EART 160: Planetary Science

1. EART 160: Planetary Science MESSENGER Flyby of Mercury This hemisphere never before seen!

2. Last Time • Celestial Mechanics • Newton Proves Kepler’s Laws • Conservation of Momentum, Angular Momentum, Energy • Collisions, Gravitational Slingshot • Solar System Formation • Nebular Theory • Jeans Collapse

3. Today • Solar System Formation • Runaway and Oligarchic Growth • Distribution of solar system materials • Planetary composition, structure • Late-stage accretion • Formation of the Moon • Planetary Migration • Late Heavy Bombardment • Extrasolar Planets: “Hot Jupiters”

4. Jeans Collapse • A perturbation will cause the density to increase locally • Runaway Process • Increased density  increased gravity  more material gets sucked in Gravitational potential energy M,r Thermal energy R Equating these two and using M~rR3 we get: Does this make sense? M=mass; r=density; R=radius; k=Boltzmann’s constant; T=temperature (K) N=no. of atoms; m=atomic weight; MH=mass of H atom

5. Proplyds in the Orion Nebula Disks radiate in the infrared All very young; few My Beta Pictoris – 50 ly Bipolar Outflow HH-30 in Taurus HST Images Courtesy NASA/ESA/STSci

6. Minimum Mass Solar Nebula We can use the present-day observed planetary masses and compositions to reconstruct how much mass was there initially Density drops off with distance. COINCIDENCE?!?!?!

7. Timeline of Planetary Growth • 1. Nebular disk formation • 2. Initial coagulation (~10km, ~104 yrs) • 3. Runaway growth (to Moon size, ~105 yrs) • 4. Oligarchic growth, gas loss(to Mars size, ~106 yrs) • 5. Late-stage collisions (~107-8 yrs)

8. Collisional Accretion (104 y) Inelastic Collisions between dust grains Dust grains also accrete onto chondrules: solidified molten fragments Forms Planetesimals R < few km Vertical Motions canceled out Disk orientation controlled by angular momentum Disk’s gravity also draws material toward midplane

9. Runaway Growth (105 y) • Slow-moving planetesimals accrete • Protoplanets grow to size of moon (3500 km) Fg = GMm / R2 vorbital < vesc vorbital > vesc “The rich get richer!” -- Bender

10. Oligarchic Growth (105 y) • Cosmic Feudal System • Only a few dozen big guys left (oligarchs) • And a lot of very small stuff (serfs?) • Oligarchs sweep up everything in their feeding zones • Gas drag slows large objects down, circularizes orbits • Brightening sun clears away nebular gas.

11. Composition • Solar Nebula • 98.4 % gas (H, He) • 1.1 % ices (e.g. H2O, NH3, CH4) • 0.4 % rock (e.g. MgSiO4) • 0.1 % metal (mostly Fe, Ni) • How do we know this? • Look at the Sun! • Absorpiton lines indicate elements • Discovery of He Volatile Refractory Image courtesy N.A.Sharp, NOAO/NSO/Kitt Peak FTS/AURA/NSF

12. Terrestrial planets Gas giants Ice giants Disk cools by radiation Nebula disk (dust/gas) Polar jets Cold, low r Hot, high r Infalling material Dust grains Stellar magnetic field (sweeps innermost disk clear, reduces stellar spin rate) Condensation in the Nebula Metals and Rocks Ices 1600 K 180 K The Frost Line

13. Terrestrial v. Jovian • Only refractories in inner SS • Planets can only grow to Earth-size • Too small to hold onto gas • Ices also available beyond frost line • Much more material • Ice-rock planets up to 20 M possible • Big enough to accrete H, He  can get huge, 300 M • Why no giant planets farther out than Neptune?

14. Final Compositions Io Ganymede • Terrestrial Planets • Iron Core (Red), Silicate Mantle (Grey) • Mercury has v. thin mantle. Why? • Very few volatiles, thin atmospheres? • Jovian Planets • Rock (Grey) and Ice (Blue Cores) • Gas envelope (Red, Yellow) • Jupiter and Saturn mostly H, He • Uranus, Neptune mostly ice Guillot, Physics Today, (2004).

15. Satellites • Satellites formed from mini-accretion disks about giant planets • Explains why they all orbit the same way and in the same plane • Irregular satellites (including Mars’s moons) captured later (high e, i) • What about our own freakishly large Moon?

16. Problems with this • Why exactly four terrestrial planets? • Numerical models can’t do this. • What is up with the Moon? • Gas Loss Timing • As star heats up, gas in disk is blown away • Gas causes planets to spiral in • Gas must stick around long enough to form giant planets • Why are Uranus and Neptune so shrimpy? • Why are extrasolar planets so close in? • Alan Boss • Rapid giant planet formation by disk instability (100s of years) • Planets tend to spiral into Sun • Hard to explain heavy elements abundances • Migration

17. Late-stage accretion (107-108 y) • Oligarchic growth results in dozens of planetesimals • Oligarchy is unstable! • Perturb each other until orbits cross • Giant Impacts • Large basins on all planetary bodies • Retrograde rotation of Venus • Obliquity of Uranus • Formation of the Earth’s Moon

18. It’s huge! Perturbs anything nearby Disrupted accretion at 2-3 AU No planet here where we expected one. Location of the asteroid belt Ejected icy planetesimals Gravitational slingshot effect Scattered in all directions  The Oort Cloud Jupiter: The Cosmic Bully

19. All planets’ orbits in a single plane. Sun’s rotation in same plane. Prograde orbits of all planets Planetary orbits nearly circular Angular momentum distribution Some meteorites contain unique inclusions Correlation of planetary composition with solar distance. Meteorites different from terrestrial and lunar rocks Spacing of the planets Giant impacts on all planetary bodies Prograde rotation, low obliquity of most planets Similar rotation periods for many planets Spherical distribution of comets Satellite systems of giant planets The Nebular Theory Explains:

20. Formation of the Moon • Co-accretion (sibling) •  and  formed together from Solar Nebula • Capture (spouse) •  made a close pass to , captured into orbit • Fission (child) • Fast-spinning , a blob tore away • Apollo mission to determine which one is real.

21. None of Them! •  similar to ’s mantle. Depleted in Fe, siderophiles, volatiles. • Cannot form from same assemblage • O, Si-isotopes in  and  rocks IDENTICAL. • Meteorites all different • Implies common origin of the silicates. • Angular Momentum of  - too small for fission. • -orbit not in equatorial plane. • Implies different trajectories

22. Requirements • Explain Angular Momentum of System • Explain Metal depletion of Moon • Initially different orbits • Silicates mixed • Earth’s core untouched •  Giant Impact! • Parasite-host relationship? • Genetic Engineering Experiment? • Other bad relationship analogy?

23. Giant Impact Hypothesis Mars-sized Planetesimal Proto-Earth Asphaug et al., 2001

24. Oblique impact, rotation increases 5 hour day! Impactor destroyed, Mantle stripped away Cores merge, silicates form accretion disk Some silicates fall back onto planet Rest forms the Moon At 12 R Canup and Asphaug, 2001

25. Migration • Do planets have to stay where they formed? • Why are Uranus and Neptune so small? • Extrasolar gas giants have TIGHT orbits! • Hot, hot, hot! WAY inside “frost line” Cheese it! Um, guys? ! Bwa ha ha!

26. Gas Giant Formation • Beyond frost line, planets accrete rock AND ice • Grow to 10-15 M • Accrete Gas • Uranus and Neptune have little gas • Failed cores • BUT nebula too sparse that far out to even get cores! • Standard formation model doesn’t work!

27. Four 15 M cores between 4 and 10 AU. • Jupiter forms where nebula is the densest, gets big. • All three other cores scatter off Jupiter, flung outward • Saturn still close enough to accrete a bunch of gas. • What happens to Joop? Conservation of Angular Momentum! Thommes et al., 1999

28. Hot Jupiters • Less than 0.05 AU from star • Problems with forming in situ • Not enough material • No ice, gas at all! • Atmosphere gets stripped away? HD209458b Image Courtesy ESA/ Alfred Vidal-Madjar / NASA

29. Inward Migration • Type I: Dynamical Friction • Small Planets drive spiral density waves in disk • Outer wave imparts torque, planet loses L. • Moves inward. • Type II: Coevolution • Growing planet clears a gap in the disk • “Relay station” for L-transport • Moves L outward, planet and gap move inward

30. Movie courtesy Phil Armitage http://jilawww.colorado.edu/~pja/planet_migration.html

31. Consequences • Hot Jupiters probably were Regular Jupiters that got Type II Migration • Giant moves in • What does Conservation of Angular Momentum say? • Terrestrial Planets move out. Wayyyy out! • Why did we escape this fate? • Atmosphere stripped off by solar wind? • Chthonian planet?

32. Next Time • Paper Discussions • Asphaug et al. (2006) • Thommes et al. (1999) • Meteorites • Asteroids • The Late Heavy Bombardment • You should now have everything you need to complete the homework. Really. I mean it this time.