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6 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, 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, 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, Zorzano, M-P, Mangold, Nicolas, Cosmochimie [IMPMC] (IMPMC_COSMO), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Liu, Y [0000-0003-0308-0942], Tice, MM [0000-0003-2560-1702], Schmidt, ME [0000-0003-4793-7899], Treiman, AH [0000-0002-8073-2839], Kizovski, TV [0000-0001-8188-9769], Hurowitz, JA [0000-0002-5857-8652], Henneke, J [0000-0002-3195-7417], Pedersen, DAK [0000-0001-7182-8567], VanBommel, SJ [0000-0002-6565-0827], Jones, MWM [0000-0002-0720-8715], Knight, AL [0000-0001-6832-8190], Orenstein, BJ [0000-0002-6586-4227], Clark, BC [0000-0002-5546-8757], Beegle, LW [0000-0002-4944-4353], Benzerara, K [0000-0002-0553-0137], Bernard, S [0000-0001-5576-7020], Beyssac, O [0000-0001-8879-4762], Bosak, T [0000-0001-5179-5323], Brown, AJ [0000-0002-9352-6989], Cardarelli, EL [0000-0001-5451-2309], Catling, DC [0000-0001-5646-120X], Christian, JR [0000-0003-4646-2852], Cloutis, EA [0000-0001-7301-0929], Cohen, BA [0000-0001-5896-5903], Davidoff, S [0000-0002-4417-7268], Fairén, AG [0000-0002-2938-6010], Flannery, DT [0000-0001-8982-496X], Grotzinger, JP [0000-0001-9324-1257], Gupta, S [0000-0001-6415-1332], Hall, J [0000-0003-0884-3777], Herd, CDK [0000-0001-5210-4002], Hickman-Lewis, K [0000-0001-8014-233X], Hodyss, RP [0000-0002-6523-3660], Horgan, BHN [0000-0001-6314-9724], Johnson, JR [0000-0002-5586-4901], Jørgensen, JL [0000-0002-0343-239X], Kah, LC [0000-0001-7172-2033], Maki, JN [0000-0002-7887-0343], Mandon, L [0000-0002-9310-0742], Mangold, N [0000-0002-0022-0631], McCubbin, FM [0000-0002-2101-4431], McLennan, SM [0000-0003-4259-7178], Nachon, M [0000-0003-0417-7076], Nothdurft, LD [0000-0001-9646-9070], Núñez, JI [0000-0003-0930-6674], O'Neil, L [0000-0003-1555-8229], Quantin-Nataf, CM [0000-0002-8313-8595], Shuster, DL [0000-0003-2507-9977], Siebach, KL [0000-0002-6628-6297], Simon, JI [0000-0002-3969-8958], Sinclair, KP [0000-0001-6261-4591], Stack, KM [0000-0003-3444-6695], Steele, A [0000-0001-9643-2841], Tarnas, JD [0000-0002-6256-0826], Tosca, NJ [0000-0003-4415-4231], Uckert, K [0000-0002-0859-5526], Udry, A [0000-0002-0074-8110], Wade, LA [0000-0001-8254-8181], Weiss, BP [0000-0003-3113-3415], Wiens, RC [0000-0002-3409-7344], Zorzano, M-P [0000-0002-4492-9650], and Apollo - University of Cambridge Repository

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Multidisciplinary, 5101 Astronomical Sciences, 37 Earth Sciences, 3705 Geology, 5109 Space Sciences, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology, 51 Physical Sciences, 3703 Geochemistry
Abstract

International audience; 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 investigate 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 find 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 multi-stage cooling of a thick magma body.

Published
2022
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2. Diverse and highly differentiated lava suite in Jezero crater, Mars: Constraints on intracrustal magmatism revealed by Mars 2020 PIXL.

Author

Schmidt ME, Kizovski TV, Liu Y, Hernandez-Montenegro JD, Tice MM, Treiman AH, Hurowitz JA, Klevang DA, Knight AL, Labrie J, Tosca NJ, VanBommel SJ, Benaroya S, Crumpler LS, Horgan BHN, Morris RV, Simon JI, Udry A, Yanchilina A, Allwood AC, Cable ML, Christian JR, Clark BC, Flannery DT, Heirwegh CM, Henley TLJ, Henneke J, Jones MWM, Orenstein BJ, Herd CDK, Randazzo N, Shuster D, and Wadhwa M

Abstract

The Jezero crater floor features a suite of related, iron-rich lavas that were examined and sampled by the Mars 2020 rover Perseverance, and whose textures, minerals, and compositions were characterized by the Planetary Instrument for X-ray Lithochemistry (PIXL). This suite, known as the Máaz formation (fm), includes dark-toned basaltic/trachy-basaltic rocks with intergrown pyroxene, plagioclase feldspar, and altered olivine and overlying trachy-andesitic lava with reversely zoned plagioclase phenocrysts in a K-rich groundmass. Feldspar thermal disequilibrium textures indicate that they were carried from their crustal staging area. Bulk and mafic minerals have very high FeO and low MgO to FeO total ratios, which are partially reproduced by thermodynamic models involving high-degree fractional crystallization of a gabbroic assemblage and possibly also assimilation of iron-rich basement. Together, these in situ constraints on petrogenesis provide a uniquely detailed record of intracrustal processes beneath Jezero crater during a time period not represented by Mars samples to date.

Published
2025
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3. Alteration history of Séítah formation rocks inferred by PIXL x-ray fluorescence, x-ray diffraction, and multispectral imaging on Mars.

Author

Tice MM, Hurowitz JA, Allwood AC, Jones MWM, Orenstein BJ, Davidoff S, Wright AP, Pedersen DAK, Henneke J, Tosca NJ, Moore KR, Clark BC, McLennan SM, Flannery DT, Steele A, Brown AJ, Zorzano MP, Hickman-Lewis K, Liu Y, VanBommel SJ, Schmidt ME, Kizovski TV, Treiman AH, O'Neil L, Fairén AG, Shuster DL, and Gupta S

Abstract

Collocated crystal sizes and mineral identities are critical for interpreting textural relationships in rocks and testing geological hypotheses, but it has been previously impossible to unambiguously constrain these properties using in situ instruments on Mars rovers. Here, we demonstrate that diffracted and fluoresced x-rays detected by the PIXL instrument (an x-ray fluorescence microscope on the Perseverance rover) provide information about the presence or absence of coherent crystalline domains in various minerals. X-ray analysis and multispectral imaging of rocks from the Séítah formation on the floor of Jezero crater shows that they were emplaced as coarsely crystalline igneous phases. Olivine grains were then partially dissolved and filled by finely crystalline or amorphous secondary silicate, carbonate, sulfate, and chloride/oxychlorine minerals. These results support the hypothesis that Séítah formation rocks represent olivine cumulates altered by fluids far from chemical equilibrium at low water-rock ratios.

Published
2022
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4. 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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6. Evidence for sodium-rich alkaline water in the Tagish Lake parent body and implications for amino acid synthesis and racemization.

Author

White LF, Tait KT, Langelier B, Lymer EA, Černok A, Kizovski TV, Ma C, Tschauner O, and Nicklin RI

Subjects
British Columbia, Calcium chemistry, Ferrosoferric Oxide chemistry, Hydrogen-Ion Concentration, Lakes, Magnesium chemistry, Stereoisomerism, Tomography methods, Amino Acids biosynthesis, Amino Acids chemical synthesis, Meteoroids, Sodium chemistry, Water chemistry
Abstract

Understanding the timing and mechanisms of amino acid synthesis and racemization on asteroidal parent bodies is key to demonstrating how amino acids evolved to be mostly left-handed in living organisms on Earth. It has been postulated that racemization can occur rapidly dependent on several factors, including the pH of the aqueous solution. Here, we conduct nanoscale geochemical analysis of a framboidal magnetite grain within the Tagish Lake carbonaceous chondrite to demonstrate that the interlocking crystal arrangement formed within a sodium-rich, alkaline fluid environment. Notably, we report on the discovery of Na-enriched subgrain boundaries and nanometer-scale Ca and Mg layers surrounding individual framboids. These interstitial coatings would yield a surface charge state of zero in more-alkaline fluids and prevent assimilation of the individual framboids into a single grain. This basic solution would support rapid synthesis and racemization rates on the order of years, suggesting that the low abundances of amino acids in Tagish Lake cannot be ascribed to fluid chemistry., Competing Interests: The authors declare no competing interest., (Copyright © 2020 the Author(s). Published by PNAS.)

Published
2020
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