1. AST 111 Lecture 15 Formation of the Solar System

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5. Past vs. Present A formation theory must be consistent with: – Motion of the planets – Two types of planets (terrestrial and jovian) – Many asteroids and comets Can test formation theories! – We can observe forming solar systems

6. First Theories Nebular hypothesis: – Solar System formed from collapse of interstellar gas cloud called Solar Nebula – This theory is now accepted Close encounter hypothesis: – Near collision between the Sun and another star pulled blobs of gas from the Sun that formed planets

7. Initial Solar System Formation Cloud starts as large and diffuse – Slowly rotating – Cold Gravity alone may or may not have pulled it together – Shock from nearby supernova?

8. Initial Solar System Formation The cloud begins to collapse – Gravitational potential energy converted to thermal energy Temperature and density highest at center – The sun forms there

9. Initial Solar System Formation Conservation of angular momentum causes it to spin faster – Like an ice skater pulling her arms in

10. Initial Solar System Formation It flattens into a disk

11. Initial Solar System Formation Spinning, flattened disk (200 AU) Mass and temperature greatest at center

12. Observations This is consistent with the planets: – Orbiting in the same direction – (Mostly) rotating in the same direction The heating caused by the cloud’s collapse should emit infrared radiation – We have seen this!

13. Observations The star AU Microscopii has a debris disk:

14. Solar Nebula Spinning disk was about 200 AU in diameter Constant mixing of gas should ensure uniform composition of 98% H and He with 2% heavier elements

15. Early Formation of Planets Planets had to start as “seeds” – Clumps of matter which attracted other clumps of matter, and grew – One critical factor caused Jovian seeds to differ from terrestrial seeds

16. Condensation When something condenses, it turns from a gas to either a solid or liquid – Do things tend to condense at higher or lower temperatures? An element has to condense in order to stick to a planet seed

17. Solar Nebula: Composition Three chemical components: – Hydrogen and Helium: 98% – Hydrogen Compounds (ICES): 1.4% – Rock and metal: 0.6%

18. Condensation Temperatures In the Solar Nebula: – One does not condense – One condenses at low temperature – One condenses at high temperature Which ones?

19. Early Formation of Planets Metals and rock condense at a higher temperature than ices Ices (hydrogen compounds) much more abundant than rock and metal

20. Early Formation of Planets Near (what is now) Mercury’s orbit: – Temperatures dropped below the condensation point for rocks and metals – But rocks and metals are the least abundant material in the solar system!

21. Early Formation of Planets The Frost Line is the point where temperatures allow ices to condense Located between (what is now) Mars’ and Jupiter’s orbit

22. Early Formation of Planets Beyond the Frost Line, a whole new abundance of material can condense onto the planet seed.

23. Early Formation of Planets Terrestrial planets started from SMALL seeds – Rock and metal Jovian planets started from LARGE seeds – Ice (H-compounds) – Also rock and metal

24. Terrestrial Planet Formation Very little rock and metal – Terrestrial planets are smaller Accretion: – Particles moving in mostly the same direction – They gently smushed together Once large enough, gravity could take over – Large “boulders” called planetesimals

25. Terrestrial Planet Formation As planetesimals grew larger, they hit more stuff Eventually, they hit all the stuff they could hit – They would sometimes hit each other – Only the largest could survive

26. Terrestrial Planet Formation Ends with a large molten mass Cools and solidifies

27. Jovian Planet Formation Given all the ice (from H-compounds), why aren’t the jovian planets large ice spheres? – Jovian planets started as ice spheres. – Moons of jovian planets are ice spheres.

28. Jovian Planet Formation Recall that 98% of the forming Solar System was H and He. The larger planet seeds could capture H and He. Due to their larger mass and colder temperatures, they could hold onto it. Terrestrial planets could not. This is why the Jovian planets are “gas giants” (and not ice spheres).

29. Moons Recall: – Moons of terrestrial planets “out of place” – Jovian planets have large moons that follow the rotation of their parent planets

30. Jovian Moon Formation Jovian planets formed their own accretion disks – Created moons, captured smaller moons The moons aren’t gas giants – Too small to hang onto H and He

31. Terrestrial Planet Moons Terrestrial planets didn’t have “mini-solar systems” They didn’t form moons. Mars stole them from the nearby asteroid belt

32. Terrestrial Planet Moons Earth’s moon formed via catastrophic collision

33. The End of Planet Formation So… what about the leftover material? When the Sun “turned on”, solar wind swept leftover material away Be thankful for the timing of this. – Too early: planetary material would have been swept away – Too late: cooling could have turned terrestrial planets into icy worlds (condensation of H-compounds)

34. The Aftermath of Planet Formation Some planetesimals remained after solar wind kicked in – These are the asteroids and comets Main asteroids (between Mars and Jupiter): – Why are they rocky? Kuiper belt (past Neptune): – Why are they icy?