Water storage capacity of the martian mantle through time

Dong, Junjie; Fischer, R. A.; Stixrude, Lars; Lithgow‐Bertelloni, Carolina; Eriksen, Zachary; Brennan, Matthew C.

doi:10.1016/j.icarus.2022.115113

Cited by 3 publications

(1 citation statement)

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“…Volatiles, H 2 O but also C‐bearing species such as CO 2 or CH 4 , should be studied by a combination of spectroscopic and SIMS techniques to identify these volatiles and quantify their abundances and isotopic compositions in the Séítah magma. The origin, abundance, and isotopic composition of water in the Martian mantle, and its consequences for the physicochemical evolution of Mars are still a matter of debate (Barnes et al., 2020; Breuer et al., 2016; Dong et al., 2022; Filiberto et al., 2016). Water could be present not only in phosphates or in the mesostasis in Séítah rocks but also in trace abundances in nominally anhydrous minerals (D. R. Bell & Rossman, 1992) such as olivine (Bolfan‐Casanova et al., 2014) and pyroxene (Peslier et al., 2002).…”

Section: Discussionmentioning

confidence: 99%

Petrological Traverse of the Olivine Cumulate Séítah Formation at Jezero Crater, Mars: A Perspective From SuperCam Onboard Perseverance

Beyssac¹,

Forni

Cousin

et al. 2023

JGR Planets

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Séítah is the stratigraphically lowest formation visited by Perseverance in the Jezero crater floor.We present the data obtained by SuperCam: texture by imagery, chemistry by Laser-Induced Breakdown Spectroscopy, and mineralogy by Supercam Visible and Infrared reflectance and Raman spectroscopy. The Séítah formation consists of igneous, weakly altered rocks dominated by millimeter-sized grains of olivine with the presence of low-Ca and high-Ca pyroxenes, and other primary minerals (e.g., plagioclase, Cr-Fe-Ti oxides, phosphates). Along a ∼140 m long section in Séítah, SuperCam analyses showed evidence of geochemical and mineralogical variations, from the contact with the overlying Máaz formation, going deeper in the formation. Bulk rock and olivine Mg#, grain size, olivine content increase gradually further from the contact. Along the section, olivine Mg# is not in equilibrium with the bulk rock Mg#, indicating local olivine accumulation. These observations are consistent with Séítah being the deep ultramafic member of a cumulate series derived from the fractional crystallization and slow cooling of the parent magma at depth. Possible magmatic processes and exhumation mechanisms of Séítah are discussed. Séítah rocks show some affinity with some rocks at Gusev crater, and with some Martian meteorites suggesting that such rocks are not rare on the surface of Mars.

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