1. Ge/Ay133 What have radial velocity surveys told us about (exo)-planetary science?

2. Mayor, M. & Queloz, D. 1995, Nature, 378, 355

3. Udry, S. et al. 2002, A&A, 390, 26

4. Jovian planets througout the 0.05-5 AU region. And…

5. No strong preference for orbital distances… …except for a “pile up” of hot Jupiters at P~3 days.

6. Planetary characteristics? Some trend in M versus R (bias?), but beyond 0.05-0.1 AU, little preference for low eccentricities: Butler, R.P. et al. 2006, ApJ, 646, 505

7. Even with incompleteness, strong preference for ~Jovian mass: Butler, R.P. et al. 2006, ApJ, 646, 505

8. Stars are different, turnover at low mass! “The brown dwarf desert”? Does this tell us that stars and planets form differently? Orion IMF

9. Is there an eccentricity preference w/mass? Not really… Marcy, G. et al. 2005, astro-ph/0505003

10. Is there an eccentricity preference w/mass? Not really, part II… Butler, R.P. et al. 2006, ApJ, 646, 505 ?

11. Another clue as to formation: Planet formation efficiency correlates strongly with metallicity! Fischer, D.A. & Valenti, J. 2005, ApJ, 622, 1102

12. What about planetary multiplicity? Complex doppler patterns:

13. Summary of known multiple planetary systems: Marcy, G. et al. 2005, astro-ph/0505003

14. A super earth & GJ 876? Rivera, E.J. et al. 2005, (see class web site)

15. GJ 876 orbits evolve with time (expected w/mutual perturbations)! What about other systems? Rivera, E.J. et al. 2005, (see class web site)

16. HD 168443 a: 7.2 Mj 58 days b: 17 Mj 1739 days =1/29.98 ?! 30:1?

17. HD 12661 a: 2.3 Mj 263 days a: 1.6 Mj 1444 days =1/5.5 11:2?

18. 47 U Ma a: 2.5 Mj 1089 days b: 0.76 Mj 2594 days =1/2.4

19. Gleise 876 a: 1.89 Mj 61 days b: 0.56 Mj 30 days

20. HD 37124 a: 0.75 Mj 152 d b: 1.2 Mj 1495 d

21. ups And A: 0.69 Mj 4.6 d B: 1.9 Mj 241.5 d C: 3.75 Mj 1284 d

22. HD 82943 A: 1.63 Mj 444 d B: 0.88 222 d

23. 55 Cnc A:.84 Mj 14.6 d B: 0.21 Mj 44.3 d C: 4 Mj 5360 d 3:1!

24. What we know: - ~1% of solar-type stars have Hot Jupiters -~7% of solar-type stars have >Mj planets in the “terrestrial planet” region. Extrapolation of current incompeteness suggests ~12% w/planets @ <20 AU. - multiple planetary systems are ~common - planetary resonances are ~common What can explain these properties?

25. Disk-star- and protoplanet interactions lead to migration while the gas is present. Core- accretion? Theory 1 AU at 140 pc subtends 0.’’007. Jupiter (5 AU): V_doppler = 13 m/s V_orbit = 13 km/s Simulation G. Bryden, JPL Thus, need to study objects in this phase…

26. Core-accretion models can now be compared to observations: Planets versus metallicity: Data Observed in open circles. Ida, S. & Lin, D. 2004, ApJ, 616, 567

27. Early disk models held that eccentricities were DAMPED. Not so fast… Goldreich & Sari 2005 Need an initial e~0.01. Goldreich, P. & Sari, R. 2003, ApJ, 585, 1024