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2 results on '"Kizovski, TV"'

1. An olivine cumulate outcrop on the floor of Jezero crater, Mars.

Author

Liu Y, Tice MM, Schmidt ME, Treiman AH, Kizovski TV, Hurowitz JA, Allwood AC, Henneke J, Pedersen DAK, VanBommel SJ, Jones MWM, Knight AL, Orenstein BJ, Clark BC, Elam WT, Heirwegh CM, Barber T, Beegle LW, Benzerara K, Bernard S, Beyssac O, Bosak T, Brown AJ, Cardarelli EL, Catling DC, Christian JR, Cloutis EA, Cohen BA, Davidoff S, Fairén AG, Farley KA, Flannery DT, Galvin A, Grotzinger JP, Gupta S, Hall J, Herd CDK, Hickman-Lewis K, Hodyss RP, Horgan BHN, Johnson JR, Jørgensen JL, Kah LC, Maki JN, Mandon L, Mangold N, McCubbin FM, McLennan SM, Moore K, Nachon M, Nemere P, Nothdurft LD, Núñez JI, O'Neil L, Quantin-Nataf CM, Sautter V, Shuster DL, Siebach KL, Simon JI, Sinclair KP, Stack KM, Steele A, Tarnas JD, Tosca NJ, Uckert K, Udry A, Wade LA, Weiss BP, Wiens RC, Williford KH, and Zorzano MP

Abstract

The geological units on the floor of Jezero crater, Mars, are part of a wider regional stratigraphy of olivine-rich rocks, which extends well beyond the crater. We investigated the petrology of olivine and carbonate-bearing rocks of the Séítah formation in the floor of Jezero. Using multispectral images and x-ray fluorescence data, acquired by the Perseverance rover, we performed a petrographic analysis of the Bastide and Brac outcrops within this unit. We found that these outcrops are composed of igneous rock, moderately altered by aqueous fluid. The igneous rocks are mainly made of coarse-grained olivine, similar to some martian meteorites. We interpret them as an olivine cumulate, formed by settling and enrichment of olivine through multistage cooling of a thick magma body.

Published
2022
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2. Aqueously altered igneous rocks sampled on the floor of Jezero crater, Mars.

Author

Farley KA, Stack KM, Shuster DL, Horgan BHN, Hurowitz JA, Tarnas JD, Simon JI, Sun VZ, Scheller EL, Moore KR, McLennan SM, Vasconcelos PM, Wiens RC, Treiman AH, Mayhew LE, Beyssac O, Kizovski TV, Tosca NJ, Williford KH, Crumpler LS, Beegle LW, Bell JF 3rd, Ehlmann BL, Liu Y, Maki JN, Schmidt ME, Allwood AC, Amundsen HEF, Bhartia R, Bosak T, Brown AJ, Clark BC, Cousin A, Forni O, Gabriel TSJ, Goreva Y, Gupta S, Hamran SE, Herd CDK, Hickman-Lewis K, Johnson JR, Kah LC, Kelemen PB, Kinch KB, Mandon L, Mangold N, Quantin-Nataf C, Rice MS, Russell PS, Sharma S, Siljeström S, Steele A, Sullivan R, Wadhwa M, Weiss BP, Williams AJ, Wogsland BV, Willis PA, Acosta-Maeda TA, Beck P, Benzerara K, Bernard S, Burton AS, Cardarelli EL, Chide B, Clavé E, Cloutis EA, Cohen BA, Czaja AD, Debaille V, Dehouck E, Fairén AG, Flannery DT, Fleron SZ, Fouchet T, Frydenvang J, Garczynski BJ, Gibbons EF, Hausrath EM, Hayes AG, Henneke J, Jørgensen JL, Kelly EM, Lasue J, Le Mouélic S, Madariaga JM, Maurice S, Merusi M, Meslin PY, Milkovich SM, Million CC, Moeller RC, Núñez JI, Ollila AM, Paar G, Paige DA, Pedersen DAK, Pilleri P, Pilorget C, Pinet PC, Rice JW Jr, Royer C, Sautter V, Schulte M, Sephton MA, Sharma SK, Sholes SF, Spanovich N, St Clair M, Tate CD, Uckert K, VanBommel SJ, Yanchilina AG, and Zorzano MP

Abstract

The Perseverance rover landed in Jezero crater, Mars, to investigate ancient lake and river deposits. We report observations of the crater floor, below the crater's sedimentary delta, finding that the floor consists of igneous rocks altered by water. The lowest exposed unit, informally named Séítah, is a coarsely crystalline olivine-rich rock, which accumulated at the base of a magma body. Magnesium-iron carbonates along grain boundaries indicate reactions with carbon dioxide-rich water under water-poor conditions. Overlying Séítah is a unit informally named Máaz, which we interpret as lava flows or the chemical complement to Séítah in a layered igneous body. Voids in these rocks contain sulfates and perchlorates, likely introduced by later near-surface brine evaporation. Core samples of these rocks have been stored aboard Perseverance for potential return to Earth.

Published
2022
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