1. Origin of the Moon September 1, 2010 Bonnie Meinke September 1, 2010 Bonnie Meinke

2. Why study the origin of the moon? How do terrestrial planets form? Effects of Moon on Earth?

3. Why study the origin of the moon? How do terrestrial planets form? Effects of Moon on Earth? Tides Obliquity changes

4. How terrestrial planets form Disk of gas and dust around Sun Interparticle collisions: if impact velocities are low enough, we get gravitationally bound aggregates 10,000 yrs: 10 km-sized bodies 100,000 yrs: Moon-Mars sized (~2000 km, ~20 “embryos”) 1 million-10 million yrs: planet-sized “giant impacts” will reduce number of embryos to 4 terrestrial planets

5. Clues to giant impacts Planets that spin fast Planets are tilted

6. Moon Properties Can you name some of the distinguishing properties of the Moon?

7. Moon Properties 1. Only 1 Moon 2. Depleted in Fe and volatiles 3. Oxygen isotopes similar to Earth 4. Moon’s orbit: is not in Earth’s equatorial plane Circular Expanding due to tidal interaction 5. Moon has very small core (I=0.39)

8. Moon Origin Hypotheses Co-accretion: Earth and Moon formed together Fission: Earth spun so fast that it split off a Moon-sized chunk Capture: Earth captured an independently-formed Moon as it passed by Giant Impact: Mars-sized body collided with proto-Earth and excavated material eventually coalesced to form Moon

9. Evaluate the Hypotheses Pros vs. Cons

10. Giant Impact Stages Earth close to final size Mars-sized impactor both differentiated both formed near 1 AU

11. Where does Iron go?

12. Both Fe cores stay with Earth 1 lunar mass in orbit outside Roche radius Moon is mostly impactor material

13. How hot is the Impact? heat removes volatiles from debris disk

14. How big of an impactor is needed to produce angular momentum of current system? To the board!

15. ReAccretion & the post- impact moon Mars-sized body collides with Earth Debris ejected into Earth orbit A. heated B. comes from mantle of both bodies (no Fe) C. ~1 lunar mass = ~1% Earth mass = ~10% impactor mass Debris accumulates to form one large Moon, not multiple small moons

16. Evolution of the Protolunar disk Centrally condensed hot disk = 2.5- 3R Earth Cooling: condensation/solidification Collisional spreading of disk Accretional growth of moonlets Tidal evolution of moonlets Collisions between moonlets yield moon

17. Evolution of the Protolunar disk Accretion in the disk collisional growth V esc a Roche = closest to a planet a body can hold together via self-gravity a Roche = 3R Earth

18. ReAccretion & the post- impact moon Earth spin and Moon orbit locked Moon orbit expands a few cm/yr Earth rotation slows

19. ReAccretion & the post- impact moon In the past, which is a possible state of the Earth/Moon system? A. Moon orbits closer in, Earth’s day is 18 hours B. Moon orbits farther away, Earth’s day is 36 hours C. Moon orbits closer in, Earth day is same as now D. Same conditions as today

20. ReAccretion & the post- impact moon In the past, which is a possible state of the Earth/Moon system? A. Moon orbits closer in, Earth’s day is 18 hours B. Moon orbits farther away, Earth’s day is 36 hours C. Moon orbits closer in, Earth day is same as now D. Same conditions as today