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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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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 the composition 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 MercuryVenusEarth 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 Carbonaceous Chondrites
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Achondrite - Stony Meterorite A stone from the Stannern eucrite shower that fell over Moravia, Czech Republic in 1808.
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Iron Meteorite
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Stony-Iron: Palasite Olivine Iron
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6. Properties of the Earth
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Origin of the Solar System: Interpretation Solar 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 Differentiate: Iron Catastrophe Heat Comes From: 1.Kinetic Energy of Accretion 2.Gravitational Energy 3.Radioactive Decay 4.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 years Meteorites 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
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