Earth formed around 4.54 billion years ago, approximately one-third the age of the universe, by accretion from the solar nebula. Volcanic outgassing probably created the primordial atmosphere and then the ocean, but the early atmosphere contained almost no oxygen.
1. The History of the Earth
2. Origin of the Universe The universe began about 14.4 billion years The Big Bang Theory states that, in the beginning, the universe was all in one place All of its matter and energy were squished into an infinitely small point, a singularity Then it exploded
3. Origin of the Universe The tremendous amount of material blown out by the explosion eventually formed the stars and After about 10 billion years, our solar system began to form
4. Birth of the Solar System We know how the Earth and Solar System are today and this allows us to work backwards and determine how the Earth and Solar System were formed Plus we can out into the universe for clues on how stars and planets are currently being formed
5. The Nebular Hypothesis In cosmogony, the Nebular Hypothesis is the currently accepted argument about how a Solar System can form
6. Other Solar Systems We have now discovered over two hundred planets orbiting other stars The processes that created our solar system have also created an uncountable number of other solar
7. The Nebular Hypothesis A large gas cloud (nebula) begins to condense Most of the mass is in the center, there is turbulence in the outer parts
8. The Nebular Hypothesis The turbulent eddies collect matter measuring meters across Small chunks grow and collide, becoming large aggregates of gas and solid chunks
9. The Nebular Hypothesis Pictures from the Hubble Space Telescope show newborn stars emerging from dense, compact pockets of interstellar gas called evaporating gaseous globules
10. The Nebular Hypothesis Gravitational attraction causes the mass of gas and dust to slowly contract and it begins to rotate The dust and matter slowly falls towards the
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12. False Color Image of Protostar The multi-colored area shows a dust disk surrounding a newborn star The red-orange area at the center represents the brightest region, which contains the young star It is surrounded by the cooler, dusty disk, which appears as yellow, green and blue The diameter of the disk is about 20 times larger than our entire solar system
13. The Sun After sufficient mass and density was achieved in the Sun, the temperature rose to one million °C, resulting in thermonuclear fusion. H atom + H atom = He atom + energy
14. Birth of the Solar System
15. Protoplanets Gravitational forces allow the inner planets to accrue and compact solid matter (including light and heavy atoms) Solar radiation blew gases (primarily hydrogen, helium) away from inner planets These gases were collected and condensed into the gas giants (Jupiter, Saturn, Uranus, Neptune) Beyond Neptune, ice and frozen gases form Pluto, Sedna and the Kuiper Belt Objects Left-over debris form comets and asteroids
16. Birth of the Solar System
17. Size of the Planets
18. Venus, Earth and Mars These maps are color coded to display different elevations on the surface of each planet Fig. 1.9
19. The Age of the Earth Earth is ~ 4,570,000,000 years old Meteorites give us access to debris left over from the formation of the solar system We can date meteorites using radioactive isotopes and their decay products
20. Geologic Time
21. Bombardment From Space For the first half billion years of its existence, the surface of the Earth was repeatedly pulverized by asteroids and comets of all sizes One of these collisions formed the Moon
22. Formation of the Moon The Giant Impact Hypothesis predicts that around 50 million years after the initial creation of Earth, a planet about the size of Mars collided with Earth This idea was first proposed about 30 years ago, but it took calculations by modern high-speed computers to prove the feasibility
23. Formation of the Moon This collision had to be very spectacular! A considerable amount of material was blown off into space, but most fell back onto the Earth
24. Formation of the Moon Part of the material from the collision remained in orbit around the Earth By the process collision and accretion, this orbiting material coalesced into the Moon The early Moon orbited very close to the Earth
25. The Early Earth Heats Up Three major factors that caused heating and melting in the early Earth’s interior: 1. Collisions (Transfer of kinetic energy into heat) 2. Compression 3. Radioactivity of elements (e.g. uranium, potassium, or thorium)
26. The Core About 100 million years after initial accretion, temperatures at depths of 400 to 800 km below the Earth’s surface reach the melting point of iron In a process called global chemical differential, the heavier elements, including the melted iron, began to sink down into the core of the Earth, while the lighter elements such as oxygen and silica floated up towards the surface
27. Global Chemical Differentiation This global chemical differential was completed by about 4.3 billion years ago, and the Earth had developed a inner and outer core, a mantle and crust
28. Chemical Composition of Earth Each of the major layers has a distinctive chemical composition, with the crust being quite different from the Earth as a whole Whole Earth: Crust: Fe+O+Si+Mg = 93% Si+O+Al = 82%
29. Chemical Composition of Earth Lithosphere: strong, rocky outer shell of the solid Earth including all the crust and the upper part of the mantle to a depth of ~100 km (forms the Asthenosphere: weak,ductile layer of the mantle beneath the lithosphere; deforms to accommodate the motions of the overlying plates Deep Mantle: mantle beneath the asthenosphere (~400 to 2900 km in depth) Outer core: liquid shell composed of mostly iron Inner core: innermost sphere composed primarily of solid iron
30. Chemical Composition of Earth Continents: Formed from solidified magma that floated up from the Mantle Oceans and Atmosphere: Fluid and gaseous outer layers believed to have been created by out- gassing of gases and fluids from volcanic eruptions (in a process called volatile transfer)
31. The Evolving Atmosphere Right after its creation, the Earth is thought to have had a thin atmosphere composed primarily of helium (He) and hydrogen (H) gases The Earths gravity could not hold these light gases and they easily escaped into outer space Today, H and He are very rare in our atmosphere
32. The Evolving Atmosphere For the next several hundred million years, volcanic out-gassing began to create a thicker atmosphere composed of a wide variety of gases The gases that were released were probably similar to those created by modern volcanic eruptions
33. The Evolving Atmosphere These would include: Water vapor (H2O) Sulfur dioxide (SO2) Hydrogen sulfide (H2S) Carbon dioxide (CO2) Carbon Monoxide (CO) Ammonia (NH3) Methane (CH4) Note that oxygen (O2) gas is not created by volcanic eruptions
34. Creating the Oceans It is hypothesized that water vapor escaping from the interior of the Earth via countless volcanic eruptions created the oceans (this took hundreds of millions of years)
35. Creating the Oceans Astronomers also hypothesize that comets impacting the Earth were a major source of water that contributed to creation of the oceans Remember, that comets are best described as “dirty ice balls”
36. Creating the Oceans The earliest evidence of surface water on Earth dates back about 3.8 billion years
37. Geologic Time
38. A billion Year Old Earth By 3.5 billion years ago, when the Earth was a billion years old, it had a thick atmosphere composed of CO2, methane, water vapor and other volcanic gases By human standards this early atmosphere was very poisonous It contained almost no oxygen Remember, today our atmosphere is 21% oxygen
39. A billion Year Old Earth By 3.5 billion years ago, the Earth also had extensive oceans and seas of salt water, which contained many dissolved elements, such as
40. A billion Year Old Earth But most important, by 3.5 billion years ago, there was life on Earth
41. The Continents By 2.5 billion years ago, the continents had been formed The density of the continental crust (2.8 gr/cm3) is lighter that the crust found on ocean bottoms (3.2 gr/cm3), so the continents rise above the ocean floor A question that remains unanswered is, when did plate tectonics start?
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