The Mineral Olivine Is an Example Of
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Bedrock Geology Glossary from the Roadside Geology of Minnesota, Richard W
Minnesota Bedrock Geology Glossary From the Roadside Geology of Minnesota, Richard W. Ojakangas Sedimentary Rock Types in Minnesota Rocks that formed from the consolidation of loose sediment Conglomerate: A coarse-grained sedimentary rock composed of pebbles, cobbles, or boul- ders set in a fine-grained matrix of silt and sand. Dolostone: A sedimentary rock composed of the mineral dolomite, a calcium magnesium car- bonate. Graywacke: A sedimentary rock made primarily of mud and sand, often deposited by turbidi- ty currents. Iron-formation: A thinly bedded sedimentary rock containing more than 15 percent iron. Limestone: A sedimentary rock composed of calcium carbonate. Mudstone: A sedimentary rock composed of mud. Sandstone: A sedimentary rock made primarily of sand. Shale: A deposit of clay, silt, or mud solidified into more or less a solid rock. Siltstone: A sedimentary rock made primarily of sand. Igneous and Volcanic Rock Types in Minnesota Rocks that solidified from cooling of molten magma Basalt: A black or dark grey volcanic rock that consists mainly of microscopic crystals of pla- gioclase feldspar, pyroxene, and perhaps olivine. Diorite: A plutonic igneous rock intermediate in composition between granite and gabbro. Gabbro: A dark igneous rock consisting mainly of plagioclase and pyroxene in crystals large enough to see with a simple magnifier. Gabbro has the same composition as basalt but contains much larger mineral grains because it cooled at depth over a longer period of time. Granite: An igneous rock composed mostly of orthoclase feldspar and quartz in grains large enough to see without using a magnifier. Most granites also contain mica and amphibole Rhyolite: A felsic (light-colored) volcanic rock, the extrusive equivalent of granite. -
Uhm Phd 9230509 R.Pdf
INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand corner and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. Higher quality 6" x 9" black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. U·M·I University Microfilms International A Bell & Howetl truorrnanoo Company 300 North Zeeb Road. Ann Arbor. M148106-1346 USA 313,761-4700 800 521-0600 Order Number 9230509 Mid-ocean ridge magmatism: Style of mantle upwelling, partial melting, crustal level processes, and spreading rate dependence. A petrologic approach Niu, Yaoling, Ph.D. -
The Geological Newsletter
JAN 90 THE GEOLOGICAL NEWSLETTER ·• GEOLOGICAL SOCIETY OF THE OREGON COUNTRY GEOLOGICAL SOCIETY Non-Profit Org. U.S. POSTAGE OF THE OREGON COUNTRY PAID P.O. BOX ?a 7- Portland, Oregon PORTLAND, OR 97207- -:· ·--~··, Permit No. 999 - -- '~ Dr. Frank Boersma 120 W. 33~d Street Vancouver, WA 98660 GEOLOGICAL SOCIETY OF THE OREGOt\ COllNTRY 1989-1990 ADMINISTRATION BOARD OF DIRECTORS President Directors Rosemary Kenney 221-0757 Peter E. Baer (3 years) 661-7995 4211 S\-1 Condor Charlene Holzwarth (2 years) 284-3444 Portland, OR 97201 Esther Kennedy (1 year) 287-3091 Vice President Margaret L. Steere 246-1670 Immediate Past Presidents Joline Robustelli 223-2852 6929 SW 34 Ave. ~ Portland, OR 97219 R.E. (Andy) Corcoran 244-5605 Secretary Alta B. Fosback 641-6323 THE GEOLOGICAL NEWSLETTER 8942 SW Fairview Place Tigard, OR 97223 Editor: Sandra Anderson 775-5538 Treasurer Calendar: Margaret Steere 246-1670 Braden Pillow 659-6318 Business Manager: Carol Cole 220-0078 19562 SE Cottonwood St. Assist: Cecelia Crater 235-5158 Milwaukie, OR 97267 ACTIVITIES CHAIRS Calligrapher Properties and PA System Wallace R.· McClung 637-3834 (Luncheon) Donald Botteron 245-6251 Field Trips (Evening) Walter A. Sunderland 625-6840 Charlene Holzwarth 284-3444 Publications Alta B. Fosback 641-6323 Geneva E. Reddekopp 654-9818 Geology Seminars Publicity Donald D. Barr 246-2785 Roberta L. Walter 235-3579 Historian Refreshments Phyllis G. Bonebrake 289-8597 (Friday Evening) Hospitality David and Marvel Gillespie 246-2368 254-0135 (Luncheon) Margaret Fink 289-0188 Harold and Patricia Gay Moore (Evening) Maxine Harrington 297-ll86 (Geology Seminars) Catherine Evenson 654-2636 Library: Esther Kennedy 287-3091 ' ' Betty Turner 246-3192 Telephone n Past Presidents Panel Jean L. -
A POST IMPACT VOLCANISM SCENARIO for the FORMATION of the OLIVINE-RICH UNIT in the REGION of NILI FOSSAE, MARS. L. Mandon1, C. Q
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 1473.pdf A POST IMPACT VOLCANISM SCENARIO FOR THE FORMATION OF THE OLIVINE - RICH UNIT IN THE REGION OF NILI FOSSAE, MARS. L. Mandon 1 , C. Quantin 1 , P. Thollot 1 , L. Lozac’h 1 , N. Mangold 2 , G. Dromart 1 , P. Beck 3 , E. Dehouck 1 , S. Breton 1 , C. Millot 1 . 1 Laboratoire de Géologie de Lyon Terre, Planètes, Environnement , Université de Lyon, France. 2 Laboratoire de Planétologie et Géodynamique , Université de Nantes, France. 3 Institut de Planétologie et d'Astrophysique de Gre- noble , Université Grenoble Alpes, France. lucia.ma ndon@univ - lyon1.fr. Introduction: The Nili Fossae region exhibits the gets using MarsSI. We used HRSC DTMs computed largest Martian exposures of olivine - rich materials, as by the Fr eie Universitaet Berlin and DLR Berlin . deduced from orbital near - infrared and thermal spec- Strikes and dips measurements were performed using troscopy [1, 2] . Several hypotheses have been pro- the ArcGIS extension LayerTools [7]. Finally, we posed to explain the origin of a widespread olivine - rich performed crater size analyses on both small (~1 km²) formati on in the region: (1) these materials might be and wide (~900 km²) olivine - rich areas. Using the crustal rocks excavated by the giant impact leading to Craterstats software [8], we compared size distribu- the formation of Isidis Planitia [2], a 1200 km wide tions to isochrons generated by the Ivanov production impact basin east of Nili Fossae. (2) They could result function to estimate a surface age [9]. from mafic effusive lava flows occurring befo re [3] or Results: At HiRISE resolution, the unit appears after [4] the giant impact. -
Lafayette - 800 Grams Nakhlite
Lafayette - 800 grams Nakhlite Figure 1. Photograph showing fine ablation features Figure 2. Photograph of bottom surface of Lafayette of fusion crust on Lafayette meteorite. Sample is meteorite. Photograph from Field Museum Natural shaped like a truncated cone. This is a view of the top History, Chicago, number 62918. of the cone. Sample is 4-5 centimeters across. Photo- graph from Field Museum Natural History, Chicago, number 62913. Introduction According to Graham et al. (1985), “a mass of about 800 grams was noticed by Farrington in 1931 in the geological collections in Purdue University in Lafayette Indiana.” It was first described by Nininger (1935) and Mason (1962). Lafayette is very similar to the Nakhla and Governador Valadares meteorites, but apparently distinct from them (Berkley et al. 1980). Lafayette is a single stone with a fusion crust showing Figure 3. Side view of Lafayette. Photograph from well-developed flow features from ablation in the Field Museum Natural History, Chicago, number Earth’s atmosphere (figures 1,2,3). The specimen is 62917. shaped like a rounded cone with a blunt bottom end. It was apparently oriented during entry into the Earth’s that the water released during stepwise heating of atmosphere. Note that the fine ablation features seen Lafayette was enriched in deuterium. The alteration on Lafayette have not been reported on any of the assemblages in Lafayette continue to be an active field Nakhla specimens. of research, because it has been shown that the alteration in Lafayette occurred on Mars. Karlsson et al. (1992) found that Lafayette contained the most extra-terrestrial water of any Martian Lafayette is 1.32 b.y. -
Module 7 Igneous Rocks IGNEOUS ROCKS
Module 7 Igneous Rocks IGNEOUS ROCKS ▪ Igneous Rocks form by crystallization of molten rock material IGNEOUS ROCKS ▪ Igneous Rocks form by crystallization of molten rock material ▪ Molten rock material below Earth’s surface is called magma ▪ Molten rock material erupted above Earth’s surface is called lava ▪ The name changes because the composition of the molten material changes as it is erupted due to escape of volatile gases Rocks Cycle Consolidation Crystallization Rock Forming Minerals 1200ºC Olivine High Ca-rich Pyroxene Ca-Na-rich Amphibole Intermediate Na-Ca-rich Continuous branch Continuous Discontinuous branch Discontinuous Biotite Na-rich Plagioclase feldspar of liquid increases liquid of 2 Temperature decreases Temperature SiO Low K-feldspar Muscovite Quartz 700ºC BOWEN’S REACTION SERIES Rock Forming Minerals Olivine Ca-rich Pyroxene Ca-Na-rich Amphibole Na-Ca-rich Continuous branch Continuous Discontinuous branch Discontinuous Biotite Na-rich Plagioclase feldspar K-feldspar Muscovite Quartz BOWEN’S REACTION SERIES Rock Forming Minerals High Temperature Mineral Suite Olivine • Isolated Tetrahedra Structure • Iron, magnesium, silicon, oxygen • Bowen’s Discontinuous Series Augite • Single Chain Structure (Pyroxene) • Iron, magnesium, calcium, silicon, aluminium, oxygen • Bowen’s Discontinuos Series Calcium Feldspar • Framework Silicate Structure (Plagioclase) • Calcium, silicon, aluminium, oxygen • Bowen’s Continuous Series Rock Forming Minerals Intermediate Temperature Mineral Suite Hornblende • Double Chain Structure (Amphibole) -
Cr-Rich Spinels As Petrogenetic Indicators
American Mineralogist, Volume 73, pages 741-753, 1988 Cr-rich spinels as petrogeneticindicators: MORB-type lavas from the Lamont seamountchain, easternPacific J,trrns F. Ar.r-.c.N* Department of Geological Sciences,Northwestern University, Evanston, Illinois 60201, U.S.A. Rrcn.qno O. Sacr Department of Earth and Atmospheric Sciences,Purdue University, West Lafayette, Indiana 47907, U.S.A. Roonv Bxttzt Department of Geological Sciences,Northwestern University, Evanston, Illinois 60201, U.S.A. Ansrucr The composition and morphology of Cr-rich spinels in MORBs reflect and record pre- eruptive petrogeneticevents such as magma-chamberrecharge, fractionation, and magma mixing. In this paper we examine Cr-rich spinels in MORB-type lavas erupted from the near-ridge Lamont seamountsand from the adjacent East Pacific Rise crest at 10'N. The spinels studied are exclusively from quickly quenchedglassy to spherulitic flow margins. The host lavas are depleted [(LalSm)" < 0.57] and relatively primitive [Me/(Me + Fe2*) to 0.71, Cr to 460 ppml, with the most primitive samplesapproaching the composition of liquids in equilibrium with mantle peridotite. The spinelscover a wide range in Al and Cr contents,with spinel Cr/(Cr + Al) ranging from 0.20 to 0.54 for the entire suite. As in other depleted MORBs, TiO, and calculated FerO. contents in the spinels are low (0. 16- 0.85 and 5.5-9.2 wto/0,respectively). Contents of Al, Mg, and Fe of groundmassspinels strongly correlate with host-glasscomposition, but spinel Cr content shows little correla- tion with host-glassCr content. Castingof spinel compositions in terms of Mg-Fe'z*spinel- host liquid exchangeequilibria and in terms of the compositionally related crystallochem- ical effectson this exchangeshows that for a given lava suite derived from similar parental lavas, spinel Crl(Cr + Al) increasesand Mg/@g + Fe2+)decreases with the amount of Fe enrichment, Al depletion, and extent of fractionation [as representedby the normative ratio Diop/(Ol + Diop)l of the liquids in which they equilibrated. -
Volcanism on Mars
Author's personal copy Chapter 41 Volcanism on Mars James R. Zimbelman Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA William Brent Garry and Jacob Elvin Bleacher Sciences and Exploration Directorate, Code 600, NASA Goddard Space Flight Center, Greenbelt, MD, USA David A. Crown Planetary Science Institute, Tucson, AZ, USA Chapter Outline 1. Introduction 717 7. Volcanic Plains 724 2. Background 718 8. Medusae Fossae Formation 725 3. Large Central Volcanoes 720 9. Compositional Constraints 726 4. Paterae and Tholi 721 10. Volcanic History of Mars 727 5. Hellas Highland Volcanoes 722 11. Future Studies 728 6. Small Constructs 723 Further Reading 728 GLOSSARY shield volcano A broad volcanic construct consisting of a multitude of individual lava flows. Flank slopes are typically w5, or less AMAZONIAN The youngest geologic time period on Mars identi- than half as steep as the flanks on a typical composite volcano. fied through geologic mapping of superposition relations and the SNC meteorites A group of igneous meteorites that originated on areal density of impact craters. Mars, as indicated by a relatively young age for most of these caldera An irregular collapse feature formed over the evacuated meteorites, but most importantly because gases trapped within magma chamber within a volcano, which includes the potential glassy parts of the meteorite are identical to the atmosphere of for a significant role for explosive volcanism. Mars. The abbreviation is derived from the names of the three central volcano Edifice created by the emplacement of volcanic meteorites that define major subdivisions identified within the materials from a centralized source vent rather than from along a group: S, Shergotty; N, Nakhla; C, Chassigny. -
Expedition 330 Core Descriptions, Site U1374 Thin Sections
Site U1374 thin sections U1374A-3R-1-W 114_116 Proc. IODP THIN SECTION: 330-U1374A-3R-1-W 114_116-BILLET 114-SLIDE 114 Piece No: Unit:I OBSERVER:THIN SECTION:SLIDE 114 Site U1374 core descriptions ROCK NAME: moderately olivine-phyric basalt clast WHERE SAMPLED: clast type 2 GRAINSIZE: fine grained TEXTURE: moderately phyric | Volume 330 PRIMARY PERCENT REL. VOL. SIZE(mm) VESICLE VESICLE MINERALOGY ORIGINAL REPLACED min. max. mode. MORPHOLOGY SPHERICITY Infilling [%] COMMENTS PHENOCRYSTS 10 olivine 5 20 8 1.2 skeletal incomplete dome face (iddingsite); "skeletal olivine" & "euhedral to subhedral" MICROPHENOCRYST plagioclase 0.01 0.3 0.4 laths[330] just 2 grains olivine 4 40 0.9 0.4 skeletal incomplete dome face (iddingsite); "skeletal olivine" & "euhedral to subhedral" augite 1 0.3 0.3 subhedral sector-zoning titanaugite VESICLES 3 0.1 1.8 0.6 low[330] 100 filled by calcite GROUNDMASS 87 opaque mineral 5 olivine 4 95 0.09 0.06 subhedral to replaced by iddingsite (hematite?) anhedral[330] glass 68 100 palagonite augite 1 anhedral plagioclase 9 0.2 0.01 microlite[330] SECONDARY SIZE(mm) MINERALOGY min. max. mode. REPLACING/FILLING COMMENTS calcite vesicle STRUCTURE no structure in groundmass COMMENTS SUMMARY DESCRIPTION Thin sections 1 U1374A-3R-2-W 7_9 Proc. IODP THIN SECTION: 330-U1374A-3R-2-W 7_9-BILLET 115-SLIDE 115 Piece No: Unit:I OBSERVER:THIN SECTION:SLIDE 115 Site U1374 core descriptions ROCK NAME: highly olivine-phyric basalt clast WHERE SAMPLED: CLAST TYPE 1 GRAINSIZE: fine grained TEXTURE: highly phyric & glomeroporphyritic | Volume 330 PRIMARY PERCENT REL. -
IDENTIFYING TWO DISTINCT OLIVINE COMPOSITIONS in TYRRHENA TERRA and LIBYA MONTES, MARS. M. D. Lane1, J. L. Bishop2, D. Loizeau3, D
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2550.pdf IDENTIFYING TWO DISTINCT OLIVINE COMPOSITIONS IN TYRRHENA TERRA AND LIBYA MONTES, MARS. M. D. Lane1, J. L. Bishop2, D. Loizeau3, D. Tirsch4, L. L. Tornabene5, L. Sacks5, C. Viviano6, J. R. C. Voigt7 1Fibernetics LLC, Lititz, PA ([email protected]), 2Carl Sagan Center, SETI Institute, Mountain View, CA, 3IAS, Université-Sud, Orsay, France, 4Institute of Planetary Research, German Aerospace Center (DLR), Ber- lin, Germany, 5Dept. of Earth Sciences, Institute for Earth and Space Exploration, University of Western Ontario, London, Canada, 6Johns Hopkins University Applied Physics Lab (JHUAPL), Laurel, MD, 7Lunar and Planetary Labora- tory, University of Arizona, Tucson, AZ. Introduction: Olivine is present across Terra Tyr- rhena (TT) and in the southern rim of the Isidis basin Figure 2. Ther- in the Libya Montes (LM) region. Using both near-IR mal emissivity Compact Reconnaissance Imaging Spectrometer for Mars spectra of syn- (CRISM) and mid-IR Thermal Emission Spectrometer thetic Mg-Fe oli- (TES) data to characterize our study site (Fig. 1), the vines. The dots strongest olivine signatures across TT are identified in represent the flec- isolated crater floor deposits, while the olivine in the tion points for LM area is associated with a stratigraphic unit con- each composi- sistent with an airfall ash deposit [2]. Using mid-IR tion. These points spectral indices developed from synthetic olivine data and the bands to [3] for 13 different olivine compositions in the forster- each side migrate ite (Fo100) to fayalite (Fo0) solid solution series (Fig. with changes in 2), specific Mg-Fe olivine compositions were deter- chemistry. -
Aqueous Alteration of Yamato 000749 Based on Multi-Probe Microscopic Observation
Aqueous alteration of Yamato 000749 based on multi-probe microscopic observation Naoki Shiraishi1, Hiroki Suga1,2, Masaaki Miyahara1, Takuji Ohigashi3, Yuichi Inagaki3, Akira Yamaguchi4, Naotaka Tomioka 5, Yu Kodama6, and Eiji Ohtani7 1Hiroshima University, 2The University of Tokyo, 3UVSOR synchrotron facility, 4NIPR, 5Kochi Institute for Core Sample 6 7 Research, JAMSTEC, Marine Works Japan, Tohoku University Motivation Based on the results of Mars explorations and researches of Martian meteorites for many years, there is a high possibility that liquid water had existed extensively on Mars for a long time (Sekine, 2012). Martian meteorite is one of the important clues for restoring the past Martian surface environment that cannot be unveiled by Mars surface survey alone. It is expected that a member of Martian meteorites, nakhlites have evidences for a rock-fluid reaction occurred on Mars. One of the representative evidence for the rock-fluid reaction is “iddingsite”, which is an alteration texture formed in and around olivine grains in nakhlites. Many kinds of secondary minerals occur in the iddingsite through the rock-fluid reaction. The mineral assemblages, chemical compositions and chemical species of the secondary minerals depend on the varied parameters such as temperature and pH of the fluid. Suga et al. (2017) described the secondary minerals in the iddingsite of nakhlites Yamato (Y) 000593. Another Martian meteorites, Yamato (Y) 000749 is also a member of Yamato 00 nakhlites like Y 000593, containing abundant iddingsite. Based on Cohen et al. (2017), Y 000749 was located at the lower portion of the same nakhlites source compared to Y 000593. It is likely that these nakhlites have different mode of alteration even in the same source. -
Alkalic Rocks of Iron Hill Gunnison County, Colorado
If yon do not need this publication after it has served your purpose, please return it to the Geological Survey, using the official mailing label at the end UNITED STATES DEPARTMENT OF THE INTERIOR ALKALIC ROCKS OF IRON HILL GUNNISON COUNTY, COLORADO GEOLOGICAL SURVEY PROFESSIONAL PAPER 197-A UNITED STATES DEPARTMENT OF THE INTERIOR Harold L. Ickes, Secretary GEOLOGICAL SURVEY W. C. Mendenhall, Director Professional Paper 197-A ALKALIC ROCKS OF IRON HILL GUNNISON COUNTY, COLORADO BY ESPER S. LARSEN Shorter contributions to general geology, 1941 (Pages 1-64) UNITED STATES GOVERNMENT PRINTING OFFICE WASHINGTON : 1942 For sale by the Superintendent of Documents, Washington, D. C. ......... Price 40 cents CONTENTS Page Preface, by G. F. Loughlin_________________________ v Other dike rocks_______________-____________________ 29 Abstract____"_--__-___--__________________________ 1 Augite syenite and shonkinite ____.__--___--__--__ 29 Introduction. ______________________________________ 1 Olivine gabbro. ________________________________ 30 Location and topography. _______________________ 1 Carbonate veins_________----__---------__--_---___- 31 Field work and acknowledgments.________________ 2 Character __ __________________________________ 31 Geology of the surrounding area__________________ 2 Origin _______ _ ____ _ __ _.. __ __. ___ .__. 31 Age of the Iron Hill stock_____________________ 2 Hydrothermal processes- ______--_-___-_---_--__-___- 31 General geology of the Iron Hill stock _____________ 3 The hydrothermal products. _____________________