What have radial velocity surveys told us about (exo)-planetary science? Ge/Ay 133
Mayor, M. & Queloz, D. 1995, Nature, 378, 355
Udry, S. et al. 2002, A&A, 390, 26
Jovian planets througout the 0. 05 -5 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 0. 05 -0. 1 AU, little preference for low eccentricities: Butler, R. P. et al. 2006, Ap. J, 646, 505
Even with incompleteness, strong preference for ~Jovian mass: Butler, R. P. et al. 2006, Ap. J, 646, 505
Stars are different, turnover at low mass! Orion IMF “The brown dwarf desert”? Does this tell us that stars and planets form differently?
Is there an eccentricity preference w/mass? Not really… Marcy, G. et al. 2005, astro-ph/0505003
Is there an eccentricity preference w/mass? Not really, part II… ? Butler, R. P. et al. 2006, Ap. J, 646, 505
Another clue as to formation: Planet formation efficiency correlates strongly with metallicity! Fischer, D. A. & Valenti, J. 2005, Ap. J, 622, 1102
What about planetary multiplicity? Complex doppler patterns:
Summary of known multiple planetary systems: Marcy, G. et al. 2005, astro-ph/0505003
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 168443 a: 7. 2 Mj 58 days b: 17 Mj 1739 days =1/29. 98 ? ! 30: 1?
HD 12661 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 37124 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 241. 5 d C: 3. 75 Mj 1284 d
HD 82943 A: 1. 63 Mj 444 d B: 0. 88 222 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% w/planets @ <20 AU. - multiple planetary systems are ~common - planetary resonances are ~common What can explain these properties?
Theory Disk-star- and protoplanet interactions lead to migration while the gas is present. Coreaccretion? 1 AU at 140 pc subtends 0. ’’ 007. Simulation G. Bryden, JPL Thus, need to study objects in this phase… Jupiter (5 AU): V_doppler = 13 m/s V_orbit = 13 km/s
Core-accretion models can now be compared to observations: Data Planets versus metallicity: Ida, S. & Lin, D. 2004, Ap. J, 616, 567 Observed in open circles.
Early disk models held that eccentricities were DAMPED. Not so fast… Goldreich, P. & Sari, R. 2003, Ap. J, 585, 1024 Goldreich & Sari 2005 Need an initial e~0. 01.
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