NOBLE GASES IN GEOCHEMISTRY AND COSMOCHEMISTRY

Size: px
Start display at page:

Download "NOBLE GASES IN GEOCHEMISTRY AND COSMOCHEMISTRY"

Transcription

1 3m V IImm 41 NOBLE GASES IN GEOCHEMISTRY AND COSMOCHEMISTRY Editors:, '...., Donald Porcelli Chris J. Ballentine RainerWieler Department of Earth Sciences University of Oxford Oxford, United Kingdom Department of Earth Sciences University of Manchester Manchester, United Kingdom Institute for Isotope Geology and Mineral Resources ETH-Zurich Zurich, Switzerland Front cover: Courtesy Frontispiece: Cartoon by Elisabeth Wilding Series Editors: Jodi J. Rosso & Paul H. Ribbe E 'CIHIIEMIICAIL S CHETTY " HETTY. ff AMllRII'CA

2 Table of Contents Noble Gases in Geochemistry and Cosmochemistry 1 An Overview of Noble Gas Geochemistry and Cosmochemistry Donald Porcelli, Chris J. Ballentine, Rainer Wieler INTRODUCTION 1 NOBLE GAS MASS SPECTROMETRY 2 THE ATMOSPHERIC STANDARD 2 PRODUCTION OF NOBLE GAS ISOTOPES 4 BEHAVIOR OF THE NOBLE GASES 5 Water, natural gas, and oil partitioning 6 Silicate melt solubilities 6 Crystal-melt partitioning 6 Iron-silicate partitioning 6 Adsorption 6 Diffusion 7 Atmosphere losses 7 NOBLE GASES IN COSMOCHEMICAL AND GEOCHEMICAL STUDIES 7 Noble gases in cosmochemistry 8 Noble gases in the mantle 10 Noble gases in surface reservoirs 11 Noble gases and geochronology 13 END NOTE 14 ACKNOWLEDGMENTS.. 14 REFERENCES 14 APPENDIX Noble Gases in the Solar System Rainer Wieler INTRODUCTION 21 ANALYTICAL TECHNIQUES 21 THE SUN 23 Solar noble gas abundances 23 Helium in the Sun 26 Noble gases in the solar corpuscular radiation 27 THE GIANT PLANETS 36 The He abundances 36 The Ne-Xe abundances in Jupiter 39 i Isotopic ratios in Jupiter 40 VENUS :. : 42 THE MOON 43 Trapped solar (and other) noble gases in the lunar (and asteroidal) regoliths.-; 43 Nitrogen in lunar samples Cosmogenic noble gases in lunar samples 53 THE EXOSPHERES OF THE MOON AND MERCURY : 55 Sources and sinks 57 COMETS 58 INTERPLANETARY DUST PARTICLES AND MICROMETEORITES 59 IX

3 ELEMENTARY PARTICLES IN INTERPLANETARY SPACE 61 Galactic cosmic rays 61 Interstellar and interplanetary pick-up ions 62 Anomalous cosmic rays'. '. 63 ACKNOWLEDGMENTS 63 REFERENCES 63 3 Noble Gases in Meteorites - Trapped Components UlrichOtt OVERVIEW AND HISTORY 71 ELEMENTAL ABUNDANCE PATTERNS 73 I SOTOPIC COMPOSITIONS... : : 74 Helium '. :...; 75 Neon : ; 76 Argon..'...'.'...:. '...' 77 Krypton '. 78 Xenon 80 ORIGINS AND HISTORY Q(Pl)-gases,.... ; :'. :...83 Gases in presolar silicon carbide and graphite..' '. 84 Gases trapped in presolar diamond (HL, P3 and P6 components) 87 Ureilite gases...' '. 89 Subsolarand sub-q gases... ; 89 Sitings V.,..90 Other (lesser) components RELATIONS..;...91 Relationship between Q and solar gases..91 A more primitive component (in Xe and only in Xe?) 94 CONCLUDING REMARKS :. 96 ACKNOWLEDGMENTS 96 REFERENCES.' Noble Gases in the Moon and Meteorites: Radiogenic Components and Early Volatile Chronologies Timothy D. Swindle INTRODUCTION 101 LONG-LIVED NUCLIDES: CHRONOLOGY OF SOLAR SYSTEM EVOLUTION 102 Solar system impact history 103 Extinct radionuclides: Chronology of solar system formation 108 Iodine-xenon ;...1O9 '"Plutonium ;...;;.; Other fissioning nuclides? : 120 Other radiogenic noble gases ' ACKNOWLEDGMENTS...;; REFERENCES...;. ; 121

4 5 Cosmic-Ray-Produced Noble Gases in Meteorites Rainer Wieler INTRODUCTION 125 THE PRODUCTION OF COSMOGENIC NUCLIDES IN METEORITES ;...: 126 Fundamentals 126 Production systematics 128 Cosmogenic noble gases produced by capture of low-energy neutrons 139 Isotopic abundances of cosmogenic noble gases 141 EXPOSURE AGE DISTRIBUTIONS OF METEORITES 144 Undifferentiated meteorites 146 Differentiated meteorites : 149 Exposure ages and dynamical models of meteorite delivery 153 COMPLEX EXPOSUREHISTORIES.:...: 155 THE COSMIC RAY FLUX IN TIME 159 TERRESTRIAL AGES 161 COSMOGENIC NOBLE GASES PRODUCED BY SOLAR COSMIC RAYS (SCR) 162 ACKNOWLEDGMENTS 162 REFERENCES Martian Noble Gases Timothy D. Swindle STUDYING MARS AS ANOTHER PLANET 171 DISCOVERY OF MARTIAN METEORITES 171 MARTIAN ATMOSPHERE 175 OTHER MARTIAN NOBLE GAS RESERVOIRS 180 Martian interior (Chassigny) :..; 180 Other reservoirs I: Nakhlite (and ALH84001)Xe 181 Other reservoirs II: Shergottite Ar 182 Paleoatmosphere 183 MARTIAN CHRONOLOGY Ar- 39 Ar dating.-.-. ; 184 Cosmic-ray exposure ages 185 ACKNOWLEDGMENTS 187 REFERENCES Origin of Noble Gases in the Terrestrial Planets Robert O. Pepin, Donald Porcelli INTRODUCTION...; : 191 CHARACTERISTICS OF PLANETARY NOBLE GASES : 193 Planetary noble gas abundance patterns.... ; 193 Terrestrial noble gases.' '. 196 Noble gases on Venus : 205 Noble Gases on Mars : ACQUISITION OF PLANETARY NOBLE GASES..; 208 Early post-nebular solar wind 209 Adsorption on pre-planetary grains or protoplanetary bodies 210 Gravitational capture 210 Accretion of volatile-rich planetesimals 213

5 LOSSES AND MODIFICATIONS OF PLANETARY NOBLE GASES 216 Losses during accretion 216 Sputtering 217 Hydrodynamic escape Primordial xenon :.231 OUTSTANDING ISSUES ; 235 ACKNOWLEDGMENTS 239 REFERENCES Noble Gas Isotope Geochemistry of Mid-Ocean Ridge and Ocean Island Basalts: Characterization of Mantle Source Reservoirs David W. Graham INTRODUCTION 247 BACKGROUND 249 Noble gas chemical behavior 249 Mantle structure and noble gases 252 HELIUM 254 Significance '. 254 Radiogenic production 255 Mid-ocean ridge basalts 255 Ocean island basalts 265 NEON ; 279 Significance 279 Nucleogenic production ; Mid-ocean ridge basalts 281 Ocean island basalts 283 ARGON 284 Significance 284 Radiogenic production 284 Atmospheric contamination 284 Mid-ocean ridge basalts 285 Ocean island basalts 288 KRYPTON 289 XENON 289 Significance 289 Radiogenic production 290 Mid-ocean ridge basalts 291 Ocean island basalts 292 COUPLED RADIOGENIC/NUCLEOGENIC PRODUCTION 293 Neon-helium systematics 293 Argon-helium systematics 297 Xenon-neon-helium systematics 300 MANTLE ABUNDANCE PATTERNS OF NOBLE GASES 301 PRINCIPAL OBSERVATIONS 302 SUMMARY 303 ACKNOWLEDGMENTS 305 REFERENCES 305 xil

6 9 Noble Gases and Volatile Recycling at Subduction Zones David R. Hilton, Tobias P. Fischer, Bernard Marry INTRODUCTION ;..319 SAMPLING FOR NOBLE GASES../. 320 Volcanic and geothermal fluids ; 320 Hot spring waters and groundwaters ^." Geothermal wells 322 Natural gases 322 Mafic phenocrysts and xenoliths 322 Submarine glasses 323 Problematic issues of noble gas analysis 323 NOBLE GAS SYSTEMATICS OF ARC-RELATED VOLCAMSM 324 Helium isotope systematics of arc-related volcanism 325 Neon and argon isotope systematics of arc-related volcanism 330 Krypton and xenon isotope systematics of arc-related volcanism 333 Relative noble gas abundance systematics of arc-related volcanism 333 NOBLE GASES IN BACK-ARC BASINS Helium isotopes in back-arc basins 334 Neon isotopes in back-arc basins 337 Argon, krypton and xenon isotopes in back-arc basins 338 RECYCLING OF VOLATILES AT SUBDUCTION ZONES: A MASS BALANCE APPROACH 340 The global volatile output at arc volcanoes: The 3 He approach 340 Volatile output at individual arcs SO 2 and the power law distribution 341 Using helium to resolve volatile provenance 349 Problematic issues regarding estimates of volatile output at arcs 351 Volatile output at the back-arc and fore-arc regions 352 The volatile input via the trench 353 Volatile mass balance at subduction zones 355 Global implications of volatile recycling at subduction zones 358 SUMMARY AND FUTURE WORK.": ; 361 ACKNOWLEDGMENTS ' REFERENCES Storage and Transport of Noble Gases in the Subcontinental Lithosphere Tibor J. Dunai, Donald Porcelli INTRODUCTION 371 SUBCONTINENTAL MANTLE AS GEOCHEMICAL RESERVOIR Thickness of the lithosphere 372 Composition of the lithosphere 373 Age of the lithosphere ; 374 Possible xenolith noble gas components 374 NOBLE GASES IN ULTRAMAFIC XENOLITHS AND PHENOCRYSTS 377 Fluid inclusions as hosts for noble gases 377 Helium isotopic variations 381 He-Sr relationships 382 He-C relationships : 384 The heavier noble gases Regional studies of the sources of xenolith mantle rare gases 388 The mantle sources of xenolith He 394 Introducing He into the lithosphere : 396 xiii

7 DIAMONDS 397 Ancient He 398 Ancient Xe 399 Mantle sources of diamond rare gases 399 MANTLE VOLATILES IN THE CONTINENTAL CRUST CONCLUSIONS : ;. 400 ACKNOWLEDGMENTS REFERENCES:...:...;: :; ; Models for the Distribution of Terrestrial Noble Gases and Evolution of the Atmosphere D. Porcelli, C.J. Ballentine INTRODUCTION 411 RADIOGENIC COMPONENTS IN THE BULK EARTH AND ATMOSPHERE...; 412 Radiogenic He and nucleogenic Ne : 412 Radiogenic Ar...: Radiogenic and fissiogenic Xe ;: MANTLE NOBLE GAS CHARACTERISTICS : 419 Helium isotopic compositions in the mantle 419 Neon isotopic compositions in the mantle.. ' Argon isotopic compositions in the mantle : 423 Xe isotopes and a nonresidual upper mantle 427 Mantle noble gas relative abundances 428 Noble gas fluxes and mantle concentrations : Undepleted mantle...: : : Coupled degassing of noble gases....:...: TRACE ELEMENT ISOTOPE CONSTRAINTS ON MANTLE RESERVOIRS'. :: 436 Relationship between noble gases and radiogenic isotopes : 436 Mass and character of the depleted mantle 436 Timing of mantle depletion and recycling 438 PHYSICAL CONSTRAINTS ON MANTLE MODELS Mantle reservoirs 438 Geophysical evidence for the scale of mantle convection 439 Early Earth history 443 NOBLE GAS MANTLE MODELS 446 Single reservoir degassing 446 Limited interaction box models 448 Steady state box models 452 Break-up of a previously layered mantle 457 The lower boundary layer reservoir 457 The upper boundary layer reservoir, 459 Deeper or 'abyssal' layering 459 Heterogeneities preserved within the convecting mantle 460 Depleted, high He/U mantle 462 Storage of noble gases in the core 463 Subduction of meteoritic He : 465 CONCLUSIONS Overall assessment of the models 466 Some persistent misconceptions 467 Important parameters that are still unknown 468 ACKNOWLEDGMENTS ; REFERENCES 469 xiv

8 12 Production, Release and Transport of Noble Gases in the Continental Crust Chris J. Ballentine, Pete G. Burnard INTRODUCTION 481 RADIOGENIC, NUCLEOGENIC, AND FISSIOGENIC NOBLE GASES 482 The subsurface neutron flux and reaction probability :.482 Helium ;.../ : 487 Neon. ;.49O Argon 495 Krypton and xenon 498 Cosmogenic noble gas production 501 Interplanetary dust accumulation 503 Production rates in continental crust today and over the history of the Earth 504 RELEASE OF NOBLE GASES FROM MINERALS IN THE CRUST 506 Recoil loss Diffusive loss from minerals 506 :.5O9 Mineral breakdown/diagenesis/metamorphism/alteration 512 TRANSPORT OF NOBLE GASES FROM THE DEEP CRUST TO SHALLOW LEVEL SYSTEMS 514. Diffusion: A viable transport mechanism to degas the continental crust? 515 Differential release and transport of helium and argon 517 Accumulation and release: Fluid flow in the crust ; 5 19 HEAT AND HELIUM : The relationship between 4 He and heat Transport of mantle heat and helium through the crust : 521 Transport of crustal heat and 4 He 524 MAGMATIC NOBLE GASES IN THE CRUST..: '. 525 Tectonic control on magmatic fluid location Fossil magmatic gases 529 ACKNOWLEDGMENTS. REFERENCES......:..: : : Tracing Fluid Origin, Transport and Interaction in the Crust Chris J. Ballentine, Ray Burgess, Bernard Marty INTRODUCTION :: : : ; 539 PHYSICAL CHEMISTRY OF NOBLE GASES IN CRUSTAL FLUIDS.540 Henry's law and the assumption of ideality. 540 Non-ideality in the gas phase Non-ideality in the fluid phase :...:. 544 Noble gas solubility in water and oil 546 PHASE EQUILIBRIUM AND FRACTIONATION OF NOBLE GASES Liquid-gas phase partitioning of noble gases 548 Liquid-liquid phase partitioning of noble gases 549 Relative fractionation Rayleigh fractionation ;. 551 Re-solution and effervescence 555 Multiple subsurface fluid phases 558 Diffusion or kinetic fractionation RESOLVING DIFFERENT NOBLE GAS COMPONENTS IN CRUSTAL FLUIDS 562 NOBLE GASES IN HYDROCARBON GAS AND OIL RESERVOIRS 565 Identifying and quantifying groundwater/gas/oil interaction '. 567 Case studies...: 569 NOBLE GASES IN ANCIENT GROUNDWATERS AND CRUSTAL DEGASSING 581 Sources of He isotopes in groundwaters.. : 582 Deep aquifers and the crustal He flux 584 xv

9 Advective versus diffusive transfer of noble gases in basins 590 Tentative synthesis 592 MAGMATIC FLUIDS IN THE CRUST 595 Mantle degassing in the continental crust: The noble gas imprint 595 NOBLE GASES IN MINERAL DEPOSITS AND HYDROTHERMAL FLUIDS Post-entrapment modification of He and Ar isotopes Noble gas mixtures in mineralizing fluids 601 Description and analysis of multi-component noble gas mixtures in ore fluids 601 Further developments.605 ACKNOWLEDGMENTS 608 REFERENCES Noble Gases in Lakes and Ground Waters Rolf Kipfer, Werner Aeschbach-Hertig, Frank Peeters, Marvin Stute INTRODUCTION... : : ;: : ' 615 ANALYTICAL TECHNIQUES.617 NOBLE GAS COMPONENTS IN WATER ; 619 Atmospheric noble gases 1: Solubility equilibrium 619 Atmospheric noble gases 2: Excess Air.' ; 624 Radiogenic He (and Ar) 629 Terrigenic He... :...: Radioactive noble gas isotopes Man made pseudo-conservative trace gases 633 Data evaluation and interpretation 633 Conceptual models for noble gases in water 634 Separation of the components., 641 Interpretation :.: 647 APPLICATIONS IN LAKES.,..: Mixing and the distribution of dissolved substances in lakes 651 Distribution of noble gases in lakes :. 653 Application of 3 H- 3 He dating in lakes 654 Quantification of vertical exchange rates and vertical turbulent diffusivities 658 He flux from the continental crust and oxygen depletion : 661 Noble gases from the Earth's mantle.: 664 Applications in ground water 666 Dating of young ground waters 667 Dating of old ground waters 676 Noble gas recharge temperatures 679 Excess air 683 NOBLE GASES IN ICE.. 687; Gravitational separation :... '. 687 Thermal diffusion 687 Helium isotopes 689 REFERENCES:.. ;..:, Noble Gases in Ocean Waters and Sediments Peter Schlosser, Gisela Winckler INTRODUCTION 701 TRACING OCEAN CIRCULATION USING 3 HE AND TRITIUM 702 Tritium/ 3 He method : 702 Exemplary results from tritium/ 3 He studies..706 MANTLE 3 HE.' : 709 General background 709 Geochemical background, He plumes in the ocean 710 xvi

10 THE FLUX OF 3 HE AND 4 HE FROM THE SEAFLOOR 711 "He He 713 EXTRATERRESTRIAL 3 HE IN DEEP-SEA SEDIMENTS 715 Delivery of extraterrestrial 3 He to the ocean sediments Applications of the IDP-derived 3 He method : 717 NOBLE GASES IN DEEP-SEA BRINES 720 The Red Sea 720 The Eastern Mediterranean 721 AIR/SEA GAS EXCHANGE STUDIED BY DUAL TRACER RELEASE EXPERIMENTS Background 721 SF 6 / 3 He Method 723 Results from oceanic dual gas tracer releases...: '.'. 723 PERSPECTIVES : 723 REFERENCES Cosmic-Ray-Produced Noble Gases in Terrestrial Rocks: Dating Tools for Surface Processes Samuel Niedermann INTRODUCTION 731 THE FUNDAMENTALS OF SURFACE EXPOSURE DATING 732 Production mechanisms of cosmogenic nuclides in terrestrial rocks 732 Temporal variation of cosmogenic nuclide production 740 Cosmogenic nuclide production at depth and on eroding surfaces 748 Derivation of exposure ages and erosion rates 750 Error considerations 754 PRODUCTION RATES OF COSMOGENIC NUCLIDES 755 Experimental determinations of production rates 755 Production rates obtained by model calculations >. 761 EXPERIMENTAL ISSUES 762 Retentivity of minerals for cosmogenic He and Ne 762 Discrimination of cosmogenic against trapped, radiogenic, and nucleogenic components 763 Cosmogenic noble gases as a nuisance 769 Cosmogenic noble gases versus radionuclides :.770 APPLICATION EXAMPLES '..771 Dating of lava flows Glacier movement and ice sheet evolution :.: 772 Rates of erosion and soil accumulation 773 Rates of tectonic uplift 775 Earthquakes and landslides 775 Further applications 776 Future prospects 776 ACKNOWLEDGMENTS ; 777 REFERENCES : 777 xvii

11 17 K-Ar and Ar-Ar Dating Simon Kelley INTRODUCTION A BIT OF HISTORY 785 THE K-AR AND AR-AR DATING METHODS 786 Introduction 786 Assumptions 787 CALCULATING K-AR AND AR-AR AGES 788 The values of constants and estimation of errors 792 ARGON DIFFUSION AND SOLUBILITY '. 795 Argon diffusion (and its use to determine thermal histories) 795 Argon solubility (and the causes of extraneous argon) 798 APPLICATIONS 806 Thermochronology 806 Dating young volcanic eruptions : '. 809 High-precision ages on altered basalts 809 Dating low-temperature processes 809 Unique samples 810 Acknowledgments 810 REFERENCES (U-Th)/He Dating: Techniques, Calibrations, and Applications Kenneth A. Farley INTRODUCTION....' Rationale 819 TECHNICAL ASPECTS : He ingrowth DIFFUSION BEHAVIOR 821 Apatite '. 822 Hematite.:. '. 825 Titanite 825 Zircon 826 Garnet 827 The cc-emission correction 827 Analytical procedures, accuracy, precision and mineral standards 832 INTERPRETATION OF HE AGES AND EXAMPLES 835 He cooling ages 835 Some case studies FUTURE PROSPECTS ' 839 ACKNOWLEDGMENTS.840 REFERENCES, APPENDIX: ANALYTICAL TECHNIQUES 844 xv in

Composition and the Early History of the Earth

Composition and the Early History of the Earth Composition and the Early History of the Earth Sujoy Mukhopadhyay CIDER 2006 What we will cover in this lecture Composition of Earth Short lived nuclides and differentiation of the Earth Atmosphere and

More information

What can isotopes tell us about mantle dynamics? Sujoy Mukhopadhyay. Harvard University

What can isotopes tell us about mantle dynamics? Sujoy Mukhopadhyay. Harvard University What can isotopes tell us about mantle dynamics? Sujoy Mukhopadhyay Harvard University The mantle zoo Hofmann, 1997 187 Os/ 188 Os 0.168 0.156 0.144 0.132 EM1 Hawaii Pitcairn DMM peridotites Shield Basalts

More information

Halogen and argon evidence of Martian hydrous fluids in nakhlite meteorites Ray Burgess

Halogen and argon evidence of Martian hydrous fluids in nakhlite meteorites Ray Burgess Halogen and argon evidence of Martian hydrous fluids in nakhlite meteorites Ray Burgess School of Earth, Atmospheric and Environmental Sciences University of Manchester, UK Topics Halogens and noble gases

More information

Volatiles in the terrestrial planets. Sujoy Mukhopadhyay University of California, Davis CIDER, 2014

Volatiles in the terrestrial planets. Sujoy Mukhopadhyay University of California, Davis CIDER, 2014 Volatiles in the terrestrial planets Sujoy Mukhopadhyay University of California, Davis CIDER, 2014 Atmophiles: Elements I will talk about rock-loving iron-loving sulfur-loving Temperatures in Protoplanetary

More information

Chapter 1: Introduction...1 Chapter 2: Energy, Entropy and Fundamental Thermodynamic Concepts...24

Chapter 1: Introduction...1 Chapter 2: Energy, Entropy and Fundamental Thermodynamic Concepts...24 Table of Contents Part I: The Geochemical Toolbox Chapter 1: Introduction...1 Geochemistry...1 This Book...2 The Philosophy of Science...4 Building Scientific Understanding...4 The Scientist as Skeptic...5

More information

Isotopic record of the atmosphere and hydrosphere

Isotopic record of the atmosphere and hydrosphere Isotopic record of the atmosphere and hydrosphere W. F. McDonough 1 1 Department of Earth Sciences and Research Center for Neutrino Science, Tohoku University, Sendai 980-8578, Japan (Dated: March 7, 2018)

More information

Origin of the Solar System

Origin of the Solar System Origin of the Solar System Look for General Properties Dynamical Regularities Orbits in plane, nearly circular Orbit sun in same direction (CCW from N.P.) Rotation Axes to orbit plane (Sun & most planets;

More information

PTYS 214 Spring Announcements. Next midterm 3/1!

PTYS 214 Spring Announcements. Next midterm 3/1! PTYS 214 Spring 2018 Announcements Next midterm 3/1! 1 Previously Solar flux decreases as radiation spreads out away from the Sun Planets are exposed to some small amount of the total solar radiation A

More information

For thought: Excess volatiles

For thought: Excess volatiles For thought: Excess volatiles Term coined by William Rubey (circa 1955) Definition: Compounds present at Earth s surface that were not derived from converting igneous rock to sedimentary rock Rubey and

More information

THE PLANETARY SCIENTIST'S COMPANION

THE PLANETARY SCIENTIST'S COMPANION THE PLANETARY SCIENTIST'S COMPANION Katharina Lodders Bruce Fegley, Jr. New York Oxford Oxford University Press 1998 Contents 1 Technical data Table 1.1 The Greek alphabet 1 Table 1.2 Prefixes used with

More information

RAYMOND SIEVER Harvard University

RAYMOND SIEVER Harvard University E A R T H FOURTH EDITION FRANK PRESS National Academy of Sciences RAYMOND SIEVER Harvard University W. H. Freeman and Company New York Preface xiii Acknowledgments xviii PART I PROLOGUE CHAPTER 1 HISTORY

More information

Radiogenic Isotope Systematics and Noble Gases. Sujoy Mukhopadhyay CIDER 2006

Radiogenic Isotope Systematics and Noble Gases. Sujoy Mukhopadhyay CIDER 2006 Radiogenic Isotope Systematics and Noble Gases Sujoy Mukhopadhyay CIDER 2006 What I will not cover.. U-Th-Pb sytematics 206 Pb 204 Pb 207 Pb 204 Pb 208 Pb 204 Pb = t = t = t 206 Pb 204 Pb 207 Pb 204 Pb

More information

The History of the Earth

The History of the Earth The History of the Earth We have talked about how the universe and sun formed, but what about the planets and moons? Review: Origin of the Universe The universe began about 13.7 billion years ago The Big

More information

Terrestrial Planets: The Earth as a Planet

Terrestrial Planets: The Earth as a Planet Terrestrial Planets: The Earth as a Planet In today s class, we want to look at those characteristics of the Earth that are also important in our understanding of the other terrestrial planets. This is

More information

Question 1 (1 point) Question 2 (1 point) Question 3 (1 point)

Question 1 (1 point) Question 2 (1 point) Question 3 (1 point) Question 1 (1 point) If the Earth accreted relatively slowly, the heat obtained from the gravitational potential energy would have had time to escape during its accretion. We know that the Earth was already

More information

General Introduction. The Earth as an evolving geologic body

General Introduction. The Earth as an evolving geologic body General Introduction The Earth as an evolving geologic body Unique/important attributes of Planet Earth 1. Rocky planet w/ strong magnetic field Mercury has a weak field, Mars has a dead field 1 Unique/important

More information

Tectonics. Planets, Moons & Rings 9/11/13 movements of the planet s crust

Tectonics. Planets, Moons & Rings 9/11/13 movements of the planet s crust Tectonics Planets, Moons & Rings 9/11/13 movements of the planet s crust Planetary History Planets formed HOT Denser materials fall to center Planet cools by conduction, convection, radiation to space

More information

Chapter 9. ASTRONOMY 202 Spring 2007: Solar System Exploration. Class 26: Planetary Geology [3/23/07] Announcements.

Chapter 9. ASTRONOMY 202 Spring 2007: Solar System Exploration. Class 26: Planetary Geology [3/23/07] Announcements. ASTRONOMY 202 Spring 2007: Solar System Exploration Instructor: Dr. David Alexander Web-site: www.ruf.rice.edu/~dalex/astr202_s07 Class 26: Planetary Geology [3/23/07] Announcements Planetary Geology Planetary

More information

What can noble gases really say about mantle. 2) Extent of mantle degassing

What can noble gases really say about mantle. 2) Extent of mantle degassing What can noble gases really say about mantle convection and the deep Earth volatile cycles? 1) Constraints on mass flow 1) Constraints on mass flow 2) Extent of mantle degassing Outline: -Noble gas geochemistry

More information

Volatiles on Venus: A missing link in understanding terrestrial planet evolution

Volatiles on Venus: A missing link in understanding terrestrial planet evolution Volatiles on Venus: A missing link in understanding terrestrial planet evolution Melissa G. Trainer Planetary Environments Laboratory NASA Goddard Space Flight Center 12 July 2017 Trainer - DS Mid-Term

More information

EARTH S ENERGY SOURCES

EARTH S ENERGY SOURCES EARTH S ENERGY SOURCES The geological processes that shape the Earth s surface are powered by two major sources of energy; geothermal heat from the Earth s interior and external energy from the sun. The

More information

Marine Science and Oceanography

Marine Science and Oceanography Marine Science and Oceanography Marine geology- study of the ocean floor Physical oceanography- study of waves, currents, and tides Marine biology study of nature and distribution of marine organisms Chemical

More information

Formation of the Earth and Solar System

Formation of the Earth and Solar System Formation of the Earth and Solar System a. Supernova and formation of primordial dust cloud. NEBULAR HYPOTHESIS b. Condensation of primordial dust. Forms disk-shaped nubular cloud rotating counterclockwise.

More information

Nitrogen speciation in upper mantle fluids and the origin of Earth s nitrogen-rich atmosphere

Nitrogen speciation in upper mantle fluids and the origin of Earth s nitrogen-rich atmosphere Supporting Online Material for Nitrogen speciation in upper mantle fluids and the origin of Earth s nitrogen-rich atmosphere Sami Mikhail & Dimitri Sverjensky S1. Supplementary discussion S1.1 The selection

More information

Use models to describe the sun s place in space in relation to the Milky Way Galaxy and the distribution of galaxy clusters in the universe.

Use models to describe the sun s place in space in relation to the Milky Way Galaxy and the distribution of galaxy clusters in the universe. The Milky Way Galaxy consists of more than two hundred billion stars, the sun being one of them, and is one of hundreds of billions of galaxies in the known universe. s of the formation and structure of

More information

Geochemical and mineralogical technics to investigate the lithosphere and the asthenosphere. 07/11/2017 GEO-DEEP 9300 Claire Aupart

Geochemical and mineralogical technics to investigate the lithosphere and the asthenosphere. 07/11/2017 GEO-DEEP 9300 Claire Aupart Geochemical and mineralogical technics to investigate the lithosphere and the asthenosphere 07/11/2017 GEO-DEEP 9300 Claire Aupart Introduction Introduction Getting samples Cores: Maximum depth reach in

More information

Comet Science Goals II

Comet Science Goals II Comet Science Goals II {questions for goals} Don Brownlee Did the events postulated by the Nice Hypothesis really happen? Were there wide-spread solar system wide impact events that were coeval with the

More information

The Earth Fast Facts. Outline. The Solar System is Ours! Astronomy 210. Section 1 MWF Astronomy Building

The Earth Fast Facts. Outline. The Solar System is Ours! Astronomy 210. Section 1 MWF Astronomy Building Astronomy 210 Section 1 MWF 1500-1550 134 Astronomy Building This Class (Lecture 19): The Earth Night Observations! Next Class: The Earth-Moon System Music: Amy Hit the Atmosphere Counting Crows The Solar

More information

Differentiation of planetary interiors. Rocky Planets Interiors and surface geophysics

Differentiation of planetary interiors. Rocky Planets Interiors and surface geophysics Differentiation of planetary interiors Rocky Planets Interiors and surface geophysics Process of separation of internal planetary layers that takes place as a result of the physical and chemical properties

More information

Today we begin with. Water is everywhere on and in Earth It is the only substance that exists in all 3 phases (solid, liquid, gas) on the surface!

Today we begin with. Water is everywhere on and in Earth It is the only substance that exists in all 3 phases (solid, liquid, gas) on the surface! Water is everywhere on and in Earth It is the only substance that exists in all 3 phases (solid, liquid, gas) on the surface! Today we begin with Water Origin of Earth s water Properties of water Water

More information

What are terrestrial planets like on the inside? Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds. Seismic Waves.

What are terrestrial planets like on the inside? Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds. Seismic Waves. Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds What are terrestrial planets like on the inside? Seismic Waves Vibrations that travel through Earth s interior tell us what Earth is

More information

Today. Events. Terrestrial Planet Geology. Fall break next week - no class Tuesday

Today. Events. Terrestrial Planet Geology. Fall break next week - no class Tuesday Today Terrestrial Planet Geology Events Fall break next week - no class Tuesday When did the planets form? We cannot find the age of a planet, but we can find the ages of the rocks that make it up. We

More information

Comets and the Origin and Evolution of Life

Comets and the Origin and Evolution of Life Paul J. Thomas Christopher F. Chyba Christopher P. McKay Editors Comets and the Origin and Evolution of Life With 47 Illustrations Springer Contents Contributors xi Introduction: Comets and the Origin

More information

Mantle geochemistry: How geochemists see the deep Earth

Mantle geochemistry: How geochemists see the deep Earth Geochemistry: Overview: the geochemist's Earth (reservoirs, budgets and processes) Mantle geochemistry: How geochemists see the deep Earth Don DePaolo/Stan Hart CIDER - KITP Summer School Lecture #1, July

More information

Any Questions? 99.9 % of mass is in the Sun; 99 % of angular momentum is in the planets. Planets in two groups:

Any Questions? 99.9 % of mass is in the Sun; 99 % of angular momentum is in the planets. Planets in two groups: Geology of the Hawaiian Islands Class 2 15 January 2004 Any Questions? Origin of solar system Pick a theory, any theory, but it must be consistent with these facts: Planets all revolve around the Sun in

More information

Origin of solar system. Origin of solar system. Geology of the Hawaiian Islands. Any Questions? Class 2 15 January 2004

Origin of solar system. Origin of solar system. Geology of the Hawaiian Islands. Any Questions? Class 2 15 January 2004 Geology of the Hawaiian Islands Class 2 15 January 2004 Any Questions? Origin of solar system Pick a theory, any theory, but it must be consistent with these facts: Planets all revolve around the Sun in

More information

Variation of Elements in Nature

Variation of Elements in Nature Variation of Elements in Nature by V.S. Venkatavaradan There are an infinite variety of things in an infinite variety of shapes, colours and states in nature. Despite varied properties, these multitudes

More information

The Terrestrial Planets

The Terrestrial Planets The Terrestrial Planets Large Bodies: Earth (1 R E, 1 M E ) Venus (0.95 R E, 0.82 M E ) Small Bodies: Mars (0.53 R E, 0.11 M E ) Mercury (0.38 R E, 0.055 M E ) Moon (0.27 R E, 0.012 M E ) The surfaces

More information

Origin of the Solar System

Origin of the Solar System Origin of the Solar System Current Properties of the Solar System Look for General Properties Dynamical Regularities Orbits in plane, nearly circular Orbit sun in same direction (CCW from North pole) Rotation

More information

The Official CA State Science Education Standards for Earth Science K 8

The Official CA State Science Education Standards for Earth Science K 8 The Official CA State Science Education Standards for Earth Science K 8 Kindergarten The Earth is composed of land, air and water. As a basis for understanding this concept, students know: a. characteristics

More information

Outline 9: Origin of the Earth: solids, liquids, and gases. The Early Archean Earth

Outline 9: Origin of the Earth: solids, liquids, and gases. The Early Archean Earth Outline 9: Origin of the Earth: solids, liquids, and gases The Early Archean Earth Origin of Earth s Matter The earth is made of recycled elements formed in stars that existed prior to our Sun. Supernova

More information

Outline 9: Origin of the Earth: solids, liquids, and gases

Outline 9: Origin of the Earth: solids, liquids, and gases Outline 9: Origin of the Earth: solids, liquids, and gases The Early Archean Earth Origin of Earth s Matter The earth is made of recycled elements formed in stars that existed prior to our Sun. Supernova

More information

OCN 201: Earth Structure

OCN 201: Earth Structure OCN 201: Earth Structure Eric Heinen Eric H. De Carlo, Carlo: OCN 201, OCN Sp2010 201, Fall 2004 Early History of the Earth Rapid accretion of Earth and attendant dissipation of kinetic energy caused tremendous

More information

AN INTRODUCTION TO COSMOCHEMISTRY

AN INTRODUCTION TO COSMOCHEMISTRY AN INTRODUCTION TO COSMOCHEMISTRY CHARLES R. COWLEY Professor of Astronomy, University of Michigan CAMBRIDGE UNIVERSITY PRESS Foreword V a % e x i 1 Overview 1 1.1 The Scope of Cosmochemistry 1 1.2 Cosmochemistry

More information

Remote Sensing of the Earth s Interior

Remote Sensing of the Earth s Interior Remote Sensing of the Earth s Interior Earth s interior is largely inaccessible Origin and Layering of the Earth: Geochemical Perspectives Composition of Earth cannot be understood in isolation Sun and

More information

Planet Earth. Our Home APOD

Planet Earth. Our Home APOD Planet Earth Our Home APOD 1 Earth a highly evolved planet = altered dramatically since formation, due to flow of energy from interior to surface 2 Planet Earth Facts diameter (equator) 12,756 km radius

More information

Evolution of the Atmosphere: The Biological Connection

Evolution of the Atmosphere: The Biological Connection Evolution of the Atmosphere: The Biological Connection The Earth s Four Spheres How It All Began Or At Least How We Think It Began O.k. it s a good guess Egg of energy The Big Bang splattered radiation

More information

The Solar System. Earth as a Planet

The Solar System. Earth as a Planet The Solar System Earth as a Planet Earth s Interior Core: Highest density; nickel and iron Mantle: Moderate density; silicon, oxygen, etc. Crust: Lowest density; granite, basalt, etc. Differentiation Gravity

More information

Earth 50: Planets and the Layered Earth

Earth 50: Planets and the Layered Earth Earth 50: Planets and the Layered Earth 9-22-06 Formation of Elements light elements (up to Fe) heavier elements The Solar Nebula inner versus outer planets origin of compositional variations dominance

More information

For the next few weeks: Terrestrial Planets, their Moons, and the Sun. Planetary Surfaces and Interiors 2/20/07

For the next few weeks: Terrestrial Planets, their Moons, and the Sun. Planetary Surfaces and Interiors 2/20/07 For the next few weeks: Terrestrial Planets, their Moons, and the Sun Announcements Reading Assignment Section 9-1 (pp 186-189), 9-5 and 9-6 (pp 199-203) 3 rd Homework is now posted on the course website

More information

Comparative Planetology I: Our Solar System

Comparative Planetology I: Our Solar System Comparative Planetology I: Our Solar System Guiding Questions 1. Are all the other planets similar to Earth, or are they very different? 2. Do other planets have moons like Earth s Moon? 3. How do astronomers

More information

Jochen Hoefs Stable Isotope Geochemistry

Jochen Hoefs Stable Isotope Geochemistry Jochen Hoefs Stable Isotope Geochemistry Springer-Verlag Berlin Heidelberg GmbH Jochen Hoefs Stable Isotope Geochemistry 4th, Completely Revised, Updated, and Enlarged Edition With 73 Figures and 22 Tables

More information

Planetary Atmospheres

Planetary Atmospheres Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 22:1 Where do planetary atmospheres come from? Three primary sources Primordial (solar

More information

The Planets, Asteroids, Moons, etc.

The Planets, Asteroids, Moons, etc. DATE DUE: Ms. Terry J. Boroughs Geology 305 Name: Section: The Planets, Asteroids, Moons, etc. Instructions: Read each question carefully before selecting the BEST answer or option. Use GEOLOGIC vocabulary

More information

Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds

Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds Chapter 9 Planetary Geology: Earth and the Other Terrestrial Worlds 9.1 Connecting Planetary Interiors and Surfaces Our goals for learning What are terrestrial planets like on the inside? What causes geological

More information

Extraterrestrial Volcanism

Extraterrestrial Volcanism Extraterrestrial Volcanism What does it take to create volcanic activity? How do different planetary conditions influence volcanism? Venus Volcanism in our solar system. Io Europa Mercury Venus Earth/Moon

More information

Evidences for geochemically distinct mantle components

Evidences for geochemically distinct mantle components Evidences for geochemically distinct mantle components 1 Mantle Array Oceanic basalts, including seamounts, oceanic islands and middle ocean ridge basalts, were used. 2 Binary All analyses fall between

More information

Astro 1010 Planetary Astronomy Sample Questions for Exam 4

Astro 1010 Planetary Astronomy Sample Questions for Exam 4 Astro 1010 Planetary Astronomy Sample Questions for Exam 4 Chapter 8 1. Which of the following processes is not important in shaping the surface of terrestrial planets? a) Impact cratering b) Tectonism

More information

page - Lab 13 - Introduction to the Geology of the Terrestrial Planets

page - Lab 13 - Introduction to the Geology of the Terrestrial Planets page - Lab 13 - Introduction to the Geology of the Terrestrial Planets Introduction There are two main families of planets in our solar system: the inner Terrestrial planets (Earth, Mercury, Venus, and

More information

Earth and Space Science, Beginning with School Year (One Credit).

Earth and Space Science, Beginning with School Year (One Credit). 112.36. Earth and Space Science, Beginning with School Year 2010-2011 (One Credit). (c) Knowledge and skills. (1) Scientific processes. The student conducts laboratory and field investigations, for at

More information

Chapter 2 Geography. Getting to know Earth

Chapter 2 Geography. Getting to know Earth Chapter 2 Geography Getting to know Earth Our Solar System Sun is at the center of our solar system Contains a lot of Mass» Mass gives the Sun gravitational pull» This keeps the planets in our solar system

More information

LIGO sees binary neutron star merger on August 17, 2017

LIGO sees binary neutron star merger on August 17, 2017 LIGO sees binary neutron star merger on August 17, 2017 Laser Interferometer Gravitational-Wave Observatory (LIGO) Laser Interferometer Gravitational-Wave Observatory (LIGO) Multi-Messenger Astronomy This

More information

Earth, the Lively* Planet. * not counting the life on the planet!

Earth, the Lively* Planet. * not counting the life on the planet! Earth, the Lively* Planet * not counting the life on the planet! What We Will Learn Today What are planet Earth s features? What processes shape planetary surfaces? How does Earth s surface move? How did

More information

Phys 214. Planets and Life

Phys 214. Planets and Life Phys 214. Planets and Life Dr. Cristina Buzea Department of Physics Room 259 E-mail: cristi@physics.queensu.ca (Please use PHYS214 in e-mail subject) Lecture 10. Geology and life. Part 1 (Page 99-123)

More information

Module 4: Astronomy The Solar System Topic 3 Content: The Terrestrial Planets Notes Introduction

Module 4: Astronomy The Solar System Topic 3 Content: The Terrestrial Planets Notes Introduction Introduction The four planets closest to the Sun are called "the terrestrial planets." These inner planets are considered to be small and rocky. Although they are all rocky, their varying distances from

More information

Dating. AST111 Lecture 8a. Isotopic composition Radioactive dating

Dating. AST111 Lecture 8a. Isotopic composition Radioactive dating Dating Martian Lafayette Asteroid with patterns caused by the passaged through the atmosphere. Line on the fusion crust were caused by beads of molten rock. AST111 Lecture 8a Isotopic composition Radioactive

More information

Contents. 1 Introduction Stable Isotopes

Contents. 1 Introduction Stable Isotopes Contents 1 Introduction... 1 Part I Stable Isotopes 2 Isotope Geochemistry of Natural Waters... 11 2.1 Some Properties of Waters and Solutions... 11 2.1.1 The Notion of Activity and the Activity Coefficient...

More information

ESS 312 Geochemistry Simulating Earth degassing using radionuclides

ESS 312 Geochemistry Simulating Earth degassing using radionuclides ESS 312 Geochemistry Simulating Earth degassing using radionuclides CHEMICAL AND ISOTOPIC EVOLUTION OF A TWO-RESERVOIR SYSTEM In lectures we discussed radioactive decay and build-up of a daughter isotope

More information

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. ASTRO 102/104 Prelim 2 Name Section MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) This is version E of the exam. Please fill in (E). A) This

More information

Chapter 8 Lecture. The Cosmic Perspective Seventh Edition. Formation of the Solar System

Chapter 8 Lecture. The Cosmic Perspective Seventh Edition. Formation of the Solar System Chapter 8 Lecture The Cosmic Perspective Seventh Edition Formation of the Solar System Formation of the Solar System 8.1 The Search for Origins Our goals for learning: Develop a theory of solar system

More information

Analysis of samples returned by space missions : Apollo, Genesis, Stardust, Marco Polo

Analysis of samples returned by space missions : Apollo, Genesis, Stardust, Marco Polo Analysis of samples returned by space missions : Apollo, Genesis, Stardust, Marco Polo Bernard Marty Centre de Recherches Pétrographiques et Géochimiques, UPR2300 CNRS Ecole Nationale Supérieure de Géologie

More information

10/11/2010. Acceleration due to gravity, a. Bulk Properties Mass = 6 x kg Diameter = 12,756 km Density = 5515 kg/m 3 (mix of rock and iron)

10/11/2010. Acceleration due to gravity, a. Bulk Properties Mass = 6 x kg Diameter = 12,756 km Density = 5515 kg/m 3 (mix of rock and iron) Acceleration due to gravity, a Bulk Properties Mass = 6 x 10 24 kg Diameter = 12,756 km Density = 5515 kg/m 3 (mix of rock and iron) Escape Velocity, v e Albedo Amount of sunlight reflected back into space

More information

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. ASTRO 102/104 Prelim 2 Name Section MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) This is version B of the exam. Please fill in (B). A) This

More information

Mass Wasting and Landscape Evolution

Mass Wasting and Landscape Evolution Mass Wasting and Landscape Evolution 11-8-06 Uplift is a tectonic process Three types of uplift: 1. Collisional uplift 2. isostatic uplift 3. Extensional uplif. A physical experiment in isostasy: [crust

More information

Systems? Climate Systems. Earth Systems. Earth Interior Systems. Atmospheric/Biospheric Systems: Human Impact Hydrologic Cycle.

Systems? Climate Systems. Earth Systems. Earth Interior Systems. Atmospheric/Biospheric Systems: Human Impact Hydrologic Cycle. Chapter 15 Climate Systems Systems? What is a system? Geologic phenomena are complex. All processes are related to, and interact with, other processes. So it is useful to think of geologic processes as

More information

25-Nov-14. The Structure of Earth s Interior. What unique features of Earth are important for life as we know it?

25-Nov-14. The Structure of Earth s Interior. What unique features of Earth are important for life as we know it? What unique features of Earth are important for life as we know it? Surface liquid water Atmospheric oxygen These are obvious Less obvious are: Plate tectonics Climate stability The Structure of Earth

More information

The greenhouse effect

The greenhouse effect The greenhouse effect Visible light arrives About half reflected, half is absorbed by the ground. This absorbed energy is then reradiated, but NOT in the visible (would just go out again anyway); in the

More information

D) outer core B) 1300 C A) rigid mantle A) 2000 C B) density, temperature, and pressure increase D) stiffer mantle C) outer core

D) outer core B) 1300 C A) rigid mantle A) 2000 C B) density, temperature, and pressure increase D) stiffer mantle C) outer core 1. In which area of Earth's interior is the pressure most likely to be 2.5 million atmospheres? A) asthenosphere B) stiffer mantle C) inner core D) outer core Base your answers to questions 2 and 3 on

More information

Differentiation 2: mantle, crust OUTLINE

Differentiation 2: mantle, crust OUTLINE Differentiation 2: mantle, crust OUTLINE Reading this week: Should have been White Ch 10 and 11!! 7- Nov Differentiation of the Earth, Core formation W 10.6.6, 11.4 9- Nov Moon, crust, mantle, atmosphere

More information

Earth. Interior Crust Hydrosphere Atmosphere Magnetosphere Tides

Earth. Interior Crust Hydrosphere Atmosphere Magnetosphere Tides Earth Interior Crust Hydrosphere Atmosphere Magnetosphere Tides Semi-major Axis 1 A.U. Inclination 0 Orbital period 1.000 tropical year Orbital eccentricity 0.017 Rotational period 23 h 56 min 4.1 s Tilt

More information

Activity 1-2: Origin of the Earth

Activity 1-2: Origin of the Earth Earth Science 11 Name: Block: Activity 1-2: Origin of the Earth Read the following passage, and then answer the questions at the end: Where Earth Science Begins: The Solar System Where shall the study

More information

http://eps.mcgill.ca/~courses/c220/ Nucleosynthesis neutron electron + proton = é + H + t 1/2 = 12 minutes H + + neutron Deuterium (D) 2 H + + neutrons Helium (He) 3 H + + neutrons Lithium (Li) From: W.S.

More information

Radiogenic Isotopes. W. F. McDonough 1 1 Department of Earth Sciences and Research Center for

Radiogenic Isotopes. W. F. McDonough 1 1 Department of Earth Sciences and Research Center for Radiogenic Isotopes W. F. McDonough 1 1 Department of Earth Sciences and Research Center for Neutrino Science, Tohoku University, Sendai 980-8578, Japan (Dated: May 17, 2018) I. SUMMRY Isotope systems

More information

PTYS/ASTR Section 2 - Spring 2007 Practice Exam 2

PTYS/ASTR Section 2 - Spring 2007 Practice Exam 2 PTYS/ASTR 206 - Section 2 - Spring 2007 Practice Exam 2 Note: The exam is scheduled for Thursday, March 29, 2007. It will be held in-class; you will have 75 minutes to finish the exam, though many of you

More information

EASC100: EXAM1 (07) Lithosphere and Hydrosphere

EASC100: EXAM1 (07) Lithosphere and Hydrosphere EASC100: EXAM1 (07) Lithosphere and Hydrosphere Name: 1. Why do Mercury and the Moon lack an atmosphere? A) They formed after all the gas had been used up. B) They are so cold that all their gases have

More information

APPLICATIONS OF ISOTOPES TO IGNEOUS PETROGENESIS

APPLICATIONS OF ISOTOPES TO IGNEOUS PETROGENESIS APPLICATIONS OF ISOTOPES TO IGNEOUS PETROGENESIS Elisabeth Widom Miami University, Oxford, Ohio, USA Keywords: cosmogenic nuclides, crustal recycling, decay series, fractionation, igneous petrology, isochron,

More information

37. Planetary Geology p

37. Planetary Geology p 37. Planetary Geology p. 656-679 The Solar System Revisited We will now apply all the information we have learned about the geology of the earth to other planetary bodies to see how similar, or different,

More information

GEOLOGY FOR MINING ENGINEERS. Prof.Dr.Kadir DİRİK Lecture Notes 2015

GEOLOGY FOR MINING ENGINEERS. Prof.Dr.Kadir DİRİK Lecture Notes 2015 GEOLOGY FOR MINING ENGINEERS Prof.Dr.Kadir DİRİK Lecture Notes 2015 THE SCIENCE OF GEOLOGY GEOLOGY is the study of the Earth, including the materials that it is made of, the physical and chemical changes

More information

Today. Events Homework DUE next time. Terrestrial Planet Geology - Earth. Terrestrial Planet Atmospheres

Today. Events Homework DUE next time. Terrestrial Planet Geology - Earth. Terrestrial Planet Atmospheres Today Terrestrial Planet Geology - Earth Terrestrial Planet Atmospheres Events Homework DUE next time Venus Surface mapped with radar by Magellan orbtier https://www.youtube.com/watch?v=ub_bbs_oh_c Continental

More information

Next opportunity to observe the Moon and Venus close together: Dec. 31, Announcements

Next opportunity to observe the Moon and Venus close together: Dec. 31, Announcements Announcements Last OWL homework: due 12/15 before midnight Study guide for final exam is up on the class webpage Practice exam up Thursday afternoon Final exam: Monday, Dec. 15, 10:30 AM, Hasbrouck 20

More information

Big Idea Clarifying Statement Assessment boundary

Big Idea Clarifying Statement Assessment boundary Energy Big Idea Clarifying Statement Assessment boundary HS-PS3-1. Create a computational model to calculate the change in the energy of one component in a system when the change in energy of the other

More information

Grade 8 Learning Objectives MS-PS2-4.

Grade 8 Learning Objectives MS-PS2-4. MS-PS2-4. Construct and present arguments using evidence to support the claim that gravitational interactions are attractive and depend on the masses of interacting objects. [Clarification Statement: Examples

More information

Grades 9-12: Earth Sciences

Grades 9-12: Earth Sciences Grades 9-12: Earth Sciences Earth Sciences...1 Earth s Place in the Universe...1 Dynamic Earth Processes...2 Energy in the Earth System...2 Biogeochemical cycles...4 Structure and Composition of the Atmosphere...4

More information

Directed Reading. Section: Volcanoes and Plate Tectonics

Directed Reading. Section: Volcanoes and Plate Tectonics Skills Worksheet Directed Reading Section: Volcanoes and Plate Tectonics 1. What can cause some of the most dramatic changes to Earth s surface? a. solar activity b. tides c. geysers d. volcanic eruptions

More information

PUBLICATIONS. Geochemistry, Geophysics, Geosystems

PUBLICATIONS. Geochemistry, Geophysics, Geosystems PUBLICATIONS Geochemistry, Geophysics, Geosystems RESEARCH ARTICLE 10.1002/2014GC005566 Key Points: MORB fission Xe isotopes indicate MORB source is more degassed than plume source Recycled atmospheric

More information

Rocks and the Rock Cycle. Banded Iron Formation

Rocks and the Rock Cycle. Banded Iron Formation Rocks and the Rock Cycle Banded Iron Formation Rocks Big rocks into pebbles, Pebbles into sand. I really hold a million, million Rocks here in my hand. Florence Parry Heide How do rocks change? How are

More information

C. Because the Moon was formed after a Mars-sized bolide hit the Earth about 4.5b.y. This means the Earth must have been formed before it was hit

C. Because the Moon was formed after a Mars-sized bolide hit the Earth about 4.5b.y. This means the Earth must have been formed before it was hit 1. Why do we say that the Earth is older than the Moon yet the oldest rock found in the Earth (Gneiss Complex near Great Slave Lake - 4.03b.y.) is younger than the Moon (4.47b.y.)? A. Because the Moon

More information

Lecture 20. Origin of the atmosphere (Chap. 10) The carbon cycle and long-term climate (Chap. 8 of the textbook: p )

Lecture 20. Origin of the atmosphere (Chap. 10) The carbon cycle and long-term climate (Chap. 8 of the textbook: p ) Lecture 20 Origin of the atmosphere (Chap. 10) The carbon cycle and long-term climate (Chap. 8 of the textbook: p.158-170) end of last ice-age; begin civilization beginning of modern era of ice-ages asteroid

More information

Chapter 9 Lecture. The Cosmic Perspective Seventh Edition. Planetary Geology: Earth and the Other Terrestrial Worlds Pearson Education, Inc.

Chapter 9 Lecture. The Cosmic Perspective Seventh Edition. Planetary Geology: Earth and the Other Terrestrial Worlds Pearson Education, Inc. Chapter 9 Lecture The Cosmic Perspective Seventh Edition Planetary Geology: Earth and the Other Terrestrial Worlds Planetary Geology: Earth and the Other Terrestrial Worlds 9.1 Connecting Planetary Interiors

More information

Marine Sediments EPSS15 Spring 2017 Lab 4

Marine Sediments EPSS15 Spring 2017 Lab 4 Marine Sediments EPSS15 Spring 2017 Lab 4 Why Sediments? Record of Earth s history - Tectonic plate movement - Past changes in climate - Ancient ocean circulation currents - Cataclysmic events 1 Classification

More information