DOCSLIB.ORG

Buscando a Vida Fora Da Terra: Marte

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Buscando a Vida Fora Da Terra: Marte AGA 0316 Buscando a vida fora da Terra: Marte Why Mars is important for Astrobiology? • Relative proximity – first planet where we can realistically test in loco for biological potential and life • Mars is in many ways similar to Earth. Rocky, terrestrial planet in the inner part of the Solar system with an atmosphere. Yet it is also very different. • Therefore if life is found there it would be a very strong argument in favor of life being an ubiquitous phenomenum in the galaxy History of Martian “Civilization” • In 1784 William Herschel (famous for the discovery of Uranus) claimed that Mars has an atmosphere and is therefore probably inhabited. • Giovanni Schiaparelli claimed to see a network of 79 linear channels (canali) in 1877 • Percival Lowell opened Lowell Observatory in Flagstaff, Arizona in 1894. (claimed to see 200 canals) • Lowell suggested that canals were built by an ancient martian civilization. Giovanni Schiaparelli William Herschel Percival Lowell • In 1965 “Mariner 4” spacecraft send a few dozen good pictures of the Martian surface – no evidence for intelligent life. Mars is in fact a cold and dry planet! 6 7 9 1960’s 1970’s 1990’s 2000’s Pathfinder & Sojourner Spirit + Opportunity Mars Fact Sheet Parameter Value Units Diameter 6787 km Average Distance From the Sun 1.524 AU EARTH’S Atm Average Temperature 210 K (-81 F) CO2 0.04% 3 Mean Density 3.94 g/cm N2 78,1% Rotational Period 24.6229 hours Ar 0.93% Mean Atmospheric Pressure 0.007 bars H2O 0 – 4 % Surface Gravity 3.63 m/s2 Tilt of Axis 25.2 degrees Orbit period 687 days Atmospheric Components Element Symbol Percentage Carbon Dioxide CO2 95.32 Nitrogen N2 2.7 Argon Ar 1.6 Water H2O 0.03 Earth-Mars Similarities • Position in the Solar system – Martian orbit is 1.5 A.U.; Earth’s is 1 A.U. but Neptune’s is 30 A.U. • Similar bulk chemical composition – Si-rich crust and mantle and Fe-rich core • Size – Mars is only twice smaller than Earth by radius • Atmosphere has greenhouse gas (CO2) and some amount of nitrogen • Volcanoes • Similar rotation rate – 24.6 hours • Plenty of water (frozen; subsurface?) Earth-Mars Differences • Earth has a global-scale plate tectonics, Mars does not. • Earth has global oceans at its surface, Mars has not • Martian atmosphere (0.007 bar) is much thinner than Earth’s ( 1 bar) • Earth has an intrinsic global magnetic field, Mars has not Problems for life on the Martian surface • Cold (average temperature ~220K); not many known organisms on Earth can grow under these temperatures • Thin atmosphere – open liquid water is unstable • Very small amount of oxygen – no terrestrial-like animal life • Very little ozone – no UV protection • No magnetic field – poor protection from the cosmic rays Problem Water does not have a liquid phase under current low Martian pressures. Ice sublimates to water vapor directly. However, there are strong evidence that liquid water was present in the past on the Martian surface Evidence for liquid water on the Martian surface • Geomorphological evidence: 1) Look for features that are similar in appearance to terrestrial water-formed features 2) Degradation (weathering) of the ancient impact craters (erosion) • Mineralogical evidence MARTIAN SOIL FLOOD TRACES ON CRATER WALLS Valley network on the ancient terrain of the martian surface. Notice that valleys converge downstream. Individual valleys are about a kilometer across. Flood channel occurring on a relatively young surface. Note the well-defined margins of the channel indicating confined flow and the streamlined, tear-drop- shaped islands where erosional remnants have been left behind obstacles. Even the youngest features on Mars appear to show evidence for liquid water. Gullies have been identified on the walls of canyons, channels and impact craters. Most likely were formed by seepage of water from within the crust. Martian Meteorites • Meteorites which originated from Mars – impactors hit Martian surface and some small fraction of the ejected rock can arrive on Earth • Although > 31,000 meteorites were found, only 34 have been identified as Martian meteorites How do we know that some meteorites are from Mars? • Age. Almost all martian meteorites are relatively young volcanic rocks (180-1300 Myr) with composition similar to terrestrial basalts • Oxygen isotopes are distinct (16O, 17O, 18O) from terrestrial rocks and group all 34 meteorites together • The isotopic composition of gases trapped in the meteorites is almost identical to the Martian atmosphere (comparison with Viking measurements). The oxygen isotopic compositions of rocks from Earth, Mars, and the asteroid Vesta, the largest asteroid that melted, define three parallel lines on this plot of 17O / 16O vs. 18O / 16O. The lines are parallel because on each body the oxygen isotopes were separated according to their masses, when the rocks formed. Classification of Martian meteorites (SNC: shergottite, nakhlite, and chassigny ) • 1 billion tones of Martian rocks crashed into Earth ! • Shergottite (Shergotty meteorite from India, 1865) - 25 • Nakhlites (Nakhla meteorite from Egypt, 1911) - 7 • Chassignites (Chassigny meteorite from France, 1815) - 2 Evidence of water in SNCs • Carbonate minerals. Liquid water flows through fractures in rocks and dissolved CO2 can be precipitated. • Hydrated minerals with martian D/H Electron Microscope image of clay and carbonate (siderite) vein in Lafayette section. ol olivine. ALH84001 • Shergottite which containes structures that were considered to be the fossilized remains of bacteria-like lifeforms. Viking Mission • Two orbiters, two landers • Two landers landed on the opposite sides of Mars in 1976 • The Viking 1 Lander touched down at 22.7° N latitude and 48.2° W longitude • The Viking 2 Lander touched down at 48.3° N latitude and 226° W longitude Viking Results • Viking carried 4 instruments designed to detect any sign of biology: • The Labeled Release (LR), Gas Exchange (GEX), and Pyrolytic Release (PR) experiments, all designed to detect existent life on Mars. • The Gas Chromatograph/Mass Spectrometer (GC/MS) was capable of detecting organics at a level of a few parts per billion (ppb) Pyrolytic Release experiment (PR) • Martian soil was put in a chamber and exposed to CO2 and CO mixture 14 • CO2 and CO were labeled with C • Idea: “If biota were in the soil it would incorporate some CO2 or CO and convert it to organic material” • Heat the soil → break organic material → look for release of 14C Gas exchange (GEX) • Martian soil was put into a chamber and mixed with plenty of different nutrients (amino acids, glucose, salts, vitamins ..) • Look for H2, N2, O2, CH4, CO2,and Ar, Kr (for calibration) released from the soil (bacteria?). Labeled release (LR) • Martian soil was put into a chamber and mixed with nutrients (glucose and sulfate) enriched in 14C and 35S • Look for gas release enriched in 14C and/or 35S (released by bacteria?) LR - TSM Biology Package • What the Viking biology experiments found: Expected Response for Expected heat- Response for heat- sterilized Response for sample w/ sterilized Control Experiments sample Biology control Response GEX oxygen emitted oxygen emitted oxygen emitted none LR labeled gas emitted labeled gas emitted none none PR carbon detected carbon detected carbon detected none • The GC/MS detected no organics above the 10 ppb level What we expected • This was surprising as each year, 2.4 x 108 grams of reduced (organic) carbon is delivered to Mars each year by meteors, which should have been detectable by the Viking GC/MS. • Even without life, organics were expected. • With regolith mixing to a depth of 1 km, organics should be present at about 500 ppb. Viking Conclusions • It was concluded that the Martian surface is rich in UV-produced oxides and superoxides at the ppm level, which destroy any organics present. • This conclusion reconciles the apparently contradictory results of the other Viking life experiments. • However . .(cf. OH-based life) The Atacama desert • Gonzáles et al. use the oxidizing soil and hyper- arid conditions in the Atacama Desert as an analog for the Martian surface. • They analyzed the Atacaman soil with a GC/MS to compare with Viking results. What they found • In the most arid sample, both formic acid and benzene were found when pyrolized at 750ºC. • However, Viking pyrolysis temperatures maxed out at 500ºC, so . • Using the Viking pyrolysis temperature, the formic acid detected was reduced by a factor of 4 and there was no benzene detected at all. formic acid benzene • All three Viking’s experiments assumed that we would be able to culture potentially present martian organisms. • Even on Earth only 1 in 100 organisms can be cultures at best. • Viking results do not rule out the possibility of life in the martian soil. • Is there another way to discover martian life? Arguments in favor of “life on Mars” from ALH84001 • Presence of polycyclic aromatic hydrocarbons (PAHs). PAHs can form as decay products of microorganisms • Presence of magnetite crystals whose structure is very similar to crystals produced by some terrestrial bacteria • Ovoid structures in carbonate globules similar to terrestrial microbes PAHs Carbonate globules (50-250 m) Ovoid structures (20-100 nm) Magnetite crystalls (Fe3O4) History of ALH84001 • Age ~4.5 Gyr old (rock crystallized) • Carbonate globules are ~3.9 Gyr old • Rock remained on the surface of Mars until 16 Myr ago when it was ejected • Meteorite was captured by Earth 13,000 years ago and fell into Antarctica • Covered with snow and ice until 700 years ago • Recovered in 1984 Summary of ALH84001 • Most of the morphological fossils are thought to be too small to represent living organisms • Most of the organics are terrestrial in origin and the martian organics could have been produced by nonbiological processes • The magnetite grains are thought to represent the strongest evidence for life • McKay et al.
Load more

Recommended publications
  • EPSC2017-260, 2017 European Planetary Science Congress 2017 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2017
    EPSC Abstracts Vol. 11, EPSC2017-260, 2017 European Planetary Science Congress 2017 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2017 Formation of recurring slope lineae on Mars by rarefied gas-triggered granular flows F. Schmidt (1), F. Andrieu (1), F. Costard (1), M. Kocifaj (2,3) and A. G. Meresescu (1) (1) GEOPS, Univ. Paris-Sud, CNRS, Université Paris-Saclay, Rue du Belvédère, Bât. 504-509, 91405 Orsay, France (2) ICA, Slovak Academy of Sciences, Dubravska Road 9, 845 03 Bratislava, Slovak Republic (3) Faculty of Mathematics, Physics, and Informatics, Comenius University, Mlynska dolina, 842 48 Bratislava, Slovak Republic (frederic.schmidt@@u-psud.fr) Abstract been excluded near the crater rim [3]. In addition, the actual amount of atmospheric water required to re- Recurring Slope Linae or RSL are seasonal dark charge the RSL's source each year seems not features appearing when the soil reaches its sufficient. The precise thermal calculations using maximum temperature. They appear on various THEMIS measurement instrument show no evidence slopes at the equator of Mars, in orientation of liquid water [6] and there is no direct evidence of depending on the season. Today, liquid water related liquid water from CRISM, but only indirect detection processes have been promoted, such as deliquescence [4]. of salts. Nevertheless external atmospheric source of water is inconsistent with the observations. Internal We propose here a re-interpretation of the RSL source is also very unlikely. We take into features and a new process to explain the RSL consideration here the force occurring when the sun activity without involving any volatiles.
    [Show full text]
  • Active Gullies and Mass Wasting on Equatorial Mars
    EPSC Abstracts Vol. 12, EPSC2018-457-1, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Active Gullies and Mass Wasting on Equatorial Mars Alfred S. McEwen (1), Melissa F. Thomas (1), Colin M. Dundas (2) (1) LPL, University of Arizona, Tucson, Arizona, USA, (2) USGS, Flagstaff, Arizona, USA Abstract Previously-reported equatorial topographic changes include slumps on the colluvial fans below active Mid- to high-latitude gully activity has been directly RSL sites in Garni Crater [5] and in Juventae Chasma observed at hundreds of locations on Mars [1]. Here [7]. These slumps all occurred near the coldest time we describe equatorial locations (25 latitude) with of year for these locations, Ls 0-120, which is gully-like or other topographic changes in before- opposite to the seasonality of RSL. and-after images from HiRISE. This activity is concentrated in sulfate-rich sedimentary units, which We are in the process of searching HiKER pairs over places constraints on the age and mechanical steep equatorial slopes, as well as acquiring new properties of these deposits. Hydrated sulfates may HiKER images. From the effort to date we have found that equatorial changes are most common in be the largest equatorial reservoir of H2O on Mars, and their friability makes them more attractive for in- sedimentary layers that may be rich is sulfates situ resource utilization (ISRU). according to mapping by orbital spectrometers [8], and have concentrated our search in these regions. 1. Introduction The most impressive changes we have found are on Mid- to high-latitude gully activity can be explained bright layered mounds in Ganges Chasma.
    [Show full text]
  • And Leanne Brown Eat Well on $4/Day
    EAT WELL ON $4/DAY GOOD AND CHEAP LEANNE BROWN Salad ...............................................42 Broiled Eggplant Salad ....................................43 Kale Salad ..................................................... 44 NEW Ever-Popular Potato Salad ........................46 Introduction ....................5 NEW Spicy Panzanella......................................49 Text, recipes, and most photographs and A Note on $4/Day ...........................................6 Cold (and Spicy?) Asian Noodles .....................50 design by Leanne Brown, in fulfillment My Philosophy ................................................7 Taco Salad ......................................................52 of a final project for a master’s degree in Tips for Eating and Shopping Well ...................8 Beet and Chickpea Salad ................................53 First, I’d like to thank my husband, Food Studies at New York University. Pantry Basics .................................................12 Broccoli Apple Salad .......................................54 Dan. Without him this book would not NEW Charred Summer Salad ............................55 exist. Thank you also to my wonderful This book is distributed under a family and friends, who believed in this Creative Commons Attribution- idea before anyone else. And thank you NonCommercial ShareAlike 4.0 license. Breakfast ..............................14 to everyone who has taken the time to For more information, visit Tomato Scrambled Eggs .................................15 Snacks,
    [Show full text]
  • Modeling Floods in Athabasca Valles, Mars, Using CTX Stereo Topography
    Recurring Slope Lineae (RSL) near candidate Mars 2020 landing sites Alfred McEwen, Colin Dundas, Matt Chojnacki, James Wray August 2015 NOTE ADDED BY JPL WEBMASTER: This content has not been approved or adopted by, NASA, JPL, or the California Institute of Technology. This document is being made available for information purposes only, and any views and opinions expressed herein do not necessarily state or reflect those of NASA, JPL, or the California Institute of Technology. • Dark flows on steep, low-albedo slopes, What are RSL? typically associated with bedrock and small gullies. – Few meters wide, hundreds of meters long. – Not found on most steep rocky slopes. • Recur annually at nearly the same location in multiple Mars years. • Grow incrementally over a period of several months, then fade. • Fans have unique spectral properties (Ojha et al. 2013) • RSL in the southern mid-latitudes generally grow from late spring RSL Seasonality through mid-summer. – Concentrated on equator-facing slopes. • RSL in Valles Marineris often follow the sun: growth occurs on south-facing slopes in southern summer and north-facing slopes in northern summer. • RSL in N hemisphere grow mainly in very early spring (Ls 0) • Associated with peak diurnal temperatures usually >250 K. • Strongly suggests that RSL are driven by a volatile. Leading explanation is flow of (salty) liquid water, but source is unknown, and no direct detection of water. Garni crater on floor of Melas Chasm Slumping associated with RSL seen in Garni crater and 2 sites in Juventae Chasm Very Rapid Initial Lengthening Max >20 m/sol Schaefer et al., 2015, LPSC Very early (Ls <194) start of RSL activity in Hale crater • Need to check temperatures, maybe <250 K Acidalia RSL exactly match from year-to-year.
    [Show full text]
  • Report 2017 Research, Education and Public Outreach Activity Report 2017 Research, Education and Public Outreach
    Activity Report 2017 Research, Education and Public Outreach Activity Report 2017 Research, Education and Public Outreach Nathalie A. Cabrol Director, Carl Sagan Center, Pamela Harman, Acting Director, Center for Education Rebecca McDonald Director, Center for Outreach Bill Diamond President & CEO The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Activity Report 2017 Research, Education and Public Outreach TABLE OF CONTENTS Peer-reviewed publications 10 Conferences: Abstracts & Proceedings 18 Technical Reports & Data Releases 29 Outreach, Media Coverage, Web Stories & Interviews 31 Invited Talks (Professional & Public) 39 Highlights, Significant Events & Activities 46 Fieldwork 52 Honors & Awards 54 Missions, Observations & Strategic Planning 56 Acknowledgements 60 The SETI Institute: 189 N Bernardo Avenue Suite 200, Mountain View, CA 94043. Phone: (650) 961-6633 Activity Report 2017 Research, Education and Public Outreach FROM THE SETI INSTITUTE President and CEO Dear friends, The scientists, educators and outreach professionals of the SETI Institute had yet another banner year of productivity in 2017. We are delighted to present our 2nd annual report, cataloging the research and education programs of the Institute, as well as the myriad of mainstream media stories about our people and our work. Among the highlights from this year’s report are 147 peer-reviewed articles in scientific journals, 225 conference proceedings and abstracts, 172 media stories and interviews, and 177 invited talks.
    [Show full text]
  • Försvarsmaktens Årsredovisning 2006 Huvuddokument
    Försvarsmakten Årsredovisning 2006 FOTO: FÖRSVARETS BILDBYRÅ / ANDREAS KARLSSON 107 85 Stockholm. Telefon: 08-788 75 00. Fax: 08-788 77 78. Webbplats: www.mil.se 2007-02-20 23 386: 63006 Försvarsmaktens ÅRSREDOVISNING 2006 Resultatredovisning, resultaträkning, balansräkning, an- slagsredovisning, finansieringsanalys och noter 2007-02-20 23 386: 63006 INNEHÅLLSFÖRTECKNING ÖVERBEFÄLHAVARENS KOMMENTAR.....................................................................................................1 OPERATIV FÖRMÅGA M.M............................................................................................................................ 4 UTGÅNGSPUNKTER FÖR REDOVISNINGEN............................................................................................................ 4 FÖRSVARSMAKTENS OPERATIVA FÖRMÅGA ........................................................................................................ 4 INSATSORGANISATIONEN .................................................................................................................................... 7 RESULTATREDOVISNING .............................................................................................................................. 9 LÄGET I GRUNDORGANISATIONEN....................................................................................................................... 9 UTBILDNING, PLANERING M.M. ......................................................................................................................... 11 MATERIEL, ANLÄGGNINGAR
    [Show full text]
  • Modern Mars' Geomorphological Activity
    Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, Matthew Chojnacki, Susan Conway, Colin Dundas, Candice Hansen, Alfred Mcewen, et al. To cite this version: Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, et al.. Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity. Geomorphology, Elsevier, 2021, 380, pp.107627. 10.1016/j.geomorph.2021.107627. hal-03186543 HAL Id: hal-03186543 https://hal.archives-ouvertes.fr/hal-03186543 Submitted on 31 Mar 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. 1 Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity 2 3 Authors: Serina Diniega1,*, Ali M. Bramson2, Bonnie Buratti1, Peter Buhler3, Devon M. Burr4, 4 Matthew Chojnacki3, Susan J. Conway5, Colin M. Dundas6, Candice J. Hansen3, Alfred S. 5 McEwen7, Mathieu G. A. Lapôtre8, Joseph Levy9, Lauren Mc Keown10, Sylvain Piqueux1, 6 Ganna Portyankina11, Christy Swann12, Timothy N. Titus6,
    [Show full text]
  • Program to Technical Sessions Thirtieth Lunar and Planetary
    LUNAR AND PLANETARY SCIENCE CoNFERENCE MARCH 15-19, 1999 HOUSTON, TEXAS SPONSORED BY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION L UNAR AND PLANETARY INSTITUTE NASA JOHNSON SPACE CENTER Program to Technical Sessions THIRTIETH LUNAR AND PLANETARY SCIENCE CONFERENCE March 15-19, 1999 Houston, Texas Sponsored By National Aeronautics and Space Administration Lunar and Planetary Institute NASA Johnson Space Center Program Committee Carl Agee, Co-Chair, NASA Johnson Space Center David Black, Co-Chair, Lunar and Planetary Institute Cone! Alexander, Carnegie Institution of Washington Carlton Allen, Lockheed Martin Donald Bogard, NASA Johnson Space Center Harold Connolly, Jr., California Institute ofTechnology Cassandra Coombs, College of Charleston John Grant, NASA Headquarters Friedrich Horz, NASA Johnson Space Center Michael Kelley, Rensselaer Polytechnic Institute Walter Kiefer, Lunar and Planetary Institute David Kring, University of Arizona Renu Malhotra, Lunar and Planetary Institute Timothy Parker, Jet Propulsion Laboratory Frans Rietmeijer, University of New Mexico Graham Ryder, Lunar and Planetary Institute Susan Sakimoto, NASA Goddard Space Flight Center Paul Spudis, Lunar and Planetary Institute Meenakshi Wadhwa, Field Museum of Natural History, Chicago LPI ROOM C 145 FIRST FLOOR Robert R. Gilruth Recreation Facility Building 207 ROOM B ,.. SECOND FLOOR Robert R. Gilruth Recreation Facility Building 207 CONFERENCE INFORMATION Registration-LPI Open House A combination Registration/Open House will be held Sunday, March 14, 1999, from 5:00p.m. until 8:00p.m. at the Lunar and Planetary Institute. Registration will continue in the Gilruth Center, Monday through Thursday, 8:00a.m. to 5:00p.m. A shuttle bus will be available to transport participants between the LPI and local hotels Sunday evening from 4:45 p.m.
    [Show full text]
  • Charles R. Reeve Millbum, N
    30,32,34,35,36,37 and 38 Mechanic St., Newark The Oldest W holesale I V.EGBERT tCO. Supply House In Newark IRVINGTON (1920) DIRECTORY 801 PFEFFEB PILKINGTON — Eleanor M elk PruInsCo bds 512 S Grove Pilkington George H carp h 130 Park pi — Frank W shipper bds 512 S Grove — George H Jr elk Town Hall bds 130 Park *V — Harry H salesman bds 512 S Grove Pi Pfeifer Barbara Mrs h 71 Franklin ter Pillsbury John T h 1281 Clinton av — Elizabeth wid Otto h 78 Fern av Pinch Emma E wid Charles W rem to Newark > — Frank rem to Newark Pinkinson Fannie Mrs h 172 2 2 d — Fred shipping elk h 51 Washington ar — John lab bds 172 22d — Herman saloon 874 Clinton av h do Pinney William H elk h 1172 Clinton av — John ironwkr h 255 Ellis av Pins Joseph brewer h 344 17th av 3 — John W plumber bds 78 Fern a v Pinto Michele far h 521 Union av — Julius steamfitter bds 251 Ellis av Pisalsky Helen Mrs h 737 Springfield av H — Lillian jeweler bds 78 Fern a v — Herbert carp bds 737 Springfield av — Louisa Mrs h 251 Ellis av — Herman mech bds 737 Springfield av Pfeiffer Carl waiter h 24 20th av Pischel Ernest h 370 21st — Christian F h 42 Rich —-William A butcher h 447 14th av in — George h 186 Ellis av Pischottel Louis treas Reliable Tool Co 33 ( 6 — Henrietta wid Cort bds 311 21st Ellis av h 33 Alpine — Henry h 46 Florence av Pitrosky Maryan baker h 30 Arverne ter e — Henry Jr letter carrier bds 46 Florence av Pittinger John L h 303 21st — John H toolmkr h 380 21st — Mary S bds 19 Howard Pfeil A Leslie bds 518 Nye av — Theodore F leather cutter h 19 Howard — Charles
    [Show full text]
  • African Studies in French for the Elementary Grades: Phase II of a Twinned Classroom Approach to the Teaching of French in the Elementary Grades
    DOCUMENT RESUME ED 066 993 48 FL 003 581 AUTHOR Jonas, Sister Ruth TITLE African studies in French for the Elementary Grades: Phase II of a Twinned Classroom Approach to the Teaching of French in the Elementary Grades. Volume II, Tapescripts and Essays. INSTITUTION College of Mount St. Joseph-on-the-Ohio, Ohio. SPONS AGENCY Institute of International Studies (DHEW/OE), Washington, D.C. BUREAU NO BR-9-7743 PUB DATE Sep 72 CONTRACT OEC-0-9-097743-4408-014 NOTE 274p.; Final Report EDRS PRICE MF-S0.65 HC-$9.87 DESCRIPTORS *African Culture; Audiolingual Methods; Audiovisual Instruction; Cross Cultural Studies; *Cultural Education; Educational Experiments; Elementary Education; *Fles; Fles Programs; *French; *Instructional Materials; Language Instruction; Language Programs; Language Skills; Mossi; Second Language Learning; Student Evaluation; Student Motivation; Teaching Methods ABSTRACT This experiment examines a new psychological approach . to foreign language study at the elementary school level. A principal objective is to determine the nature and importance of second language learning motivation in monolingual societies devoid of the daily living example of the target language and culture. A five-year French language sequence, consisting of an exchange of 1,200 correlated slides and tapes of the participants in the program and student- and teacher-made instructional materials, is described in the report. The text contains 67 units of materials corresponding to slides of Voltan and American culture. An appendix discussing how the French acquired Upper Volta is included. For the companion document see FL 003 582. (EL) U.S. DIPAITMINI OF KWH, 10110110N & WINN OFFICI OF EDUCATION IMSDOCUMNIHMUMIRIODUUDMILYMRKMMFROMMI HISONOROMMUNNOMMM611 POWSWVIMAROPMMM re\ STATED DO NM MUMMY REPRESENT OFFICIAL OFFICI Of MAHN CT POSITION ORPOLICY.
    [Show full text]
  • Quantitative Mapping and Evaluation of Wet and Dry Formation Mechanisms of Recurring Slope Lineae (Rsl) in Garni Crater, Valles Marineris, Mars
    Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6098.pdf QUANTITATIVE MAPPING AND EVALUATION OF WET AND DRY FORMATION MECHANISMS OF RECURRING SLOPE LINEAE (RSL) IN GARNI CRATER, VALLES MARINERIS, MARS. D. E. Stillman1, B. D. Bue2, K. L. Wagstaff2, K.M. Primm1, T. I. Michaels3, and R. E. Grimm1, 1Dept. of Space Studies, Southwest Research Institute, 1050 Walnut St #300, Boulder, CO 80302 ([email protected]), 2Jet Propul- sion Laboratory, California Institute of Technology, 3SETI Institute Overview: RSL are narrow (0.5–5 m) low-albedo MY31 and MY32 and were even more significant in features that incrementally lengthen down steep slopes MY33 and MY34 before the dust storm. during warm seasons. As hundreds of RSL can exist 2) After the MY34 dust storm, RSL formed on eve- within a single HiRISE image, we developed the Map- ry intercardinal and cardinal slope-facing direction. ping and Automated Analysis of RSL (MAARSL) MAARSL data from MY31 and MY32 suggests that system to reduce the effort involved in manually map- RSL would have normally formed on only three of the ping each RSL in each image. MAARSL analyzes a set eight slope orientations. Additionally, numerous RSL of orthorectified HiRISE images and Digital Elevation tributaries are detected. Map (DEM) to detect candidate RSL, compute de- 3) MAARSL results demonstrated that RSL scriptive statistics, and characterize changes over time. lengthening and fading occur concurrently on the same The results of MAARSL are then used to evaluate dry slopes and even on the same RSL (Fig. 1&2). and wet RSL formation mechanisms.
    [Show full text]
  • The Good, the Bad, and the Ugly of the Aquifer Flow and Recharge Mechanism for Recurring Slope Lineae
    Late Mars Workshop 2018 (LPI Contrib. No. 2088) 5012.pdf THE GOOD, THE BAD, AND THE UGLY OF THE AQUIFER FLOW AND RECHARGE MECHANISM FOR RECURRING SLOPE LINEAE. D. E. Stillman and R. E. Grimm, Dept. of Space Studies, Southwest Re- search Institute, 1050 Walnut St #300, Boulder, CO 80302 ([email protected]) Introduction: Recurring slope lineae (RSL) are RSL lengthen [7]. This suggests that the water source narrow (0.5–5 m) low-albedo features that emanate of the faded RSL stopped and the RSL faded as its from bedrock (or immediately downslope of bedrock) surficial water content evaporated/sublimated away. [1-3]. They incrementally advance down steep slopes Meanwhile, the water source of the lengthening RSL during warm seasons over tens to hundreds of sols [4]. continued, allowing it to lengthen. RSL then stop lengthening and fade as the temperature Hydrated salt spectral signatures have been detect- cools. Lastly, RSL darken and fade each Mars year. ed at four confirmed RSL sites [8], suggesting the We have identified 100 confirmed RSL sites that presence of water at RSL sites. Note that only salt hy- possess (1) incremental lengthening, (2) fading, and (3) drates were detected, thus this does not guarantee that annual recurrence. Additionally, 653 candidate (that all liquid water was present. three characteristics) RSL sites have also been docu- Hydrological modeling shows that the general in- mented. Candidate and confirmed RSL sites exist on cremental lengthening rates match water flowing via dust-poor, steep slopes within a latitude range of 42°N gravity and capillary suction in a sandy porous medi- to 53°S [4].
    [Show full text]