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

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

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

Jovian planets througout the AU region. And…

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

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

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

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

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

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

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

What about planetary multiplicity? Complex doppler patterns:

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

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

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

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

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

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

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

HD a: 0.75 Mj 152 d b: 1.2 Mj 1495 d

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

HD A: 1.63 Mj 444 d B: d

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

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% <20 AU. - multiple planetary systems are ~common - planetary resonances are ~common What can explain these properties?

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…

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

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