Environmental Processes and Hazards: Formation, Structure, and Composition of Earth

Formation, Structure and Composition of Earth

Recommended Literature

  • "Understanding Earth" by Grotzinger & Jordan (2014). Older editions are also acceptable (Press and Sievers).

  • "Earth's Climate: Past and Future" by Ruddiman (2013 or 2008).

Formation of Earth

  • Earth formed approximately 4.6 billion years ago, likely from a supernova.

  • First chemical elements originated during the Big Bang, about 13.8 billion years ago.

Origin of Elements (Nucleosynthesis)
  1. Primordial period (Big Bang nucleosynthesis) - approximately 3 minutes after the Big Bang.

  2. Stellar nucleosynthesis - approximately 200 million years after the Big Bang.

  3. Supernova nucleosynthesis - approximately 9.2 billion years after the Big Bang.

1. Primordial Period: Formation of the Universe
  • "Big Bang": Occurred approximately 13.8 billion years ago.

    • The universe expanded from a primordial point in a cataclysmic explosion.

    • As the universe expanded and cooled, physical laws (gravity, magnetism) developed, and matter and energy formed and differentiated.

  • Theory: Based on the observed expansion of the Universe.

“Big Bang” Nucleosynthesis
  • Cosmos underwent an "inflation," expanding from the size of an atom to a melon in 103410^{-34} seconds.

  • Post-inflation: Cosmos filled with hot particles (quarks, leptons, photons, neutrinos) that formed the first matter.

Formation of Protons and Neutrons
  • Rapid cooling (10-6 seconds after “Big Bang”) allowed quarks to form protons and neutrons.

    • Proton (Hydrogen): Composed of 2 up quarks and 1 down quark.

    • Neutron: Composed of 1 up quark and 2 down quarks.

Formation of First Atomic Nuclei
  • Occurred during the first 2 minutes of the Universe.

    • Hydrogen (1H1H).

    • Deuterium (2H2H or D).

    • Tritium (3H3H or T).

    • Helium (3He3He and 4He4He).

  • Unstable nuclei like 5Li5Li, 5He5He, and 8Be8Be formed during the first 3 minutes but decayed back to stable 4He4He.

  • Stable hydrogen atoms formed approximately 700,000 years after the Big Bang.

2. Stellar Nucleosynthesis
  • Nebulas of Hydrogen and Helium atoms gravitationally collapsed to form the first stars and galaxies about 200 million years after the Big Bang.

  • This process generated heat and energy, fueling further fusion reactions.

Helium Fusion / Triple-alpha process
  • Helium accumulated in the cores of stars.

  • Further nuclear fusion reactions formed Beryllium (Be), Carbon (C), and Oxygen (O).

  • This released energy, powering further fusion.

  • Lighter elements (Hydrogen) diffuse to the rim, while heavier elements (Helium) concentrate in the center. This process begins at 170 million degrees Celsius.

  • White Dwarfs: Most smaller stars do not form other elements at this stage.

  • Larger Stars (700 million degrees Celsius): Heavier elements concentrate in the center, while lighter elements (gas) diffuse to the rim.

    • Magnesium and Oxygen form if the star is more than eight times as massive as the Sun.

  • Larger Stars (2 billion degrees Celsius)

  • Larger Stars (>3 billion degrees Celsius): Silicon and Sulphur atoms fuse into Iron (lasts about a day).

    • Iron cannot be fused any further due to its atomic structure.

  • Larger Stars (>100 billion degrees Celsius): Gravitational collapse occurs, and the star detonates in a cataclysmic explosion (Supernova).

3. Supernova Nucleosynthesis
  • Explosion of a giant star generates high temperatures and pressures, causing nuclear fusion reactions that create elements with atomic numbers 27-92 (greater than Iron).

  • Supernovas produce interstellar clouds of gas and dust containing a wide range of elements due to nuclear fusion.

Formation of the Solar System (4.6 Billion Years Ago)

  • A diffuse, slowly rotating nebula begins to contract.

  • The enveloping disk of gas and dust forms grains that collide and clump together into planetesimals.

  • Matter concentrated at the center becomes the Protostar (our Sun).

  • Planetesimals, approximately 1 km in size, form.

  • A flat, rapidly rotating disk forms.

Formation of Planets
  • Solid Planets: Mercury, Venus, Earth, Mars (Inner Planets).

  • Gas Giants: Jupiter, Saturn (primarily hydrogen and helium).

  • Outer Planets: Uranus, Neptune, Pluto.

  • Asteroid belt.

Earth’s Structure and Composition

  • Proto-Earth (4.6 billion years ago) differentiated into layers to form Earth as a zoned planet.

  • Iron sank to the center, and lighter material floated upward.

    • Crust: 0-40 km.

    • Mantle: 40-2890 km.

    • Liquid iron outer core: 2890-5150 km.

    • Solid iron inner core: 5150-6370 km.

Today’s Earth: Heat and Energy Balance
  • Earth’s outer core is slowly cooling down (100 degrees Celsius per billion years).

Earth's Layers
  • Layers subdivided based on seismic waves.

  • Crust: 0-100 km thick.

  • Lithosphere: Crust and uppermost solid mantle.

  • Asthenosphere: Top layer of the mantle consisting of hot, weak rock that is easily deformed.

  • Mantle: 2900 km.

  • Outer core: Liquid, 5100 km.

  • Inner core: Solid, 6378 km.

Note: Diagrams presented are not to scale.

Evidence from Seismic Studies
  • Earthquakes produce P (primary) and S (secondary) waves that penetrate Earth’s layers with different velocities depending on material density.

  • Moho (Mohorovicic Discontinuity): Separates the crust from the underlying mantle.

  • Different densities indicate different material/chemical compositions.

Earth Chemical Composition: Evidence from Geochemical Studies
  • Evidence from ore smelting slags and meteorites.

  • Melting a chondrite (extra-terrestrial rock/meteorite) yields 3 immiscible liquids plus vapor:

    • Gas Phase (Atmophile/volatile): H, He, N, Noble gases.

    • Silicate Liquid (Lithophile): Alkalis, Alkaline Earths, Halogens, B, O, Al, Si, Sc, Ti, V, Cr, Mn, Y, Zr, Nb, Lanthanides, Hf, Ta, Th, U.

    • Sulfide Liquid (Chalcophile): Cu, Zn, Ga, Ag, Cd, In, Hg, Tl, As, S, Sb, Se, Pb, Bi, Te.

    • Metallic Liquid (Siderophile): Fe, Co, Ni, Ru, Rh, Pd, Os, Ir, Pt, Mo, Re, Au, C, P, Ge, Sn.

Composition of the Core
  • Inner Core (Solid, 1230-1530 km thick, 5430°C):

    • Iron (Fe): ~80%.

    • Nickel (Ni): ~12%.

    • S, O, siderophile elements: ~8%.

  • Outer Core (Liquid, 2250 km thick, 2730–4230°C):

    • Molten Fe: ~85%.

    • Some Ni.

    • Some Si, S, C, or O.

  • Convection in the liquid outer core and spin of the solid inner core generate Earth’s magnetic field.

  • The magnetic field is also evidence for a dominantly iron core.

Earth’s Magnetic Field
  • Generation: Electrical currents flowing in the slowly moving molten iron of the fluid outer core.

  • Mechanism: Rotation of Earth on its axis causes these electric currents to form a magnetic field.

  • Extent: Extends several tens of thousands of kilometers into space.

  • Protection: Protects Earth from charged particles of the solar wind and cosmic rays (harmful ultraviolet radiation).

Composition of the Mantle
  • Mantle makes up >2/3 of Earth’s mass (4000-1400°C).

  • Composition of the upper mantle (Asthenosphere) is approximated by pyrolite, a theoretical igneous rock consisting of about three parts of peridotite and one part of tholeiitic basalt.

    • SiO2SiO_2: 45 wt%

    • MgOMgO: 30-40 wt%

    • FeOFeO: 8-13 wt%

    • Al<em>2O</em>3Al<em>2O</em>3: 3 wt%

    • CaOCaO: 3 wt%

    • High Mn, Cr, Ti concentrations

The Lithosphere
  • Earth’s hard and rigid outer layer.

  • Two types of crusts (depending on rock density):

    • Lighter, more silicic (felsic) continental crust.

    • Heavier, less silicic (mafic) oceanic crust.

Average Composition of the Crust
  • Oxygen: 47 wt%

  • Silicon: 28 wt%

  • Aluminum: 8.1 wt%

  • Iron: 5.0 wt%

  • Calcium: 3.6 wt%

  • Sodium: 2.8 wt%

  • Potassium: 2.6 wt%

  • Magnesium: 2.1 wt%

  • Others: 0.8 wt%

Composition of the Continental Crust
  • Felsic: SiO2SiO_2 concentrations between 52 and 77 wt% (composition of igneous rocks “Andesite/Diorite” and “Rhyolite/Granite”).

Composition of the Oceanic Crust
  • Mafic: SiO2SiO_2 concentrations between 48 and 52 wt% (composition of igneous rock "Basalt/Gabbro").

Plate Tectonics

The Shape of the Lithosphere
  • Typical elevation of land surface: 0-1 km.

  • Typical depth of ocean: 4-5 km.

  • Examples: Himalayan Mountains, Marianas Trench.

Mantle Convection
  • Mantle convection causes the break-up of the lithosphere into several tectonic plates.

  • Stratified Convection Boundary near 700 km separates the two convection systems.

Earth’s Tectonic Plates
  • 7 large plates and several smaller and micro plates.

  • Composed of both continental and oceanic crust.

Processes at Plate Boundaries
  • Divergent: Plates drift apart from each other (constructive).

  • Convergent: Plates collide with each other (destructive).

  • Transform: Plates slide past one another.

Divergent Boundaries
  • Oceanic Plate Separation: Mid-Ocean Ridge (MOR).

    • Volcanoes and earthquakes concentrate.

    • Most Transform faults are found in the ocean basin and connect offsets in the mid-ocean ridges.

  • Continental Plate Separation: Parallel valleys, volcanoes, and earthquakes.

    • Example: East African Rift Valley.

Convergent Boundaries
  • Ocean-Continent Convergence: Subduction zone.

    • A volcanic arc of mountains forms.

    • Shallow and deep earthquakes occur.

    • Example: Andes Mountains, Peru-Chile Trench.

  • Ocean-Ocean Convergence: Deep-sea trench, volcanic island arc.

    • Deep and shallow earthquakes occur.

    • Example: Mariana Islands, Mariana Trench.

  • Continent-Continent Convergence: Crust crumbles, creating high mountains and a wide plateau.

    • Example: Himalayas.

    • Main thrust fault, Tibetan Plateau, Eurasian Plate.

The Rock Cycle
  • Deposition of sediment -> Sedimentary rock -> Burial & Compaction -> Deformation & Metamorphism -> Metamorphic rock -> Melting -> Magma -> Crystallization of Magma -> Igneous rock -> Weathering of rocks at surface -> Erosion & Transport

The Theory of Continental Drift (Plate Tectonics)
  • Alfred Wegener (German meteorologist, 1880-1930).

Evidence of Past Plate Motions
  1. Fit of the continents and similarity of rock assemblages.

  2. Similarity of geological sequences on the different continents.

  3. The fossil record.

    • South America and Africa: Cynognathus, Mesosaurus, Lystrosaurus, Glossopteris.

  4. Evidence of similar climate zones.

    • Pioneering paleoclimatic and paleoenvironmental reconstructions.

  5. Hot spots.

    • Rate = distance/age difference = distance/timedistance/time.

Tectonic Plates - Modern Rates of Motion (cm/year)
  • Rates vary for different plates (e.g., Pacific Plate, North American Plate).

Exercise 2: Past Plate Motion Rates
  • Calculations based on distances and ages on the map involving the Emperor Seamount Chain and Hawaiian Ridge. This allows past plate motion rates to be determined by distance/timedistance/time.