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Wednesday, March 22, 2017 [W453] MARTIAN METEORITE MADNESS: MIXING on a VARIETY of SCALES 1:30 P.M
Lunar and Planetary Science XLVIII (2017) sess453.pdf Wednesday, March 22, 2017 [W453] MARTIAN METEORITE MADNESS: MIXING ON A VARIETY OF SCALES 1:30 p.m. Waterway Ballroom 5 Chairs: Arya Udry Geoffrey Howarth 1:30 p.m. Nielsen S. G. * Magna T. Mezger K. The Vanadium Isotopic Composition of Mars and Evidence for Solar System Heterogeneity During Planetary Accretion [#1225] Vanadium isotope composition of Mars distinct from Earth and chondrites. 1:45 p.m. Tait K. T. * Day J. M. D. Highly Siderophile Element and Os-Sr Isotope Systematics of Shergotittes [#3025] The shergottite meteorites represent geochemically diverse, broadly basaltic, and magmatically-derived rocks from Mars. New samples were processed and analyzed. 2:00 p.m. Armytage R. M. G. * Debaille V. Brandon A. D. Agee C. B. The Neodymium and Hafnium Isotopic Composition of NWA 7034, and Constraints on the Enriched End-Member for Shergottites [#1065] Couple Sm-Nd and Lu-Hf isotopic systematics in NWA 7034 suggest that such a crust is not the enriched end-member for shergottites. 2:15 p.m. Howarth G. H. * Udry A. Nickel in Olivine and Constraining Mantle Reservoirs for Shergottite Meteorites [#1375] Ni enrichment in olivine from enriched versus depleted shergottites provide evidence for constraining mantle reservoirs on Mars. 2:30 p.m. Jean M. M. * Taylor L. A. Exploring Martian Mantle Heterogeneity: Multiple SNC Reservoirs Revealed [#1666] The objective of the present study is to assess how many mixing components can be recognized, and address ongoing debates within the martian isotope community. 2:45 p.m. Udry A. * Day J. -
Aqueous Alteration in Martian Meteorites: Comparing Mineral Relations in Igneous-Rock Weathering of Martian Meteorites and in the Sedimentary Cycle of Mars
AQUEOUS ALTERATION IN MARTIAN METEORITES: COMPARING MINERAL RELATIONS IN IGNEOUS-ROCK WEATHERING OF MARTIAN METEORITES AND IN THE SEDIMENTARY CYCLE OF MARS MICHAEL A. VELBEL Department of Geological Sciences, 206 Natural Science Building, Michigan State University, East Lansing, Michigan 48824-1115 USA e-mail: [email protected] ABSTRACT: Many of the minerals observed or inferred to occur in the sediments and sedimentary rocks of Mars, from a variety of Mars-mission spacecraft data, also occur in Martian meteorites. Even Martian meteorites recovered after some exposure to terrestrial weathering can preserve preterrestrial evaporite minerals and useful information about aqueous alteration on Mars, but the textures and textural contexts of such minerals must be examined carefully to distinguish preterrestrial evaporite minerals from occurrences of similar minerals redistributed or formed by terrestrial processes. Textural analysis using terrestrial microscopy provides strong and compelling evidence for preterrestrial aqueous alteration products in a numberof Martian meteorites. Occurrences of corroded primary rock-forming minerals and alteration products in meteorites from Mars cover a range of ages of mineral–water interaction, from ca. 3.9 Ga (approximately mid-Noachian), through one or more episodes after ca. 1.3 Ga (approximately mid–late Amazonian), through the last half billion years (late Amazonian alteration in young shergottites), to quite recent. These occurrences record broadly similar aqueous corrosion processes and formation of soluble weathering products over a broad range of times in the paleoenvironmental history of the surface of Mars. Many of the same minerals (smectite-group clay minerals, Ca-sulfates, Mg-sulfates, and the K-Fe–sulfate jarosite) have been identified both in the Martian meteorites and from remote sensing of the Martian surface. -
Appendix a Recovery of Ejecta Material from Confirmed, Probable
Appendix A Recovery of Ejecta Material from Confirmed, Probable, or Possible Distal Ejecta Layers A.1 Introduction In this appendix we discuss the methods that we have used to recover and study ejecta found in various types of sediment and rock. The processes used to recover ejecta material vary with the degree of lithification. We thus discuss sample processing for unconsolidated, semiconsolidated, and consolidated material separately. The type of sediment or rock is also important as, for example, carbonate sediment or rock is processed differently from siliciclastic sediment or rock. The methods used to take and process samples will also vary according to the objectives of the study and the background of the investigator. We summarize below the methods that we have found useful in our studies of distal impact ejecta layers for those who are just beginning such studies. One of the authors (BPG) was trained as a marine geologist and the other (BMS) as a hard rock geologist. Our approaches to processing and studying impact ejecta differ accordingly. The methods used to recover ejecta from unconsolidated sediments have been successfully employed by BPG for more than 40 years. A.2 Taking and Handling Samples A.2.1 Introduction The size, number, and type of samples will depend on the objective of the study and nature of the sediment/rock, but there a few guidelines that should be followed regardless of the objective or rock type. All outcrops, especially those near industrialized areas or transportation routes (e.g., highways, train tracks) need to be cleaned off (i.e., the surface layer removed) prior to sampling. -
Heating Experiments of Maskelynite in Zagami, Elephant Moraine A79001 and Allan Hills 77005: Implications for the Effect of Shock Heating
51st Lunar and Planetary Science Conference (2020) 1803.pdf HEATING EXPERIMENTS OF MASKELYNITE IN ZAGAMI, ELEPHANT MORAINE A79001 AND ALLAN HILLS 77005: IMPLICATIONS FOR THE EFFECT OF SHOCK HEATING. R. Shikina1,2 and T. Mikouchi1,2, 1Department of Earth and Planet. Science, The University of Tokyo, Hongo, Tokyo 113-0033, Japan ([email protected]), 2The University Museum, The University of Tokyo, Hongo, Tokyo 113-0033, Japan. Introduction: Plagioclase is one of the important along the cracks and at edges of the original grains. constituents of extraterrestrial materials and is sensi- Although maskelynites appear to have a smooth sur- tive to the shock metamorphism. Maskelynite is under- face through optical microscopy, the recrystallized stood as a diaplectic plagioclase glass that has been plagioclase shows a dirty devitrified texture. Electron transformed from plagioclase in solid-state transfor- microprobe analysis (shown in Fig. 2) revealed that Na mation by strong impact and is commonly found in and K are reduced, but Ca is enriched in the recrystal- Martian meteorites [1]. Maskelynite is known to be lized plagioclase of the samples showing partial recrys- easily converted to crystalline plagioclase by reheating tallization (900 °C for 8 and 24 hours and 1000 °C for and the degree of recrystallization depends upon shock 1 hour). In the maskelynite grains heated at 900 °C for pressure [2]. Such plagioclase recrystallizations is 168 hours, small glass regions enriched in Na and K found in meteorites. For example, the lunar meteorite are present (Na2O: ~6.5 wt%, K2O: ~2.5 wt%), sug- Y-793169 shows a recrystallized polycrystalline plagi- gesting that Na and K concentrate in areas where re- oclase texture by a reheating event after the formation crystallization did not start yet. -
Ejection of Martian Meteorites
Meteoritics & Planetary Science 40, Nr 9/10, 1393–1411 (2005) Abstract available online at http://meteoritics.org Ejection of Martian meteorites Jˆrg FRITZ1*, Natalia ARTEMIEVA2, and Ansgar GRESHAKE1 1Institut f¸r Mineralogie, Museum f¸r Naturkunde, Humboldt-Universit‰t zu Berlin, Invalidenstrasse 43, 10115 Berlin, Germany 2Institute for Dynamics of Geospheres, Russian Academy of Science, Leninsky Prospect 38, Building 1, Moscow 119334, Russia *Corresponding author. E-mail: [email protected] (Received 29 March 2005; revision accepted 11 April 2005) Abstract–We investigated the transfer of meteorites from Mars to Earth with a combined mineralogical and numerical approach. We used quantitative shock pressure barometry and thermodynamic calculations of post-shock temperatures to constrain the pressure/temperature conditions for the ejection of Martian meteorites. The results show that shock pressures allowing the ejection of Martian meteorites range from 5 to 55 GPa, with corresponding post-shock temperature elevations of 10 to about 1000 °C. With respect to shock pressures and post-shock temperatures, an ejection of potentially viable organisms in Martian surface rocks seems possible. A calculation of the cooling time in space for the most highly shocked Martian meteorite Allan Hills (ALH) 77005 was performed and yielded a best-fit for a post-shock temperature of 1000 °C and a meteoroid size of 0.4 to 0.6 m. The final burial depths of the sub-volcanic to volcanic Martian rocks as indicated by textures and mineral compositions of meteorites are in good agreement with the postulated size of the potential source region for Martian meteorites during the impact of a small projectile (200 m), as defined by numerical modeling (Artemieva and Ivanov 2004). -
Localized Shock Melting in Lherzolitic Shergottite Northwest Africa 1950: Comparison with Allan Hills 77005
Meteoritics & Planetary Science 42, Nr 1, 63–80 (2007) Abstract available online at http://meteoritics.org Localized shock melting in lherzolitic shergottite Northwest Africa 1950: Comparison with Allan Hills 77005 E. L. WALTON* and C. D. K. HERD 1Department of Earth and Atmospheric Sciences, 1-26 Earth Sciences Building, University of Alberta, Edmonton, Alberta T6G 2E3, Canada *Corresponding author. E-mail: [email protected] (Received 14 June 2006; revision accepted 04 November 2006) Abstract–The lherzolitic Martian meteorite Northwest Africa (NWA) 1950 consists of two distinct zones: 1) low-Ca pyroxene poikilically enclosing cumulate olivine (Fo70–75) and chromite, and 2) areas interstitial to the oikocrysts comprised of maskelynite, low- and high-Ca pyroxene, cumulate olivine (Fo68–71) and chromite. Shock metamorphic effects, most likely associated with ejection from the Martian subsurface by large-scale impact, include mechanical deformation of host rock olivine and pyroxene, transformation of plagioclase to maskelynite, and localized melting (pockets and veins). These shock effects indicate that NWA 1950 experienced an equilibration shock pressure of 35–45 GPa. Large (millimeter-size) melt pockets have crystallized magnesian olivine (Fo78–87) and chromite, embedded in an Fe-rich, Al-poor basaltic to picro-basaltic glass. Within the melt pockets strong thermal gradients (minimum 1 °C/μm) existed at the onset of crystallization, giving rise to a heterogeneous distribution of nucleation sites, resulting in gradational textures of olivine and chromite. Dendritic and skeletal olivine, crystallized in the melt pocket center, has a nucleation density (1.0 × 103 crystals/mm2) that is two orders of magnitude lower than olivine euhedra near the melt margin (1.6 × 105 crystals/mm2). -
American Journal of Science, Vol
[American Journal of Science, Vol. 313, November, 2013,P.807–843, DOI 10.2475/09.2013.01] American Journal of Science NOVEMBER 2013 PALEOMINERALOGY OF THE HADEAN EON: A PRELIMINARY SPECIES LIST ROBERT M. HAZEN* “By the way, were there any clay minerals in the Archean?” Harold Morowitz, December 6, 2006 ABSTRACT. The Hadean Eon, encompassing Earth’s first 550 million years, was a time of significant planetary evolution. Nevertheless, prebiotic Earth’s near-surface environment may have held no more than approximately 420 different rock-forming or accessory mineral species that were widely distributed and/or volumetrically significant. This relative Hadean mineralogical parsimony is a consequence of the limited modes of mineral paragenesis prior to 4 Ga compared to the last 3.0 billion years. Dominant Hadean Eon mineralizing processes include the evolution of a diverse suite of intrusive and extrusive igneous lithologies; hydrothermal alteration over a wide temperature range, notably serpentinization; authigenesis in marine sediments; diagenesis and low-grade metamorphism in near-surface environments; and impact- related processes, including shock mineralization, creation of marginal hydrothermal zones, and excavation of deep metamorphosed terrains. On the other hand, the Hadean Eon may have been notably lacking in mineralization generated by plate tectonic processes, such as subduction zone volcanism and associated fluid-rock interactions, which result in massive sulfide deposition; convergent boundary orogene- sis and consequent extensive granitoid-rooted continental landmasses; and the selec- tion and concentration of incompatible elements in complex pegmatites, with hun- dreds of accompanying minerals. The dramatic mineralogical consequences of life are reflected in the absence of Hadean biomineralization; for example, the lack of extensive carbonate deposits and the associated restricted development of skarn and cave minerals prior to 4 Ga. -
Petrogenesis, Alteration, and Shock History of Intermediate Shergottite Northwest Africa 7042: Evidence for Hydrous Magmatism on Mars?
Available online at www.sciencedirect.com ScienceDirect Geochimica et Cosmochimica Acta 283 (2020) 103–123 www.elsevier.com/locate/gca Petrogenesis, alteration, and shock history of intermediate shergottite Northwest Africa 7042: Evidence for hydrous magmatism on Mars? T.V. Kizovski a,b,⇑, M.R.M. Izawa a,1, K.T. Tait a,b, D.E. Moser c, J.M.D. Day d, B.C. Hyde a,c, L.F. White a,b, L. Kovarik e, S.D. Taylor f, D.E. Perea e, I.R. Barker c, B.R. Joy g a Centre for Applied Planetary Mineralogy, Department of Natural History, Royal Ontario Museum, 100 Queen’s Park, Toronto, Ontario M5S 2C6, Canada b Department of Earth Sciences, University of Toronto, 22 Russell Street, Toronto, Ontario M5S 3B1, Canada c Department of Earth Sciences, University of Western Ontario, London, Ontario N6A 5B7, Canada d Scripps Institution of Oceanography, University of California San Diego, La Jolla, CA 92093-0244, USA e Environmental Molecular Sciences Laboratory, Pacific Northwest National Laboratory, Richland, WA 99352, USA f Physical and Computational Sciences Directorate, Pacific Northwest National Laboratory, Richland, WA 99352, USA g Department of Geological Sciences and Geological Engineering, Queen’s University, Kingston, Ontario K7L 3N6, Canada Received 23 August 2019; accepted in revised form 27 May 2020; available online 4 June 2020 Abstract Northwest Africa (NWA) 7042 is an intermediate, permafic shergottite consisting of two generations of olivine (early zoned olivine Fo41-76, and late-stage fayalitic olivine Fo46-56), complexly zoned pyroxene (En35-64Fs22-46Wo5-34), shock-melted or maskelynitized feldspar (An5-30Ab16-61Or1-47), and accessory merrillite, apatite, ilmenite, titanomagnetite, Fe-Cr-Ti spinels, pyrrhotite, and baddeleyite. -
Pb Evolution in the Martian Mantle
*Manuscript Click here to view linked References 1 Pb evolution in the Martian mantle 1* 1,2 1 1 2 2 J. J. Bellucci , A. A. Nemchin , M. J. Whitehouse , J. F. Snape , P. Bland , G.K. 3 Benedix2, J. Roszjar3 4 5 *Corresponding author, email address: [email protected] 6 7 1Department of Geosciences, Swedish Museum of Natural History, SE-104 05 8 Stockholm, Sweden 9 2 Department of Applied Geology, Curtin University, Perth, WA 6845, Australia 10 3Department of Mineralogy and Petrography, Natural History Museum Vienna, Burgring 11 7, 1010 Vienna, Austria. 12 13 Abstract 14 The initial Pb compositions of one enriched shergottite, one intermediate 15 shergottite, two depleted shergottites, and Nakhla have been measured by Secondary Ion 16 Mass Spectrometry (SIMS). These values, in addition to data from previous studies using 17 an identical analytical method performed on three enriched shergottites, ALH 84001, and 18 Chassigny, are used to construct a unified and internally consistent model for the 19 differentiation history of the Martian mantle and crystallization ages for Martian 20 meteorites is presented. The differentiation history of the shergottites and 21 Nakhla/Chassigny are fundamentally different, which is in agreement with short-lived 22 radiogenic isotope systematics. The initial Pb compositions of Nakhla/Chassigny are best 23 explained by late addition of a Pb-enriched component with a primitive, non-radiogenic 24 composition. In contrast, the Pb isotopic compositions of the shergottite group indicate a 25 relatively simple evolutionary history of the Martian mantle that can be modeled based 26 on recent results from the Sm-Nd system. -
Expanding the Application of the Eu-Oxybarometer to The
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Caltech Authors - Main Meteoritics & Planetary Science 44, Nr 5, 725–745 (2009) Abstract available online at http://meteoritics.org Expanding the application of the Eu-oxybarometer to the lherzolitic shergottites and nakhlites: Implications for the oxidation state heterogeneity of the Martian interior Molly C. MCCANTA1, 4*, Linda ELKINS-TANTON2, and Malcolm J. RUTHERFORD3 1California Institute of Technology, Department of Geological and Planetary Sciences, MS 170-25, Pasadena, California 91125, USA 2Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, 77 Massachusetts Ave., Building 54, Room 824, Cambridge, Massachusetts 02139, USA 3Brown University, Department of Geological Sciences, 324 Brook St., Providence, Rhode Island 02912, USA 4Present address: Tufts University, Geology Department, Lane Hall, 2 North Hill Road, Medford, Massachusetts 02155, USA *Corresponding author. E-mail: [email protected] (Received 07 July 2008; revision accepted 06 February 2009) Abstract–Experimentally rehomogenized melt inclusions from the nakhlite Miller Range 03346 (MIL 03346) and the lherzolitic shergottite Allan Hills 77005 (ALH 77005) have been analyzed for their rare earth element (REE) concentrations in order to characterize the early melt compositions of these Martian meteorites and to calculate the oxygen fugacity conditions they crystallized under. D(Eu/Sm)pyroxene/melt values were measured at 0.77 and 1.05 for ALH 77005 and MIL 03346, respectively. These melts and their associated whole rock compositions have similar REE patterns, suggesting that whole rock REE values are representative of those of the early melts and can be used as input into the pyroxene Eu-oxybarometer for the nakhlites and lherzolitic shergottites. -
Meteoritic Evidence for Historical Biosignatures J
84th Annual Meeting of The Meteoritical Society 2021 (LPI Contrib. No. 2609) 6003.pdf WAS THE RED PLANET ONCE BLUE? METEORITIC EVIDENCE FOR HISTORICAL BIOSIGNATURES J. C. Johnson1,2, P. A. Johnson1,2 and A. A. Mardon1,2, 1University of Alberta (116 St 85 Ave NW, Edmonton, Alta, Canada, T6G 2R3, [email protected]; [email protected]) for first author, 2Antarctic Institute of Canada (PO Box 99548 Cromdale PO Edmonton, Alta, Canada T5B0E1, [email protected]). Introduction: We have reached new degrees of certainty to suggest signatures of life beyond Mother Earth. Since the earliest days of space exploration, we have accumulated a large repository of evidence about the existence, motions, and evolution of celestial bodies. Yet, conjecture of whether there is life beyond us has perplexed and been subjected to heated debate by both scientist and sensationalist audiences. Historical Mars Expeditions: In the 1970s, the Viking collected soil samples “spiked” with organic nutrients like amino acids. These samples showed measurements approximately akin to what we would expect were there to be life present on the surface of Mars. Over time though, the scientific majority argued that these were merely the result of chemically reactive components present in the soil that reacted with terrestrial contaminants of the Earth to produce organic by-products. [1] However, discoveries from the Curiosity rover suggested otherwise. Using evolved gas analysis and chromatog- raphy-spectrometry techniques, the first conclusive proof of the presence of native organic matter on Mars was rec- orded. [2] Coupled with evidence the unit found for ancient lakes and water underneath the Martian regolith, the case for Martian life may be even stronger piecing this jigsaw together. -
A New Lherzolitic Shergottite from the Japanese Antarctic Meteorite Collection
Antarct. Meteorite Res., 10, 41-60, 1997 YA MAT0-793605: A NEW LHERZOLITIC SHERGOTTITE FROM THE JAPANESE ANTARCTIC METEORITE COLLECTION Takashi MIKOUCHI and Masamichi MIYAMOTO Mineralogical Institute, Graduate School of Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo I I 3 Abstract: Y-793605 is a new martian meteorite from Antarctica that can be clas sified as a lherzolitic shergottite. Y-793605 mainly shows a poikilitic texture (large pyroxene oikocryst with enclosed olivine and chromite), but partly contains non poikilitic areas (mainly maskelynite, olivine, and pigeonite). Olivine in the non poikilitic area is more Fe-rich and shows a narrower compositional distribution than that in the poikilitic area. Low-Ca pyroxenes in the non-poikilitic area are also more Fe-rich (Eno5Fs2RW01-En6(iFS21Wou) than those in the poikilitic area (En16Fs21Wor Eno0Fs21W 011 ). Augites in the poikilitic area are usually present rimming the oikocrysts (En52Fs16Wo12 to En49FS14Wo)1). The crystallization sequence of minerals in Y-793605 is considered to have begun by initial crystallization of cumulus phases (olivine and chromite) from the parent magma. Then, low-Ca pyroxenes and later augite poikilitically enclosed cumulus phases, and became a large oikocryst. Due to accumulation of phases, small interstitial melts formed between the oikocryst boundaries, and plagioclase crystallized from the Ca-Fe-rich melt along with pigeonite. After minor augite crystallization in the non-poikilitic area, all phases experienced re-equilibration (e.g., homogenization of olivine). Y-793605 shows a close relationship to previously known lherzolitic shergottites ALH77005 and LEW88516. Especially, olivine composition of Y-793605 is nearly identical to that of LEW885 l 6.