history of the earth chapter 1: formation of the earth from the big bang to early planets
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History of the Earth Chapter 1: Formation
of the Earth
From the Big Bang to Early Planets
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Origins of…• The Universe (13.7 Gyr)
• The Elements (13.7 - 4.6 Gyr)• The Solar System & the Earth (4.6 Gyr)
• The Moon (4.5-4.6 Gyr)
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Hubble Deep Field
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Origin of the Universe (13.7 Gyr)
TheBig Bang
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WMAPWilkinson Microwave Anisotrophy
Probe
Microwave light emitted 380,000 yrs after the Big Bang
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History of the Universe
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Stars Begin to Form about 300,000 years after the Big Bang
At that time Universe is:• 75% Hydrogen• 25% Helium
What about the rest of the elements?
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Nebula
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How a Star Works
RadiationPressure
Gravity
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Nucleosynthesis
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Stellar Death: Collapse
RadiationPressure
Gravity
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Supernova: Crab Nebula
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Supernova Remnants
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Eagle Nebul
a
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Origin of the Elements
• Hydrogen & Helium: Big Bang
• Helium to Iron: Stellar Fusion Multiples of 4 most common:
Helium Carbon, Oxygen, Neon, Magnesium, Silicon, Sulfur, Iron
• Iron to Uranium: Supernova
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Origin of the Solar System:The Data
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1. 99% of the mass of the solar system is in
the sun
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2. We know thecomposition of the sun
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3. Planets orbit the sun in the plane of the sun’s equator
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4. Planets come in two groups:
Terrestrial Planets
Mercury Venus Earth Mars
- Small, Dense and made of Rock and Iron
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4. Planets come in two groups:
Jovian Planets
Jupiter Saturn
Uranus Neptune
- Large, Low Density, and Made of Gas and Ice
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Asteroids
Mathilde & Eros (NEAR)
Ida & Dactyl
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Kuiper Belt & Pluto
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5. Meteorites
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Chondrites
Carbonaceous
Ordinary
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Chondrules under a scope
X-Ray Image
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Abundance of Elements
in Carbonaceou
s Chondrites
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Achondrite - Stony Meterorite
A stone from the Stannern eucrite showerthat fell over Moravia, Czech Republic in 1808.
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Iron Meteorit
e
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Stony-Iron:
PalasiteOlivine
Iron
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6. Properties of the Earth
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Origin of the Solar System:InterpretationSolar Nebula Hypothesis
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1. Start With a Nebula
Something (Supernova
?) Triggers Nebula to Collapse
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2. Nebula Collapses to form Protostar (Early
Sun)
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Protostar Formation
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3. Residual Material Begins to Cool and
Accrete
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3a. “Gas” Segregated by Melting Temperature
and Condenses
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3b. Accretion: Dust Particles Accrete into
Planetesimals
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3b. Planetesimals Accrete into Planets
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DaDa! - A Solar System
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Dust Disks Around Young Stars
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Extrasolar
Planets
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First Extra-Solar Planet
Photographed
(2005)
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4. Terrestrial Planets Heat
up and Differentiat
e:Iron
CatastropheHeat Comes From:1. Kinetic Energy of Accretion2. Gravitational Energy3. Radioactive Decay4. Differentiation
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Earth’s
Interior
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Meteorite Sources
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Meteorites & Solar System Age
•Formation: 4.56 billion yearsMeteorites all with 20 myrs(earliest within few Myrs of supernova)
•Supernova to sun and planetesimals - few million years! •Layered earth about 96±12 Myrs after meteorites•Nebula to layered earth & moon - about 100 Myrs
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Earth in the Early Hadean?
2004 - Fred Sulahria