI chondrite as an analog of Mars. Here we present an alternative model composition for Mars that avoids such an assumption and is based on data from Martian meteorites and spacecraft observations. Our modeling method was previously applied to predict the Earth's composition. The model establishes the absolute abundances of refractory lithophile elements in the bulk silicate Mars (BSM) at 2.26 times higher than that in CI carbonaceous chondrites. Relative to this chondritic composition, Mars has a systematic depletion in moderately volatile lithophile elements as a function of their condensation temperatures. Given this finding, we constrain the abundances of siderophile and chalcophile elements in the bulk Mars and its core. The Martian volatility trend is consistent with $ \leq $7 wt\% S in its core, which is significantly lower than that assumed in most core models (i.e., $ > $10 wt\% S). Furthermore, the occurrence of ringwoodite at the Martian core-mantle boundary might have contributed to the partitioning of O and H into the Martian core.