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Bowden DL, Bridges JC, Cousin A, Rapin W, Semprich J, Gasnault O, Forni O, Gasda P, Das D, Payré V, Sautter V, Bedford CC, Wiens RC, Pinet P, Frydenvang J. Askival: An altered feldspathic cumulate sample in Gale crater. Meteorit Planet Sci 2023; 58:41-62. [PMID: 37082523 PMCID: PMC10108227 DOI: 10.1111/maps.13933] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/15/2022] [Accepted: 10/28/2022] [Indexed: 05/03/2023]
Abstract
Askival is a light-toned, coarsely crystalline float rock, which was identified near the base of Vera Rubin Ridge in Gale crater. We have studied Askival, principally with the ChemCam instrument but also using APXS compositional data and MAHLI images. Askival and an earlier identified sample, Bindi, represent two rare examples of feldspathic cumulate float rocks in Gale crater with >65% relict plagioclase. Bindi appears unaltered whereas Askival shows textural and compositional signatures of silicification, along with alkali remobilization and hydration. Askival likely experienced multiple stages of alteration, occurring first through acidic hydrolysis of metal cations, followed by deposition of silica and possible phyllosilicates at low T and neutral-alkaline pH. Through laser-induced breakdown spectroscopy compositional analyses and normative calculations, we suggest that an assemblage of Fe-Mg silicates including amphibole and pyroxene, Fe phases, and possibly Mg-rich phyllosilicate are present. Thermodynamic modeling of the more pristine Bindi composition predicts that amphibole and feldspar are stable within an upper crustal setting. This is consistent with the presence of amphibole in the parent igneous rocks of Askival and suggests that the paucity of amphiboles in other known Martian samples reflects the lack of representative samples of the Martian crust rather than their absence on Mars.
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Affiliation(s)
| | - John C. Bridges
- School of Physics and AstronomyUniversity of LeicesterLE1 7RHLeicesterUK
| | - Agnes Cousin
- Institut de Recherche en Astrophysique et PlanétologieUniversité de ToulouseCNRS, CNES31400ToulouseFrance
| | - William Rapin
- Institut de Recherche en Astrophysique et PlanétologieUniversité de ToulouseCNRS, CNES31400ToulouseFrance
| | - Julia Semprich
- AstrobiologyOU, School of Environment, Earth and Ecosystem SciencesThe Open UniversityMK7 6AAMilton KeynesWalton HallUK
| | - Olivier Gasnault
- Institut de Recherche en Astrophysique et PlanétologieUniversité de ToulouseCNRS, CNES31400ToulouseFrance
| | - Olivier Forni
- Institut de Recherche en Astrophysique et PlanétologieUniversité de ToulouseCNRS, CNES31400ToulouseFrance
| | - Patrick Gasda
- Los Alamos National Laboratory87545New MexicoLos AlamosUSA
| | - Debarati Das
- Department of Earth and Planetary SciencesMcGill UniversityH3A 0E8QuebecMontrealCanada
| | - Valerie Payré
- Department of Earth and Environmental SciencesThe University of Iowa52242IowaIowa CityUSA
| | | | - Candice C. Bedford
- Lunar and Planetary InstituteUSRA77058TexasHoustonUSA
- Astromaterials Research and Exploration ScienceNASA Johnson Space Center77058TexasHoustonUSA
| | - Roger C. Wiens
- Los Alamos National Laboratory87545New MexicoLos AlamosUSA
| | - Patrick Pinet
- Institut de Recherche en Astrophysique et PlanétologieUniversité de ToulouseCNRS, CNES31400ToulouseFrance
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Brown MAJ, Patel MR, Lewis SR, Holmes JA, Sellers GJ, Streeter PM, Bennaceur A, Liuzzi G, Villanueva GL, Vandaele AC. Impacts of Heterogeneous Chemistry on Vertical Profiles of Martian Ozone. J Geophys Res Planets 2022; 127:e2022JE007346. [PMID: 36588804 PMCID: PMC9787587 DOI: 10.1029/2022je007346] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/29/2022] [Revised: 10/21/2022] [Accepted: 10/25/2022] [Indexed: 06/17/2023]
Abstract
We show a positive vertical correlation between ozone and water ice using a vertical cross-correlation analysis with observations from the ExoMars Trace Gas Orbiter's Nadir and Occultation for Mars Discovery instrument. This is particularly apparent during L S = 0°-180°, Mars Year 35 at high southern latitudes, when the water vapor abundance is low. Ozone and water vapor are anti-correlated on Mars; Clancy et al. (2016, https://doi.org/10.1016/j.icarus.2015.11.016) also discuss the anti-correlation between ozone and water ice. However, our simulations with gas-phase-only chemistry using a 1-D model show that ozone concentration is not influenced by water ice. Heterogeneous chemistry has been proposed as a mechanism to explain the underprediction of ozone in global climate models (GCMs) through the removal of HO x . We find improving the heterogeneous chemical scheme by creating a separate tracer for the HO x adsorbed state, causes ozone abundance to increase when water ice is present (30-50 km), better matching observed trends. When water vapor abundance is high, there is no consistent vertical correlation between observed ozone and water ice and, in simulated scenarios, the heterogeneous chemistry has a minor influence on ozone. HO x , which are by-products of water vapor, dominate ozone abundance, masking the effects of heterogeneous chemistry on ozone, and making adsorption of HO x have a negligible impact on ozone. This is consistent with gas-phase-only modeled ozone, showing good agreement with observations when water vapor is abundant. Overall, the inclusion of heterogeneous chemistry improves the ozone vertical structure in regions of low water vapor abundance, which may partially explain GCM ozone deficits.
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Affiliation(s)
| | - M. R. Patel
- The Open UniversityMilton KeynesUK
- Space Science and Technology DepartmentScience and Technology Facilities CouncilRutherford Appleton LaboratoryOxfordshireUK
| | | | | | | | | | | | - G. Liuzzi
- Planetary Systems LaboratoryNASA Goddard Space Flight CenterGreenbeltMDUSA
- Department of PhysicsAmerican UniversityWashingtonDCUSA
| | - G. L. Villanueva
- Planetary Systems LaboratoryNASA Goddard Space Flight CenterGreenbeltMDUSA
| | - A. C. Vandaele
- Royal Belgian Institute for Space Aeronomy (BIRA‐IASB)BrusselsBelgium
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Holmes JA, Lewis SR, Patel MR, Alday J, Aoki S, Liuzzi G, Villanueva GL, Crismani MMJ, Fedorova AA, Olsen KS, Kass DM, Vandaele AC, Korablev O. Global Variations in Water Vapor and Saturation State Throughout the Mars Year 34 Dusty Season. J Geophys Res Planets 2022; 127:e2022JE007203. [PMID: 36589717 PMCID: PMC9788072 DOI: 10.1029/2022je007203] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/21/2022] [Revised: 09/30/2022] [Accepted: 10/05/2022] [Indexed: 06/17/2023]
Abstract
To understand the evolving martian water cycle, a global perspective of the combined vertical and horizontal distribution of water is needed in relation to supersaturation and water loss and how it varies spatially and temporally. The global vertical water vapor distribution is investigated through an analysis that unifies water, temperature and dust retrievals from several instruments on multiple spacecraft throughout Mars Year (MY) 34 with a global circulation model. During the dusty season of MY 34, northern polar latitudes are largely absent of water vapor below 20 km with variations above this altitude due to transport from mid-latitudes during a global dust storm, the downwelling branch of circulation during perihelion season and the intense MY 34 southern summer regional dust storm. Evidence is found of supersaturated water vapor breaking into the northern winter polar vortex. Supersaturation above around 60 km is found for most of the time period, with lower altitudes showing more diurnal variation in the saturation state of the atmosphere. Discrete layers of supersaturated water are found across all latitudes. The global dust storm and southern summer regional dust storm forced water vapor at all latitudes in a supersaturated state to 60-90 km where it is more likely to escape from the atmosphere. The reanalysis data set provides a constrained global perspective of the water cycle in which to investigate the horizontal and vertical transport of water throughout the atmosphere, of critical importance to understand how water is exchanged between different reservoirs and escapes the atmosphere.
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Affiliation(s)
- J. A. Holmes
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - S. R. Lewis
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - M. R. Patel
- School of Physical SciencesThe Open UniversityMilton KeynesUK
- Space Science and Technology DepartmentScience and Technology Facilities CouncilRutherford Appleton LaboratoryDidcotUK
| | - J. Alday
- School of Physical SciencesThe Open UniversityMilton KeynesUK
- Department of PhysicsUniversity of OxfordOxfordUK
| | - S. Aoki
- Institute of Space and Astronautical ScienceJapan Aerospace Exploration AgencyKanagawaJapan
- Royal Belgian Institute for Space AeronomyBrusselsBelgium
| | - G. Liuzzi
- NASA Goddard Space Flight CenterGreenbeltMDUSA
- Department of PhysicsAmerican UniversityWashingtonDCUSA
| | | | - M. M. J. Crismani
- Department of PhysicsCalifornia State University San BernardinoSan BernardinoCAUSA
| | - A. A. Fedorova
- Space Research Institute of the Russian Academy of Sciences (IKI RAS)MoscowRussia
| | - K. S. Olsen
- Department of PhysicsUniversity of OxfordOxfordUK
| | - D. M. Kass
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - A. C. Vandaele
- Royal Belgian Institute for Space AeronomyBrusselsBelgium
| | - O. Korablev
- Space Research Institute of the Russian Academy of Sciences (IKI RAS)MoscowRussia
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Caravaca G, Mangold N, Dehouck E, Schieber J, Zaugg L, Bryk AB, Fedo CM, Le Mouélic S, Le Deit L, Banham SG, Gupta S, Cousin A, Rapin W, Gasnault O, Rivera‐Hernández F, Wiens RC, Lanza NL. From Lake to River: Documenting an Environmental Transition Across the Jura/Knockfarril Hill Members Boundary in the Glen Torridon Region of Gale Crater (Mars). J Geophys Res Planets 2022; 127:e2021JE007093. [PMID: 36246083 PMCID: PMC9541347 DOI: 10.1029/2021je007093] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 10/14/2021] [Revised: 04/12/2022] [Accepted: 04/12/2022] [Indexed: 06/16/2023]
Abstract
Between January 2019 and January 2021, the Mars Science Laboratory team explored the Glen Torridon (GT) region in Gale crater (Mars), known for its orbital detection of clay minerals. Mastcam, Mars Hand Lens Imager, and ChemCam data are used in an integrated sedimentological and geochemical study to characterize the Jura member of the upper Murray formation and the Knockfarril Hill member of the overlying Carolyn Shoemaker formation in northern GT. The studied strata show a progressive transition represented by interfingering beds of fine-grained, recessive mudstones of the Jura member and coarser-grained, cross-stratified sandstones attributed to the Knockfarril Hill member. Whereas the former are interpreted as lacustrine deposits, the latter are interpreted as predominantly fluvial deposits. The geochemical composition seen by the ChemCam instrument show K2O-rich mudstones (∼1-2 wt.%) versus MgO-rich sandstones (>6 wt.%), relative to the average composition of the underlying Murray formation. We document consistent sedimentary and geochemical data sets showing that low-energy mudstones of the Jura member are associated with the K-rich endmember, and that high-energy cross-stratified sandstones of the Knockfarril Hill member are associated with the Mg-rich endmember, regardless of stratigraphic position. The Jura to Knockfarril Hill transition therefore marks a significant paleoenvironmental change, where a long-lived and comparatively quiescent lacustrine setting progressively changes into a more energetic fluvial setting, as a consequence of shoreline regression due to either increased sediment supply or lake-level drop.
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Affiliation(s)
- Gwénaël Caravaca
- UMR 5277 CNRSUPSCNES Institut de Recherche en Astrophysique et PlanétologieUniversité Paul Sabatier Toulouse IIIToulouseFrance
- UMR 6112 CNRS Laboratoire de Planétologie et GéosciencesNantes UniversitéUniversité d’AngersNantesFrance
- Now at Institut de Recherche en Astrophysique et PlanétologieToulouseFrance
| | - Nicolas Mangold
- UMR 6112 CNRS Laboratoire de Planétologie et GéosciencesNantes UniversitéUniversité d’AngersNantesFrance
| | - Erwin Dehouck
- Université de LyonUCBLENSLUJMCNRSLGL‐TPEVilleurbanneFrance
| | - Juergen Schieber
- Department of Geological SciencesIndiana University BloomingtonBloomingtonINUSA
| | - Louis Zaugg
- UMR 6112 CNRS Laboratoire de Planétologie et GéosciencesNantes UniversitéUniversité d’AngersNantesFrance
| | | | - Christopher M. Fedo
- Department of Earth & Planetary SciencesUniversity of TennesseeKnoxvilleTNUSA
| | - Stéphane Le Mouélic
- UMR 6112 CNRS Laboratoire de Planétologie et GéosciencesNantes UniversitéUniversité d’AngersNantesFrance
| | - Laetitia Le Deit
- UMR 6112 CNRS Laboratoire de Planétologie et GéosciencesNantes UniversitéUniversité d’AngersNantesFrance
| | - Steven G. Banham
- Department of Earth Sciences and EngineeringImperial College LondonLondonUK
| | - Sanjeev Gupta
- Department of Earth Sciences and EngineeringImperial College LondonLondonUK
| | - Agnès Cousin
- UMR 5277 CNRSUPSCNES Institut de Recherche en Astrophysique et PlanétologieUniversité Paul Sabatier Toulouse IIIToulouseFrance
| | - William Rapin
- UMR 5277 CNRSUPSCNES Institut de Recherche en Astrophysique et PlanétologieUniversité Paul Sabatier Toulouse IIIToulouseFrance
| | - Olivier Gasnault
- UMR 5277 CNRSUPSCNES Institut de Recherche en Astrophysique et PlanétologieUniversité Paul Sabatier Toulouse IIIToulouseFrance
| | | | - Roger C. Wiens
- Earth, Atmospheric, and Planetary SciencesPurdue UniversityWest LafayetteINUSA
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5
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Collins GS, Newland EL, Schwarz D, Coleman M, McMullan S, Daubar IJ, Miljković K, Neidhart T, Sansom E. Meteoroid Fragmentation in the Martian Atmosphere and the Formation of Crater Clusters. J Geophys Res Planets 2022; 127:e2021JE007149. [PMID: 36247718 PMCID: PMC9541127 DOI: 10.1029/2021je007149] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/06/2021] [Revised: 05/20/2022] [Accepted: 06/18/2022] [Indexed: 06/16/2023]
Abstract
The current rate of small impacts on Mars is informed by more than one thousand impact sites formed in the last 20 years, detected in images of the martian surface. More than half of these impacts produced a cluster of small craters formed by fragmentation of the meteoroid in the martian atmosphere. The spatial distributions, number and sizes of craters in these clusters provide valuable constraints on the properties of the impacting meteoroid population as well as the meteoroid fragmentation process. In this paper, we use a recently compiled database of crater cluster observations to calibrate a model of meteoroid fragmentation in Mars' atmosphere and constrain key model parameters, including the lift coefficient and fragment separation velocity, as well as meteoroid property distributions. The model distribution of dynamic meteoroid strength that produces the best match to observations has a minimum strength of 10-90 kPa, a maximum strength of 3-6 MPa and a median strength of 0.2-0.5 MPa. An important feature of the model is that individual fragmentation events are able to produce fragments with a wide range of dynamic strengths as much as 10 times stronger or weaker than the parent fragment. The calibrated model suggests that the rate of small impacts on Mars is 1.5-4 times higher than recent observation-based estimates. It also shows how impactor properties relevant to seismic wave generation, such as the total impact momentum, can be inferred from cluster characteristics.
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Affiliation(s)
- G. S. Collins
- Department of Earth Science and EngineeringImperial CollegeLondonUK
| | - E. L. Newland
- Department of Earth Science and EngineeringImperial CollegeLondonUK
| | - D. Schwarz
- Department of Earth Science and EngineeringImperial CollegeLondonUK
| | - M. Coleman
- Department of Earth Science and EngineeringImperial CollegeLondonUK
| | - S. McMullan
- Department of Earth Science and EngineeringImperial CollegeLondonUK
| | - I. J. Daubar
- Earth, Environmental, and Planetary SciencesBrown UniversityProvidenceRIUSA
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6
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Palmerio E, Nieves‐Chinchilla T, Kilpua EKJ, Barnes D, Zhukov AN, Jian LK, Witasse O, Provan G, Tao C, Lamy L, Bradley TJ, Mays ML, Möstl C, Roussos E, Futaana Y, Masters A, Sánchez‐Cano B. Magnetic Structure and Propagation of Two Interacting CMEs From the Sun to Saturn. J Geophys Res Space Phys 2021; 126:e2021JA029770. [PMID: 35864948 PMCID: PMC9286593 DOI: 10.1029/2021ja029770] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/08/2021] [Revised: 10/01/2021] [Accepted: 10/05/2021] [Indexed: 06/15/2023]
Abstract
One of the grand challenges in heliophysics is the characterization of coronal mass ejection (CME) magnetic structure and evolution from eruption at the Sun through heliospheric propagation. At present, the main difficulties are related to the lack of direct measurements of the coronal magnetic fields and the lack of 3D in-situ measurements of the CME body in interplanetary space. Nevertheless, the evolution of a CME magnetic structure can be followed using a combination of multi-point remote-sensing observations and multi-spacecraft in-situ measurements as well as modeling. Accordingly, we present in this work the analysis of two CMEs that erupted from the Sun on April 28, 2012. We follow their eruption and early evolution using remote-sensing data, finding indications of CME-CME interaction, and then analyze their interplanetary counterpart(s) using in-situ measurements at Venus, Earth, and Saturn. We observe a seemingly single flux rope at all locations, but find possible signatures of interaction at Earth, where high-cadence plasma data are available. Reconstructions of the in-situ flux ropes provide almost identical results at Venus and Earth but show greater discrepancies at Saturn, suggesting that the CME was highly distorted and/or that further interaction with nearby solar wind structures took place before 10 AU. This work highlights the difficulties in connecting structures from the Sun to the outer heliosphere and demonstrates the importance of multi-spacecraft studies to achieve a deeper understanding of the magnetic configuration of CMEs.
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Affiliation(s)
- Erika Palmerio
- Space Sciences LaboratoryUniversity of California–BerkeleyBerkeleyCAUSA
- CPAESSUniversity Corporation for Atmospheric ResearchBoulderCOUSA
| | | | | | - David Barnes
- STFC RAL SpaceRutherford Appleton LaboratoryHarwell CampusOxfordshireUK
| | - Andrei N. Zhukov
- Solar–Terrestrial Centre of Excellence—SIDCRoyal Observatory of BelgiumBrusselsBelgium
- Skobeltsyn Institute of Nuclear PhysicsMoscow State UniversityMoscowRussia
| | - Lan K. Jian
- Heliophysics Science DivisionNASA Goddard Space Flight CenterGreenbeltMDUSA
| | | | - Gabrielle Provan
- School of Physics and AstronomyUniversity of LeicesterLeicesterUK
| | - Chihiro Tao
- National Institute of Information and Communications Technology (NICT)KoganeiJapan
| | - Laurent Lamy
- LESIAObservatoire de ParisPSLCNRSUPMCUniversité Paris DiderotMeudonFrance
- LAMPythéasAix Marseille UniversitéCNRSCNESMarseilleFrance
| | | | - M. Leila Mays
- Heliophysics Science DivisionNASA Goddard Space Flight CenterGreenbeltMDUSA
| | - Christian Möstl
- Space Research InstituteAustrian Academy of SciencesGrazAustria
- Institute of GeodesyGraz University of TechnologyGrazAustria
| | - Elias Roussos
- Max Planck Institute for Solar System ResearchGöttingenGermany
| | | | - Adam Masters
- The Blackett LaboratoryImperial College LondonLondonUK
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