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GY111 Physical Geology GY111 Physical Geology

GY111 Physical Geology - PowerPoint Presentation

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GY111 Physical Geology - PPT Presentation

Solar System Nebular Hypothesis Nebular Hypothesis Solar System was produced by the gravitational collapse of a gas cloud the remnant of a supernova explosion Concentration of heavy elements in inner ID: 571985

earth mars system early mars earth early system solar earth

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Slide1

GY111 Physical Geology

Solar SystemSlide2

Nebular Hypothesis

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

Concentration of heavy elements in inner planets.Most of the mass of the Solar System is composed of H and He atoms.Slide3

Planets of the Solar System

Inner (Terrestrial) Planets: Mercury, Venus, Earth, Mars.

Outer (Jovian) Planets: Jupiter, Saturn, Uranus, Neptune.Pluto: former moon of Neptune.Asteroid belts: shattered remains of a proto-planet.Slide4

Inner (Terrestrial) Planet Characteristics

Metallic Core and rocky (silicate) mantle/crust.

Thin atmospheres because of proximity to Sun.Very small moons because of low gravitational attraction (Earth being a notable exception).Asteroid belt probably represents a failed planet formation from early in the Hadean Eon.Density is high – averaging approximately 5.0.Slide5

Outer (Jovian) Planet Characteristics

Thick gaseous atmospheres dwarf a small metallic/silicate core/mantle/crust.

Atmospheric gas is retained because of distance from the sun.Intense gravitational fields can capture large comets or planets. This protects the inner planets from impacts.Overall density is low – Saturn has a density < 1.0.Slide6

Earth’s Early HistorySlide7

Early Impactor Hypothesis

Mars-sized (33% mass of Earth) impactor collided during the Hadean.

Isotopic signatures on Earth and Moon are very similar.Earth’s gravity would not have been able to capture a mass as large (25% of Earth) as our moon.The melting event triggered by the impact allowed Earth to differentiate into Crust, Mantle, and Core.Slide8

Differentiated Earth

Fe-rich core.

Silicate mantle and crust.Differentiation makes possible plate tectonics and the magnetic field of the Earth.Slide9

Earth’s Early Atmosphere

Volcanic outgassing formed Earth’s early atmosphere and hydrosphere (H, N, CO

2, H2O).Comet impacts also added gases and water.Note that the early atmosphere lacked oxygen (O2).Slide10

Early Bombardment Period

Haden Eon marked by bombardment of asteroids and comets.

Evolution of life was impossible until heavy bombardment ceased.The cratered surface of the moon best records the Late Heavy Bombardment Period.Slide11

Significant Solar System Events Through TimeSlide12

Earth/Venus Tectonics ComparisonSlide13

Mars Topography

Mars has more extreme topographic relief because of the lack of water erosion.

Olympus Mons: largest known volcano in the solar system (elev.=22 km; 14 miles).Slide14

Mars Exploration

Mars rovers have provided a wealth of data about the planet.

Mars resembles Earth more than any other planet.Slide15

Evidence of a “Wet” Early Mars History

Stream-cut channels dissect the topography.

Stratified and cross-bedded sediments.Evaporite deposits.Slide16

Mars Lake Beds

Precipitation of Hematite from evaporating lake.

Laterally continuous stratified beds.Evaporite deposits of Halite and Gypsum.Slide17

Exam Summary

Know difference between inner and outer planets.

Be familiar with the Impactor hypothesis for the origin of the moon.Know the lines of evidence that point to the past presence of liquid water on Mars.Know why Olympus Mons is the largest volcano in the solar system .Know about the origin and early composition of Earth’s atmosphere.