observed properties of planetary...
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Geoff Marcy & Paul Butler Debra Fischer, Steve Vogt
Greg Laughlin, Eric Ford, Andrew Cumming, Greg Henry, Jack Lissauer Jason Wright, Brad Carter,
Chris McCarthy, John Johnson
10 Mar 200510 Mar 2005
Disks to PlanetsDisks to Planets
Observed Properties ofPlanetary Systems
Theory meets ObservationTheory meets Observation
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Observed Properties ofObserved Properties ofPlanetary SystemsPlanetary Systems
Update:Update: Planet Mass Distrib. Orbits: a, e Distrib. Metallicities of Host Stars
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- Stellar Sample -
1330 Nearby FGKM Stars
(~2000 stars total with Mayor et al. )
Star Selection Criteria:Star Selection Criteria:
•Vmag < 10 mag• No Close Binaries• Age > 2 Gyr
Hipparcos Cat. d < 100 pc
Lum
1.3Msun
0.3 MSUN
.. 1330 Target Stars 1330 Target StarsH-R DiagramH-R Diagram
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Typical Doppler Data
Errors: 2-3 m/s
Const. Vel.:80% of All Stars
No gas-giantNo gas-giantwithin 5 AU.within 5 AU.
KeckKeck
Significance ofSignificance of NondetectionsNondetections::
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Past 2 Years:New Planet Domains
• a > 2 AU• 1 M NEP < Msini < 1 M SAT
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Planet Discovery Space: Mass vs a
MASS(MJup) 1
0.1
10
1 1 MMearth earth @ 1 AU for d= 1 pc @ 1 AU for d= 1 pc ==> 3==> 3 microarcsec microarcsec
0.1 1.0 10 a (AU)
Sub-Saturn Masses:Sub-Saturn Masses: 30 - 100 30 - 100 MMEarthEarth
BeyondBeyond1 AU1 AU
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Gliese 436:Velocity vs. Phase
MsinMsinii = 21 M= 21 MEarthEarth
Tidal LockTidal Lock P = 2.64 dP = 2.64 d
Composition ?Composition ? rock + icerock + ice rock + Ferock + Fe gaseous gaseous
L = 1/50 LL = 1/50 LOOAtmosphere?Atmosphere? TTfrontfront = 650 K= 650 K
..
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Poor
Detect-
ability
Flat Extrapolation:Flat Extrapolation: +6% of stars have+6% of stars have giant planetsgiant planets 3 - 20 AU .3 - 20 AU . Total: 12 %*Total: 12 %*RiseRise
*But planetoccurrence is astrong functionof stellarmetallicity
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Future: Gas Giants Beyond 5 AUG5 VG5 V
Represents 3 %Represents 3 % of Starsof Stars
Orbits:Orbits: Circular orCircular or Eccentric?Eccentric?
G0 VG0 V
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P (d) ecc omega K(m/s) 4.617 0.01 69.2 69.6 241.342 0.25 249.2 55.21292.4 0.26 282.3 63.3
At Lick, wecontinue to observeall stars withdetected planets toimprove orbitalparameters and tosearch for additionalplanets.
Upsilon Upsilon AndromedaeAndromedae
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Orbital Eccentricities
TidalTidalCirc.Circ.
JupitersJupitersat 2-4 AU:at 2-4 AU: StillStillEccentricEccentric..
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a = 4.5 AU
Planets Orbiting Beyond Planets Orbiting Beyond 2 AU2 AU
a = 2.6 AU
a = 3.78 AUa = 3.78 AU
EccentricityEccentricity > 0.1 +/- 0.1 > 0.1 +/- 0.1
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70 VirLone, Eccentric Orbit
• 16 yrs• No TrendNo 2nd
planet
70 70 Vir Vir ((unphasedunphased))
ResidualsResiduals
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Origin of Eccentricities
Two Options:
1. Planet - Disk Pumping of ecc. - Get e = 0.5 ?
2. Resonance - Pumping, followed by ejection. - Ejection common ?
- however, a continuum of planetary companions in eccentric systems is not currently observed.
(Kley, Dirksen, Lee & Peale, Lin & Bryden, E.Chiang)
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Spectral SynthesisModeling
1) Solar spectrum setsgf values,broadeningcoefficients.
2) LTE radiativetransfer withKurucz modelatmospheres.
3) Least-Squares fit tospectral lines.
ChemicalChemicalAbundancesAbundancesOf StarsOf StarsWith Jeff With Jeff ValentiValenti
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P(planet) = 0.03 x
2.0
(NFe/NH)SUN
(NFe/NH)
Planet – Metallicity CorrelationAbundanceAnalysis of1040 stars onplanet search
Previous evidence:Gonzalez; Santos
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Stars with known exoplanets (highest metallicitydistribution) have a metallicity distribution that is about0.1 dex more metal-rich than other stars (solid line) onthe Lick, Keck and AAT programs.
These conclusions apply toFGK stars with exoplanets inorbital periods shorter than 4years and K > 30 m/s.
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•Subgiants without planetshave same metallicitydistribution as MS starswithout planets!
•Subgiants with planets havesame metallicity distributionas MS stars with planets!
No metallicity gradientacross the subgiant branch
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(Multi-planet systemsconnected with lines)
No corrrelation betweenmetallicity and orbitaleccentricity or orbital period.
Stars with planets are metal-rich, even when planets arein wide orbits!
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Exploiting the Planet-Metallicity Correlation
Hot Jupiter Search: “N2K”
International ConsortiumD. Fischer, G. Laughlin, R.P. Butler, G. Marcy (Keck)S. Ida, B. Sato (Japan: Subaru)D. Minniti (Chile: Magellan)G. Henry (Photometric Follow-up)M. Lopez-Morales, E. Ford, J. Valenti, C. McCarthyM. Ammons, S. Robinson, J. Johnson, R. Sareen
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Hot JupitersBoundary conditions for theories of orbital migration, planet-planetand planet-disk interactions, parking mechanisms and disk evolution
High probability transit candidates (e.g., HD 209458) - direct observations: atmosphere, reflected light, polarimetry - transit surveys miss 90% of close-in (non-transiting) planets
Serve as tracers of multiple planet systems with orbital periods shortenough to exhibit observable non-Keplerian interactions
Statistical anomalies: 3d periods, lower planet mass, higher stellarmass
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Strategy:Strategy:
• Start with database of 14,000 stars
V< 10.5, d < 110 pc, FGK
• Cull out high [Fe/H] candidates
• “Quick-look” 3-4 observations to check RV’s
RMS > 18 m/s: warrants follow-up
RMS < 18 m/s: drop
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High VelocityRMS reveals planetcandidates afterjust 3 observations!
About 40 new candidates!
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• The discoveries emerging from RV surveys continue tobreak new scientific ground:
lower mass planetslonger orbital periods
• These discoveries provide the foundation for further studiesthat characterize extrasolar planets
Spitzer observationsExtreme Adaptive Opticstransmission spectra of planet atmospheresreflected light, polarimetrySpace missions (SIM, TPF)
The field is making the transition from “stampcollecting” to planet characterization.