14. Formation of our solar system: The nebular hypothesis (Kant, 1755)
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16. .2% 1,000 – 1,600 K Iron (Fe), Nickel (Ni), Aluminum (Al) Metals .4% 500 – 1300 K Various Rock 1.4% < 150 K Water (H20), Methane (CH4), Ammonia (NH3) Hydrogen Compounds 98% Do not condense in nebula Hydrogen (H), Helium (He) Hydrogen and Helium Gas Relative Abundance in Solar System Condensation Temperature Examples
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18. Earth formation Nebula forms out of H, He clouds and fusion products from now dead stars. Gravity pulls gas and dust inward, and rotation makes a accretionary disk. The proto-sun is at the center and fusion begins when it is hot enough. Heavier elements concentrate in the inner rings. Collisions and gravitational attraction leads to the formation of planetesimals. Gravity reshapes the proto-Earth into a sphere Soon after Earth formed, a Mars-size planet collided with Earth, blasting debris into space that will form our Moon. Volcanic gases form the atmosphere, and as Earth cools, moisture condenses and rains into oceans. Some gases may have come from passing comets.
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21. 2. List each planet and the main facts about each.