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Planetary Geology (Part of Chapter 9): General Processes Affecting the Terrestrial Planets (And the Moon)
Planetary Geology (part of Chapter 9): General Processes Affecting the Terrestrial Planets (and the Moon) Many geological features on planetary surfaces are shaped by processes within the planet’s interior. The interior of a terrestrial world is divided into three layers of differing densities and chemical compositions: core of high-density metal, mantle of moderate- density rock, and crust of low-density rock. Although we see molten rock (lava) coming out of the Earth, only a thin layer near the top of the mantle is partially molten. However, the solid rock within planets can flow like a liquid over periods of millions of years at speeds of around 1 cm per year. The crust and very top part of the mantle do not deform or flow easily, they are called the lithosphere. The thickness of a planet’s lithosphere affects how easily it can be fractured and rearranged into mountains and valleys, and how easily lava can be erupted onto the surface. Interior heat causes geological activity. Terrestrial worlds were heated during their formation due to accretion and differentiation, and are still heated today by radioactive decay. They are slowly cooling down, with heat moving up through the mantle by convection, up through the crust by conduction, and radiating out to space. Larger planets retain heat for longer than smaller planets, so larger planets are more geologically active. If a rapidly-rotating planet contains a layer of electrically conducting fluid, such as a liquid metal core, then it will have a magnetic field. This magnetic field can protect its atmosphere from the solar wind. -
Planetary Geology GEOLOGY 307 Spring 2018 Tuesday & Thursday 9:30 -10:50 A.M
Planetary Geology GEOLOGY 307 Spring 2018 Tuesday & Thursday 9:30 -10:50 a.m. C. M. Bailey Office- McStreet Hall 215 x12445 [email protected] Preamble Space, the Final Frontier! Although the Earth provides a rich tapestry for geologists, other planetary bodies in our Solar System are equally worthy of study. Many of the same processes that operate on Earth modify these worlds, but each planet is unique in many respects. Planetary bodies also contain a record of the solar system’s history. The goals of this course include a better understanding of the processes that operate on distant worlds, gaining insight into how the Solar System has changed through time, and thinking about the future opportunties in planetary science. This class will not simply be a tour of the planets, nor will it attempt to answer all the questions normally dealt with in Astronomy and Cosmology courses. We will start from observations and use a judicious amount of mathematics, physics, and chemistry to achieve our goals. At semester’s end we hope you will have developed an understanding of the Solar System, a sense for the new and exciting discoveries in planetary science, as well as an appreciation of the important questions still to be answered. Week Dates Topic Readings 1 Jan. 18 Planetary Geology Introduced WHOOPS! Ch. 1 2 Jan. 23, 25 Planetary Geology Introduced Ch. 1 The Universe: matter, stars, planets, and life- oh my! 3 Jan. 30, Feb. 1 Celestial Mechanics Ch. 2 Ch. 5, pg. 64-67 4 Feb. 6, 8 Solar System Formation Meteorites are Mighty Important 5 Feb. -
Effects of Water on Seismic Wave Velocities in the Upper Mantle Terior. Therefore, If One Understands the Relation Between Water
No. 2] Proc. Japan Acad., 71, Ser. B (1995) 61 Effects of Water on Seismic Wave Velocities in the Upper Mantle By Shun-ichiro KARATO Department of Geology and Geophysics, University of Minnesota, Minneapolis, MN 55455 (Communicated by Yoshibumi ToMODA,M. J. A., Feb. 13, 1995) Abstract : Possible roles of water to affect seismic wave velocities in the upper mantle of the Earth are examined based on mineral physics observations. Three mechanisms are considered: (i) direct effects through the change in bond strength due to the presence of water, (ii) effects due to the enhanced anelastic relaxation and (iii) effects due to the change in preferred orientation of minerals. It is concluded that the first direct mechanism yields negligibly small effects for a reasonable range of water content in the upper mantle, but the latter two indirect effects involving the motion of crystalline defects can be significant. The enhanced anelastic relaxation will significantly (several %) reduce the seismic wave velocities. Based on the laboratory observations on dislocation mobility in olivine, a possible change in the dominant slip direction in olivine from [100] to [001] and a resultant change in seismic anisotropy is suggested at high water fugacities. Changes in seismic wave velocities due to water will be important, particularly in the wedge mantle above subducting oceanic lithosphere where water content is likely to be large. Key words : Water; seismic wave velocity; upper mantle; anelasticity; seismic anisotropy. Introduction. Water plays important roles in the terior. Therefore, if one understands the relation melting processes and hence resultant chemical evolu- between water content and seismic wave velocities, tion of the solid Earth. -
Mars Field Geology, Biology, and Paleontology Workshop, Summary
MARS FIELD GEOLOGY, BIOLOGY, AND PALEONTOLOGY WORKSHOP: SUMMARY AND RECOMMENDATIONS November 18–19, 1998 Space Center Houston, Houston, Texas LPI Contribution No. 968 MARS FIELD GEOLOGY, BIOLOGY, AND PALEONTOLOGY WORKSHOP: SUMMARY AND RECOMMENDATIONS November 18–19, 1998 Space Center Houston Edited by Nancy Ann Budden Lunar and Planetary Institute Sponsored by Lunar and Planetary Institute National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Contribution No. 968 Compiled in 1999 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautcis and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This volume may be cited as Budden N. A., ed. (1999) Mars Field Geology, Biology, and Paleontology Workshop: Summary and Recommendations. LPI Contribution No. 968, Lunar and Planetary Institute, Houston. 80 pp. This volume is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Phone: 281-486-2172 Fax: 281-486-2186 E-mail: [email protected] Mail order requestors will be invoiced for the cost of shipping and handling. _________________ Cover: Mars test suit subject and field geologist Dean Eppler overlooking Meteor Crater, Arizona, in Mark III Mars EVA suit. PREFACE In November 1998 the Lunar and Planetary Institute, under the sponsorship of the NASA/HEDS (Human Exploration and Development of Space) Enterprise, held a workshop to explore the objectives, desired capabilities, and operational requirements for the first human exploration of Mars. -
Burlington House Fire Safety Information
William Smith Meeting 2015 (Part 2) 5 November 2015 200 Years and Beyond: The future of geological mapping Contents Page 2 Acknowledgements Page 3 Conference Programme Page 5 Speaker Biographies and Abstracts Page 29 Poster Abstracts Page 40 Burlington House Fire Safety Information Page 41 Ground Floor Plan of the Geological Society, Burlington House @geolsoc #wsmith15 #williamsmith200 Page 1 William Smith Meeting 2015 (Part 2) 5 November 2015 200 Years and Beyond: The future of geological mapping WELCOME FROM THE CONVENORS In 1815 William Smith published the first edition of his Geological Map of England and Wales. Smith’s map made a seminal contribution to the understanding of the ground beneath our feet and, by showing the location of coal, iron ore, clays and other raw materials, helped fuel the industrial revolution. Two hundred years on, the demands for spatial knowledge about our geological environment and its resources and hazards have become ever more diverse and pressing. Nevertheless, many of the motivators, approaches and principles pioneered by William Smith survive in the geological maps, models and information systems of today. The History of Geology Group and the British Geological Survey have worked together to convene two William Smith meetings at the Geological Society in 2015 to celebrate this landmark anniversary. The first, very successful meeting in April 2015, convened by HOGG, chronicled the history and development of the geological map from its earliest beginnings to the digital maps of today. This second meeting, convened by the BGS, looks to the future of geological mapping, and to the grand challenges for geoscience that will motivate the ‘William Smiths’ of tomorrow. -
Geomagnetism and Paleomagnetism Membership Survey
Membership Survey: Geomagnetism and Paleomagnetism (GP) Section What is your primary section or focus group affiliation? Response Answer Options Response Count Percent Geomagnetism and Paleomagnetism (GP) Section 71.0% 363 Study of Earths Deep Interior (SEDI) Focus Group 4.5% 23 Planetary Sciences (P) Section 2.0% 10 Tectonophysics (T) Section 7.0% 36 Near-Surface Geophysics (NS) Focus Group 5.1% 26 Other (please specify) 10.4% 53 answered question 511 skipped question 0 What is your primary section or focus group affiliation? Geomagnetism and Paleomagnetism (GP) Section Study of Earths Deep Interior (SEDI) Focus Group Planetary Sciences (P) Section Tectonophysics (T) Section Near-Surface Geophysics (NS) Focus Group Other (please specify) Membership Survey: Geomagnetism and Paleomagnetism (GP) Section What (if any) is your secondary affiliation? Response Answer Options Response Count Percent Geomagnetism and Paleomagntism Section 24.0% 121 Study of Earth's Deep Interior Focus Group 15.0% 76 Planetary Sciences Section 13.7% 69 Tetonophysics Section 22.8% 115 Near-Surface Geophysics Focus Group 10.7% 54 None 24.2% 122 answered question 505 skipped question 6 What (if any) is your secondary affiliation? 30.0% 25.0% 20.0% 15.0% 10.0% 5.0% 0.0% None and Section Section Geophysics FocusGroup Near-Surface Planetary Focus Group DeepInterior Tetonophysics Geomagnetism Paleomagntism Study of Earth's Study of SciencesSection Membership Survey: Geomagnetism and Paleomagnetism (GP) Section List additional secondary affiliations (if any): Answer Options -
GEOLOGY THEME STUDY Page 1
NATIONAL HISTORIC LANDMARKS Dr. Harry A. Butowsky GEOLOGY THEME STUDY Page 1 Geology National Historic Landmark Theme Study (Draft 1990) Introduction by Dr. Harry A. Butowsky Historian, History Division National Park Service, Washington, DC The Geology National Historic Landmark Theme Study represents the second phase of the National Park Service's thematic study of the history of American science. Phase one of this study, Astronomy and Astrophysics: A National Historic Landmark Theme Study was completed in l989. Subsequent phases of the science theme study will include the disciplines of biology, chemistry, mathematics, physics and other related sciences. The Science Theme Study is being completed by the National Historic Landmarks Survey of the National Park Service in compliance with the requirements of the Historic Sites Act of l935. The Historic Sites Act established "a national policy to preserve for public use historic sites, buildings and objects of national significance for the inspiration and benefit of the American people." Under the terms of the Act, the service is required to survey, study, protect, preserve, maintain, or operate nationally significant historic buildings, sites & objects. The National Historic Landmarks Survey of the National Park Service is charged with the responsibility of identifying America's nationally significant historic property. The survey meets this obligation through a comprehensive process involving thematic study of the facets of American History. In recent years, the survey has completed National Historic Landmark theme studies on topics as diverse as the American space program, World War II in the Pacific, the US Constitution, recreation in the United States and architecture in the National Parks. -
The Upper Mantle and Transition Zone
The Upper Mantle and Transition Zone Daniel J. Frost* DOI: 10.2113/GSELEMENTS.4.3.171 he upper mantle is the source of almost all magmas. It contains major body wave velocity structure, such as PREM (preliminary reference transitions in rheological and thermal behaviour that control the character Earth model) (e.g. Dziewonski and Tof plate tectonics and the style of mantle dynamics. Essential parameters Anderson 1981). in any model to describe these phenomena are the mantle’s compositional The transition zone, between 410 and thermal structure. Most samples of the mantle come from the lithosphere. and 660 km, is an excellent region Although the composition of the underlying asthenospheric mantle can be to perform such a comparison estimated, this is made difficult by the fact that this part of the mantle partially because it is free of the complex thermal and chemical structure melts and differentiates before samples ever reach the surface. The composition imparted on the shallow mantle by and conditions in the mantle at depths significantly below the lithosphere must the lithosphere and melting be interpreted from geophysical observations combined with experimental processes. It contains a number of seismic discontinuities—sharp jumps data on mineral and rock properties. Fortunately, the transition zone, which in seismic velocity, that are gener- extends from approximately 410 to 660 km, has a number of characteristic ally accepted to arise from mineral globally observed seismic properties that should ultimately place essential phase transformations (Agee 1998). These discontinuities have certain constraints on the compositional and thermal state of the mantle. features that correlate directly with characteristics of the mineral trans- KEYWORDS: seismic discontinuity, phase transformation, pyrolite, wadsleyite, ringwoodite formations, such as the proportions of the transforming minerals and the temperature at the discontinu- INTRODUCTION ity. -
Joint Mineral Physics and Seismic Wave Traveltime Analysis of Upper Mantle Temperature
Joint mineral physics and seismic wave traveltime analysis of upper mantle temperature Jeroen Ritsema1, Paul Cupillard2, Benoit Tauzin3, Wenbo Xu1, Lars Stixrude4, Carolina Lithgow-Bertelloni4 1Department of Geological Sciences, University of Michigan, Ann Arbor, Michigan 48109, USA 2Seismological Laboratory, University of California–Berkeley, Berkeley, California 94720, USA 3Ecole et Observatoire des Sciences de la Terre, Institut de Physique du Globe de Strasbourg, 67084 Strasbourg, France 4Department of Earth Sciences, University College London, London WC1E 6BT, UK ABSTRACT CONVERTED WAVE TRAVELTIMES We employ a new thermodynamic method for self-consistent Teleseismic P wave conversions, denoted as Pds, propagate as com- computation of compositional and thermal effects on phase transition pressional (P) waves through the deep mantle and convert to shear (S) depths, density, and seismic velocities. Using these profi les, we compare waves at an upper mantle discontinuity at depth d beneath the seismom- theoretical and observed differential traveltimes between P410s and eter. The phases P410s and P660s, for example, are waves that have P (T410) and between P600s and P410s (T660–410) that are affected only by converted from P to S at the 410 km and the 660 km transitions, respec- seismic structure in the upper mantle. The anticorrelation between T410 tively (Fig. 1). and T660–410 suggests that variations in T410 and T660–410 of ~8 s are due to Our data are recorded traveltime differences between the phases lateral temperature variations in the upper mantle transition zone of P410s and P (T410) and between P660s and P410s (T660–410). T410 and ~400 K. If the mantle is a mechanical mixture of basaltic and harzbur- T660–410 are unaffected by imprecise earthquake locations and lower mantle gitic components, our traveltime data suggest that the mantle has an hetero geneity. -
Chapter 9 Planetary Geology: Agenda Ad Hoc Rover Update
Chapter 9 Planetary Geology: Agenda Earth and the Other Terrestrial Worlds • Announce: – Part 2 of Projects due – Read Ch. 11 for Tuesday • Ad hoc, ex post facto • Rover Update • Ch. 9—Planetary Geology • Lab: Parallax or Waves on a String Rover Update Ad Hoc • More than 1000 Martian days • From Wikipedia: – Ad hoc is a Latin phrase which means "for this [purpose]." It generally signifies a solution that has been designed for a specific problem, is non-generalizable and can not be adapted to other purposes. – Ex post facto : from the Latin for "from something done afterward" 1 9.1 Connecting Planetary Interiors and What are terrestrial planets like Surfaces on the inside? • Our goals for learning • What are terrestrial planets like on the inside? • What causes geological activity? • Why do some planetary interiors create magnetic fields? Seismic Waves Earth’s Interior • Vibrations • Core: Highest that travel density; nickel through and iron Earth’s • Mantle: Moderate interior tell us density; silicon, what Earth is oxygen, etc. like on the • Crust: Lowest inside density; granite, basalt, etc. Terrestrial Planet Interiors Differentiation • Gravity pulls high-density material to center • Lower-density material rises to surface • Material ends up • Applying what we have learned about Earth’s separated by interior to other planets tells us what their interiors density are probably like 2 Lithosphere Strength of Rock • A planet’s outer • Rock stretches when layer of cool, rigid pulled slowly but rock is called the breaks when pulled lithosphere -
Planetary Geology: Goals, Future Directions, and Recommendations
NASA Conference Publication 3005 Planetary Geology: Goals, Future Directions, and Recommendations Proceedings of a workshop held at Arizona State University Tempe, Arizona January 1987 NASA Conference Publication 3005 Planetary Geology: Goals, Future Directions, and Recommendations NASA Office of Space Science and Applications Washington, D. C. Proceedings of a workshop held at Arizona State University Tempe, Arizona January 1987 National Aeronautics and Space Administration Scientific and Technical Information Division Preface This report gives results of a workshop on planetary geology held in January, 1987, at Arizona State University at the request of Dr. David Scott, Discipline Scientist, Planetary Geology and Geophysics, NASA. In addition to reviews by the workshop members, it was reviewed by the Planetary Geology and Geophysics Working Group and incorporated comments from Dr. James Underwood, current Discipline Scientist for the program. R. Greeley, January 1988 TABLE OF CONTENTS Page 1.0 Executive Summary ............................................................................... 1 2.0 Introduction ........................................................................................ 3 3.0 Workshop Conclusions ........................................................................... 5 3.1 Planetary geology studies are in transition from a descriptive phase to prcxess-oriented research .................................................. 5 3.2 Quantitative techniques can be applied to existing data. but there is a need for -
Magnetic Properties of Single and Multi-Domain Magnetite Under Pressures from 0 to 6
GEOPHYSICAL RESEARCH LETTERS, VOL. 31, L10612, doi:10.1029/2004GL019844, 2004 Magnetic properties of single and multi--domain magnetite under pressures from 0 to 6 GPa Stuart A. Gilder,1 Maxime LeGoff,1 Jean-Claude Chervin,2 and Jean Peyronneau1 Received 1 April 2004; revised 13 April 2004; accepted 21 April 2004; published 26 May 2004. [1] Using novel experimental methods, we measured the [3] How stress influences magnetic remanence also acquisition of isothermal remanent magnetization, direct depends on the size and shape of the substance. The field demagnetization, and alternating field demagnetization magnetizations of single domain (SD) and multi-domain of multi-domain (MD) and single domain (SD) magnetite (MD) magnetite grains react differently to imposed stresses. under hydrostatic pressures to 6 GPa. We find that Stress may cause the net spontaneous moment in a SD grain the saturation remanence of MD magnetite increases to reorient to a new position depending on the angle 2.8 times over initial, non-compressed values by 6 GPa, between the stress and magnetic easy axis direction, the while its remanent coercivity remains relatively constant. grain’s shape, etc. [Hodych, 1977]. The individual domains For SD magnetite, remanent coercivity and saturation in a multi-domain grain grow or shrink to compensate for remanence vary little from 0 to 1 GPa, increase markedly the stress, which modify the grain’s magnetic intensity and from 1 to 3 GPa, then plateau above 3 GPa. These new direction [Bogdanov and Vlasov, 1966]. In sum, two pro-