History of the Earth Chapter 1: Formation of the EarthFrom the Big Bang to Early PlanetsOrigins 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)Origin of the Universe (13.7 Gyr)TheBig BangQuantum Mechanical Statistical Vacuum Fluctuation?History of the UniverseHubble Deep FieldOrigin Answer came from Distance vs.Relative Velocity of galaxiesDistance to GalaxiesDistanceActualBrightnessObservedBrightnessMeasured in:Light Years ~ 10 trillion km Parsec ~3.25 light yearsHow do we Know Distance?Velocity comes fromDoppler EffectElectromagnetic RadiationDoppler EffectDoppler Effect:Red Shift&Blue ShiftRed Shift of SpectrumslowfastnearfarGalaxiesHubble lawGalaxy VelocityMore Red ShiftedExpansion of the UniverseThe galaxies are not moving through space, they are stationary is space. Space itself, between the galaxies is stretching and carrying the galaxies farther away from each other.History of the UniverseWMAPWilkinson Microwave Anisotrophy Probe Microwave light emitted 380,000 yrs after the Big BangStars Begin to Form about 300,000 years after the Big BangAt that time Universe is:• 75% Hydrogen• 25% HeliumWhat about the rest of the elements?NebulaHow a Star WorksRadiationPressureGravityNucleosynthesisStellar Death: CollapseRadiationPressureGravitySupernova: Crab NebulaSupernova RemnantsOrigin 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: SupernovaOrigin of the Solar System:The Data1. 99% of the mass of the solar system is in the sun2. We know thecomposition of the sun3. Planets orbit the sun in the plane of the sun’s equator4. Planets come in two groups:Terrestrial PlanetsMercury Venus EarthMars - Small, Dense and made of Rock and Iron4. Planets come in two groups:Jovian PlanetsJupiterSaturnUranusNeptune- Large, Low Density, and Made of Gas and IceAsteroidsMathilde & Eros (NEAR)Ida & DactylKuiper Belt & Pluto5. MeteoritesChondritesCarbonaceousOrdinaryChondrules under a scopeX-Ray ImageAbundance of Elements in Carbonaceous ChondritesAchondrite - Stony MeteroriteA stone from the Stannern eucrite showerthat fell over Moravia, Czech Republic in 1808.Iron MeteoriteStony-Iron:PalasiteOlivineIron6. Properties of the EarthOrigin of the Solar System:InterpretationSolar Nebula Hypothesis1. Start With a NebulaSomething (Supernova?) Triggers Nebula to CollapseEagle Nebula2. Nebula Collapses to form Protostar (Early Sun)Protostar Formation3. Residual Material Begins to Cool and Accrete3a. “Gas” Segregated by Melting Temperature and Condenses3b. Accretion: Dust Particles Accrete into Planetesimals3b. Planetesimals Accrete into PlanetsDaDa! - A Solar SystemDust Disks Around Young StarsExtrasolar PlanetsFirst Extra-Solar Planet Photographed (2005)4. Terrestrial Planets Heat up and Differentiate:Iron CatastropheHeat Comes From:1. Kinetic Energy of Accretion2. Gravitational Energy3. Radioactive Decay4. DifferentiationEarth’s InteriorMeteorite SourcesMeteorites & 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 MyrsEarth in the Early Hadean?2004 - Fred
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