The Earth is differentiated

Slides:

Advertisements

Similar presentations

Interior structure, origin and evolution of the Moon Key Features of the Moon: pages

Advertisements

The nebular hypothesis

Mantle composition 1800s meteorites contain similar minerals to terrestrial rocks Hypothesis that meteorites come from asteroid belt and originate from.

Solar System Formation – Earth Formation Layers of the Earth Review.

History of “primordial” Pb Meteorite samples Chondrite – a primitive, undifferentiated meteorite CI refers to a particular class of carbonaceous chondrite.

Anne M. Hofmeister and Robert E. Criss

Open Questions in Geosciences Collaborators: - Ricardo Arévalo, Mario Luong : UMD - Kevin Wheeler, Dave Walker : Columbia Univ - Corgne, Keshav & Fei :

Other clues to the formation of the Solar System Inner planets are small and dense Outer planets are large and have low density Satellites of the outer.

Earth’s Energy Equation, simplified Q surface ≈ H radioactive + H mantle secular cooling + Q core Q surface ≈ 44 TW (surface heat flow measurements) H.

Pt. II: Oxygen Isotopes in Meteorites Stefan Schröder February 14, 2006 Lecture Series “Origin of Solar Systems” by Dr. Klaus Jockers.

Micro fossil in a meteorite ? (R. Hoover 2011). Lecture 7: Geologic History of Life Oldest signatures of life in sedimentary rocks: Microfossils Molecular.

Emil Johann Wiechert In 1897, Earth’s 1 st order structure -- silicate shell surrounding metal core.

Wee Rocky Droplets in Comet Dust Comet dust collected by the Stardust mission Small samples (10-40 microns)

How did the Solar System form? 3. What are the broad general characteristics or physical features of our Solar System and how do they illuminate Solar.

 Satellites – natural or artificial bodies that revolve around larger bodies such as planets.

Lecture 3 – Planetary Migration, the Moon, and the Late Heavy Bombardment Abiol 574.

Basic Structure of the Earth

ICES OF THE SATURN SYSTEM ICES OF THE SATURN SYSTEM V.A. Dorofeeva Vernadsky Institute of Geochemistry and Analytical Chemistry RAS, Russia.

Earth and Other Planets Chapter 16 Great Idea: Earth, one of the planets that orbit the Sun, formed 4.5 billion years ago from a great cloud of dust.

Hadean Eon & the formation of Earth

Structure of the Earth. Gravity reshapes the proto-Earth into a sphere. The interior of the Earth separates into a core and mantle. Forming the planets.

Natural Disasters Earth’s Internal Structure Introduction to Plate Tectonics Earth’s Energy Sources and Systems.

Slide 1 Observations/Inferences: Rocky inner, icy outer solar system Asteroid differentiation temperatures heliocentrically distributed Gross zonal structure.

Earth's Internal Structure → Layers core mantle crust These are identified using seismic waves p-waves & s-waves.

Carbon in the Earth’s core Yingwei Fei Geophysical Laboratory Carnegie Institution of Washington.

Hadean plate tectonics – fact or fiction? Martin J.Whitehouse Swedish Museum of Natural History, Stockholm, Sweden Penrose, June 2006.

Chapter 8: Terrestrial interiors. Interiors How might we learn about the interior structure of the Earth, or other planets?  What observations can you.

Asteroids (in space) and Meteorites (once they have entered the atmosphere) Meteorites hit the atmosphere with speeds from 12 to 72 km/s. Earth’s orbital.

Earth Formation and Structure. Early Earth: Age and Formation Condensed from solar nebula 4.6 billion years ago along with the rest of the planets in.

Earth Structure broadest view: 1) solid Earth and 2) atmosphere atmosphere primarily composed of nitrogen (78%) and oxygen (21%) important gas CO 2 = 0.03%--for.

STRUCTURE OF THE EARTH. Differentiation of Earth Earth is divided into layers based on density and composition Solid Layers – Core (iron-nickel) – Mantle.

SIO224 Internal Constitution of the Earth Fundamental problem: the nature of mass and heat transfer in the mantle and the evolution of the Earth.

E. M. Parmentier Department of Geological Sciences Brown University in collaboration with: Linda Elkins-Tanton; Paul Hess; Yan Liang Early planetary differentiation.

The Sun & The Solar System. Structure of the Sun The Sun has layers which can be compared to the Earth’s core, mantle, crust, and atmosphere All of these.

Formation of the Universe and Earth’s Interior 1.

Structure of the Earth and Mineralogy Environmental Science Earth Science Unit Environmental Science Earth Science Unit.

Structure and chemistry of the Earth Today’s topic: The chemistry of Earth’s mantle and crust.

Magma Oceans in the Inner Solar System Linda T. Elkins-Tanton.

Importance of tighter constraints on U and Th abundances of the whole Earth by Geo-neutrino determinations Shun’ichi Nakai ERI, The University of Tokyo.

Nucleosynthetic processes: Fusion: Hydrogen Helium Carbon Oxygen After Fe, neutron addition takes place (rapid and slow processes)

…and how we know it today. How Did the Earth Form?  KMR0nx8&feature=related KMR0nx8&feature=related.

Slide 1 Pre Type II Nucleosynthesis (s-process) 21 solar mass star ratio to solar abundance Rauscher et al. (2002)

Slide 1 The Earth is differentiated How and When did this occur? Two Sets of Constraints: Physical Mechanisms and Chemical Signatures.

Jeff Taylor Ages of Highland Rocks1 Ages of Pristine Highlands Rocks Ages of lunar rocks informative about: –Timing of magma ocean crystallization –Timescales.

The Core-Mantle Boundary Region Jeanloz & Williams, 1998 Lower mantle Outer core CMB Heat flow.

1. Inner Core Outer Core Mantle Crust 2  The Earth's outermost surface is called the crust. The crust is typically about 25 miles thick beneath continents,

Signatures of Early Earth Differentiation in the Deep Mantle?

Notes: Earth/Moon Formation 3/11. 1.Explain the three sources of heat that contributed to the high temperature of the newly formed Earth. (p. 688). The.

Solar System.  Nebular Hypothesis: Solar System was produced by the gravitational collapse of a gas cloud – the remnant of a supernova explosion.  Concentration.

Earth’s Interior “Seeing into the Earth”

Theories of Formation for the Moon

Origin of the solar system Solar Systems Form by Accretion Let us study the sequence in slightly more detail: The processes by which.

Origin of the Moon 22 September 2017.

Pt. II: Oxygen Isotopes in Meteorites

SIO224 Internal Constitution of the Earth

Water in Asteroid 4 Vesta

Origin of the Moon 13 February 2018.

Crust and mantle are solid rock not liquid

Interior of the Earth Lecture #3.

Geology Thinking Sheet 11/29/17 or 11/30/2017

Geology Thinking Sheet 12/1/17 or 12/4/17

The Earth is differentiated

Compositional Balancing Before Moon Formation

Lunar Interior Magnetic Sounding

Origin of the Moon 11 September 2018.

Structure of the Earth.

SATISH PRADHAN DNYANASADHANA COLLEGE,THANE

Stochastic Late Accretion on the Earth, Moon and Mars

The Moon Topographic map from Lunar Reconnaissance Orbiter.

Presentation transcript:

The Earth is differentiated How and When did this occur? Two Sets of Constraints: Physical Mechanisms and Chemical Signatures

Observations/Inferences: Rocky inner, icy outer solar system Asteroid differentiation temperatures heliocentrically distributed Gross zonal structure within asteroid belt preserved The Moon had a magma ocean The solar photosphere has a composition very similar to CI carbonaceous chondrites Heat source concentrated near Sun? or Longer times to accrete object farther from the sun (less Al heating)? 26

Solar/Magnetic Induction heating (but T-Tauri: Polar Flows) Heat Sources: Solar/Magnetic Induction heating (but T-Tauri: Polar Flows) Short-lived radioisotopes ( 26 Al 0.73 Ma half life: must accrete fast) Long-lived radioisotopes (U, Th, K) (slow, only for larger bodies) Large impacts (only for larger bodies: between Moon and Mars-sized) Potential energy of core formation (larger bodies: 6300 km radius: 2300°C rise, 3000 km radius: 600°C rise) Resonant tidal heating (Only moons: Moon?, Titan, Io, Europa)

Timing of Core formation

Two Possible Mechanisms to Separate Metal from Silicate Porous Flow Immiscible Liquids and Deformation

Dihedral (wetting) Angle Theory The Dihedral Angle Theta is a force balance between interfacial energies

Sulfide Melt in an Olivine Matrix Most Fe-Ni-S melts do not form interconnected melt channels

Samples Recording Planetary Differentiation

Pallasites: Asteroid Core-Mantle Boundary Brenham

Old Lunar Highland Crust

An Oblique Collision between the proto-Earth and a Mars-sized impactor 4.2 minutes 8.4 minutes 12.5 minutes Kipp and Melosh (86), Tonks and Melosh (93)

Magma Ocean Crystallization No Crystal Settling Crystal Cummulates 15 22.5 7.5 15 22.5 7.5 t Quench Crust Quench Crust Liquid Pressure Depth Pressure GPa Liquid km GPa 250 Dunite High Mg/Si Liquid 500 Perovskite Settling Low Mg/Si 750 Cummulates should give a chemical signature after Carlson, 1994

Lower Mantle Solidus Pressure (GPa) 2000 T e m p r a t u ( K ) 3000 Diamond Anvil Peridotite Solidus Pressure (GPa) 2000 T e m p r a t u ( K ) 3000 4000 5000 20 40 80 120 CMB M n l A d i b s o Olivine shock meltin g n g e l t i m e ü s t i t w e s i o g n n d ) Core T M a o u r b p p e s ( u d u Multianvil Peridotite Solidus Zerr et al (98), Holland & Ahrens (97)

Useful Isotope Systems Parent nuclide 182Hf 146Sm 147Sm 176Lu 187Re 232Th 235U 238U Daughter nuclide 182W 142Nd 143Nd 176Hf 187Os 208Pb 207Pb 206Pb Tracer ratio (daughter/stable) 182W/184W 142Nd/144Nd 143Nd/144Nd 176Hf/177Hf 187Os/188Os 208Pb/204Pb 207Pb/204Pb 206Pb/204Pb Half-life 9 Ma 103 Ma 106 Ga 35.9 Ga 42.2 Ga 14.01 Ga 0.7038 Ga 4.468 Ga

Short Lived Isotopes: Early Solar System Gilmore (2002) Science

Oxygen d-Notation A scaled deviation from a standard 18O/16Osample - 18O/16OSMOW d18O = X 1000 18O/16OSMOW SMOW: Standard Mean Ocean Water abundance 16O 99.76% 17O 0.037% 18O 0.200%

Sulfur d-Notation A scaled deviation from a standard 33S/32Ssample - 33S/32SCDT d33S = X 1000 33S/32SCDT CDT: Canyon Diablo Troilite abundance 32S 95% 33S 0.75% 34S 4.2% 36S 0.017%

Mass-Dependent Fractionation Wiechert et al (2001) Science 294: 345