EE144 Solar Nebula Hypothesis

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Across
  1. 1. Inside-out heating of the disk, hotter toward the center
  2. 3. Vast cold cloud of gas and dust that collapses to form a solar system
  3. 9. General term for the molecular cloud that collapses into a star system
  4. 10. Boundary where temperatures are cold enough for ices to condense
  5. 11. Process where dust grains collide and stick together to build planets
  6. 14. Effect of rotation causing the nebula to flatten into a disk
  7. 16. The hot, growing star at the center of the collapsing nebula
  8. 17. Process where hydrogen fuses into helium and releases energy
  9. 19. Small solid bodies formed from sticking dust; building blocks of planets
  10. 20. Moment when fusion begins in the young Sun
  11. 21. Force causing the molecular cloud to collapse inward
  12. 22. Cooling of the disk allowing solids (rocks, metals, ices) to form
  13. 23. Second-most abundant element in the original solar nebula
  14. 24. Light element present in trace amounts in the early solar nebula
Down
  1. 2. Worlds forming inside the frost line from metal and rock
  2. 4. Most abundant element in the solar nebula making up most of its mass
  3. 5. Type of young, variable star stage the early Sun passed through (T-Tauri phase)
  4. 6. The flattened rotating disk of gas and dust where planets formed
  5. 7. Energy released during collapse that raises central temperature above 3000 K
  6. 8. Leftover icy planetesimals that form beyond the frost line
  7. 12. Leftover rocky planetesimals inside the frost line
  8. 13. Conserved property causing the collapsing nebula to spin faster
  9. 15. Large planets forming beyond the frost line where ices and gases survive
  10. 18. Stream of charged particles from the young Sun that blows gas and dust away