Lafayette - 800 Grams Nakhlite
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Wind Measurements of Martian Dust Devils from Hirise
EPSC Abstracts Vol. 6, EPSC-DPS2011-570, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Wind Measurements of Martian Dust Devils from HiRISE D. S. Choi (1) and C. M. Dundas (2) (1) Department of Planetary Sciences, University of Arizona, Tucson, AZ, USA ([email protected]) (2) United States Geological Survey, Flagstaff, AZ, USA Abstract servation crosses an active feature such as a dust devil, changes in the active feature are apparent from the We report direct measurements of the winds within three separate views. Treating the dust clouds as pas- Martian dust devils from HiRISE imagery. The cen- sive tracers of motion then allows for the direct mea- tral color swath of the HiRISE instrument observes surement of wind velocities. the surface by using separate CCDs and color filters in We utilize measurements from manual (hand-eye) rapid cadence. Active features, such as a dust devil, tracking of the clouds through image blinking, as appear in motion when serendipitously captured by well as automated correlation methods [9]. Typically, this region of the instrument. Our measurements re- manual measurements are more successful than au- veal clear circulation within the vortices, and that the tomated measurements. The relatively diffuse dust majority of overall wind magnitude within a dust devil clouds, combined with the static background terrain, 1 is between 10 and 30 m s− . cause the automated software to incorrectly report the movement as stationary. Successful automated results were obtained from images with more substantial dust 1. Introduction clouds and relatively featureless background terrain. Direct measurements of the winds within a Martian dust devil [1] are challenging to obtain. -
Cosmic-Ray-Exposure Ages Martian Meteorites Million Years
Introduction to MMC 2012 someone keeps adding pieces as you go along (see my Introduction 2006). Most Martian meteorites are mafic As of the end of 2012, we now know of about 65 basalts. That is, they have an abundance of Fe and different meteorites from Mars with a total weight about Mg, are low in Si and Al and have a texture of 120 kilograms. Some fell as showers (e.g. Nakhla, intergrown minerals typical of terrestrial basalts (the Tissint), and some can be paired by common lithology, tradition has been to call them “shergottites”, after the age and fall location, but it is more instructive to first sample recognized as such). Some often have an consider how they are grouped by “launch pairs”. If abundance of large olivine crystals (so called olivine- you add the terrestrial age to the cosmic exposure age phyric). Others have an abundance of both high- and (CRE) you get the time when the meteorite was low-Ca pyroxene, with poikilitic textures and were launched off of Mars by impact. Since only rather large originally called “lherzolitic shergottites”. But it has impacts would do this, there must be a finite number now been recognized that there is a more fundamental of such impacts – hence grouping of samples. and better way to describe these rocks (Irving 2012). Now that we have such a large number of samples, it Figure 1 shows a crude summary of CRE that have is time to understand what we have and infer what we been determined for Martian meteorites. Note that can about Mars. -
The Analysis of Life Struggle in Andy Weir's
THE ANALYSIS OF LIFE STRUGGLE IN ANDY WEIR‘S NOVEL THE MARTIAN A THESIS BY ALEMINA BR KABAN REG. NO. 140721012 DEPARTMENT OF ENGLISH FACULTY OF CULTURAL STUDIES UNIVERSITY OF SUMATERA UTARA MEDAN 2018 UNIVERSITAS SUMATERA UTARA THE ANALYSIS OF LIFE STRUGGLE IN ANDY WEIR‘S NOVEL THE MARTIAN A THESIS BY ALEMINA BR KABAN REG. NO. 140721012 SUPERVISOR CO-SUPERVISOR Drs. Parlindungan Purba,M.Hum. Riko Andika Pohan, S.S., M.Hum. NIP.1963021619 89031003001 NIP. 1984060920150410010016026 Submitted to Faculty of Cultural Studies University of Sumatera Utara Medan in partial fulfilment of the requirements for the degree of Sarjana Sastra from Department of English DEPARTMENT OF ENGLISH FACULTY OF CULTURAL STUDIES UNIVERSITY OF SUMATERA UTARA MEDAN 2018 UNIVERSITAS SUMATERA UTARA Approved by the Department of English, Faculty of Cultural Studies University of Sumatera Utara (USU) Medan as thesis for The Sarjana Sastra Examination. Head, Secretary, Prof. T.Silvana Sinar,Dipl.TEFL,MA.,Ph.D Rahmadsyah Rangkuti, M.A. Ph.D. NIP. 19571117 198303 2 002 NIP. 19750209 200812 1 002 UNIVERSITAS SUMATERA UTARA Accepted by the Board of Examiners in partial fulfillment of requirements for the degree of Sarjana Sastra from the Department of English, Faculty of Cultural Studies University of Sumatera Utara, Medan. The examination is held in Department of English Faculty of Cultural Studies University of Sumatera Utara on July 6th, 2018 Dean of Faculty of Cultural Studies University of Sumatera Utara Dr. Budi Agustono, M.S. NIP.19600805 198703 1 001 Board of Examiners Rahmadsyah Rangkuti, M.A., Ph.D __________________ Drs. Parlindungan Purba, M.Hum. -
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. -
An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger Depauw University
DePauw University Scholarly and Creative Work from DePauw University Student research Student Work 2015 An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger DePauw University Follow this and additional works at: http://scholarship.depauw.edu/studentresearch Part of the Economics Commons, and the The unS and the Solar System Commons Recommended Citation Knappenberger, Clayton, "An Economic Analysis of Mars Exploration and Colonization" (2015). Student research. Paper 28. This Thesis is brought to you for free and open access by the Student Work at Scholarly and Creative Work from DePauw University. It has been accepted for inclusion in Student research by an authorized administrator of Scholarly and Creative Work from DePauw University. For more information, please contact [email protected]. An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger 2015 Sponsored by: Dr. Villinski Committee: Dr. Barreto and Dr. Brown Contents I. Why colonize Mars? ............................................................................................................................ 2 II. Can We Colonize Mars? .................................................................................................................... 11 III. What would it look like? ............................................................................................................... 16 A. National Program ......................................................................................................................... -
Sequestration of Martian CO2 by Mineral Carbonation
ARTICLE Received 11 Jun 2013 | Accepted 24 Sep 2013 | Published 22 Oct 2013 DOI: 10.1038/ncomms3662 OPEN Sequestration of Martian CO2 by mineral carbonation Tim Tomkinson1, Martin R. Lee2, Darren F. Mark1 & Caroline L. Smith3,4,5 Carbonation is the water-mediated replacement of silicate minerals, such as olivine, by carbonate, and is commonplace in the Earth’s crust. This reaction can remove significant quantities of CO2 from the atmosphere and store it over geological timescales. Here we present the first direct evidence for CO2 sequestration and storage on Mars by mineral carbonation. Electron beam imaging and analysis show that olivine and a plagioclase feldspar- rich mesostasis in the Lafayette meteorite have been replaced by carbonate. The susceptibility of olivine to replacement was enhanced by the presence of smectite veins along which CO2-rich fluids gained access to grain interiors. Lafayette was partially carbonated during the Amazonian, when liquid water was available intermittently and atmospheric CO2 concentrations were close to their present-day values. Earlier in Mars’ history, when the planet had a much thicker atmosphere and an active hydrosphere, carbonation is likely to have been an effective mechanism for sequestration of CO2. 1 Scottish Universities Environmental Research Centre, Rankine Avenue, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK. 2 School of Geographical and Earth Sciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow G12 8QQ, UK. 3 Department of Earth Sciences, Natural History Museum, Cromwell Road, London SW7 5BD, UK. 4 ESA ESTEC, Keplerlaan 1, 200 AG Noordwijk, The Netherlands. 5 UK Space Agency, Atlas Building, Harwell Oxford, Didcot, Oxfordshire OX11 0QX, UK. -
Secondary Minerals in the Nakhlite Meteorite Yamato 000593: Distinguishing Martian from Terrestrial Alteration Products
46th Lunar and Planetary Science Conference (2015) 2010.pdf SECONDARY MINERALS IN THE NAKHLITE METEORITE YAMATO 000593: DISTINGUISHING MARTIAN FROM TERRESTRIAL ALTERATION PRODUCTS. H. Breton1, M. R. Lee1, and D. F. Mark2 1School of Geographical and Earth Sciences, University of Glasgow, University Ave, Glasgow, Lanarkshire G12 8QQ, UK ([email protected]), 2Scottish Universities Environmental Research Center, Rankine Ave, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK Introduction: The nakhlites are olivine-bearing Methods: A thin section of Y-000593 was studied clinopyroxenites that formed in a Martian lava flow or using a Carl Zeiss Sigma field-emission SEM equipped shallow intrusion 1.3 Ga ago [1, 2]. They are scientifi- with an Oxford Instruments Aztec microanalysis sys- cally extremely valuable because they interacted with tem at the University of Glasgow. Chemical and miner- water-bearing fluids on Mars [3]. Fluid-rock interac- alogical identification within the secondary minerals tions led to the precipitation of secondary minerals, were obtained through backscattered electron (BSE) many of which are hydrous. The secondary minerals imaging and energy dispersive spectroscopy (EDS) consist in a mixture of poorly crystalline smectitic ma- mapping and quantitative microanalysis. terial and Fe-oxide, collectively called “iddingsite”, but Results and discussions: Y-000593 is an unbrec- also carbonate and sulphate [4]. The proportion, chem- ciated cumulate rock whose mineralogy is similar to istry and habit of the secondary minerals vary between other nakhlites: a predominance of augite and minor members of the Nakhlite group, which is thought to olivine phenocrysts surrounded by a microcrystalline reflect compositional variation of the fluid within the mesostasis [9]. -
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. -
The Physical Properties of Asteroids
University of Central Florida STARS Electronic Theses and Dissertations, 2020- 2020 The Physical Properties of Asteroids Leos Pohl University of Central Florida Part of the Physics Commons Find similar works at: https://stars.library.ucf.edu/etd2020 University of Central Florida Libraries http://library.ucf.edu This Doctoral Dissertation (Open Access) is brought to you for free and open access by STARS. It has been accepted for inclusion in Electronic Theses and Dissertations, 2020- by an authorized administrator of STARS. For more information, please contact [email protected]. STARS Citation Pohl, Leos, "The Physical Properties of Asteroids" (2020). Electronic Theses and Dissertations, 2020-. 269. https://stars.library.ucf.edu/etd2020/269 THE PHYSICAL PROPERTIES OF ASTEROIDS by LEOS POHL B.S. Charles University, Prague, 2011 M.S. Charles University, Prague, 2014 A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics in the Department of Physics in the College of Sciences at the University of Central Florida Orlando, Florida Summer Term 2020 Major Professor: Daniel T. Britt © 2020 LEOS POHL ii ABSTRACT The Small Bodies of the Solar System are leftover material from the formation of planets. Compared with planetary bodies, they have undergone relatively little transfor- mation. Embedded in their physical properties, are clues to the conditions and processes that took place since the condensation of the Solar Nebula. Furthermore, asteroids are sources of raw materials that have become a topic of significant interest. In this dis- sertation, I explore several properties of asteroid material: strength of asteroids, their shielding properties against high energetic particles and their water content. -
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. -
PETROLOGY and GEOCHEMISTRY of NAKHLITE MIL 03346: a NEW MARTIAN METEORITE from ANTARCTICA M. Anand ([email protected]), C.T. Williams, S.S
Lunar and Planetary Science XXXVI (2005) 1639.pdf PETROLOGY AND GEOCHEMISTRY OF NAKHLITE MIL 03346: A NEW MARTIAN METEORITE FROM ANTARCTICA M. Anand ([email protected]), C.T. Williams, S.S. Russell, G. Jones, S. James, and M.M. Grady Department of Mineralogy, The Natural History Museum, Cromwell Road, London, SW7 5BD, UK MIL 03346 is a newly discovered meteorite origin. In textural appearance, this rocks appears most from Miller Range in Antarctica, which belongs to the similar to the nakhlite group nakhlite, of Martian NWA 817 meteorites [3]. [1]. It is an The unbrecciated, modal medium- mineralogy grained of MIL olivine- 03346 is bearing dominated clinopy- by cumulus roxenite with pyroxenes a cumulate (~70%) fol- texture, lowed by similar to the glassy 6 other pre- mesostasis viously (~25%). known Olivine is nakhlites. only present in minor amounts and no crystalline pla- This is only gioclase was observed in our sample. However, the the 2nd composition of the glassy mesostasis is most closely nakhlite in Antarctic collections, the other being Ya- mato 000593 and its pairs. The Meteorite Working Group (MWG) allocated us two polished sections (MIL 03346,102 & MIL 03346,116), and 1 g rock chip (MIL 03346,37) for carrying out petrological and geochemi- cal investigations. Petrography and Mineral Chemistry: The rock displays a cumulate texture (Fig. 1) consisting predominantly of zoned matched by a Na-K-rich-feldspar. The majority of the euhedral pyroxene grains show extensive zoning from core to clinopyroxene the rim. The outer 10-20 µm zones of pyroxene grains (0.5-1 mm display several generations of growth (sometimes up to long) and 4), clearly evident in back scatter electron images. -
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. _____________________