11

Lyot Lyot ConferenceConference

5 June 20075 June 2007

Properties of Properties of ExoplanetsExoplanets::from Giants toward Rocky Planetsfrom Giants toward Rocky Planets

& & InformingInforming Coronagraphy Coronagraphy

Collaborators:Collaborators: Paul Butler, Debra Fischer, Steve VogtPaul Butler, Debra Fischer, Steve Vogt

Chris McCarthy, Jason Wright, John Johnson, Katie PeekChris McCarthy, Jason Wright, John Johnson, Katie PeekChris Chris TinneyTinney, Hugh Jones, Brad Carter, Hugh Jones, Brad Carter

Greg Laughlin, Doug Lin, Shigeru Ida, Jack Greg Laughlin, Doug Lin, Shigeru Ida, Jack LissauerLissauer, , Eugenio Eugenio RiveraRivera

--Stellar Sample -Stellar Sample -

1330 Nearby FGKM Stars1330 Nearby FGKM Stars

(~2000 stars total with Mayor et al. )(~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 Stars

Target List:Target List:PublishedPublished

H-R DiagramH-R Diagram

22

Michel Mayor & DidierMichel Mayor & Didier Queloz Queloz

51 Peg51 Peg

First First ExoPlanetExoPlanet

Now Now Stephane Udry Stephane Udry plays leadership role also.plays leadership role also.

2000 FGKM M.S. Stars2000 FGKM M.S. StarsThree TelescopesThree Telescopes

19 Years19 Years(6 AU)(6 AU)

LickLick

8 Years8 Years (3.5 AU)

7 Years7 Years (3 AU)

Uniform Doppler Precision: 1-3 m sUniform Doppler Precision: 1-3 m s-1-1Doppler Doppler Monitering Monitering Begun: 1987Begun: 1987

Anglo-Aus. Tel.Anglo-Aus. Tel.KeckKeck

33

Precision: 1.5 m sPrecision: 1.5 m s-1-1

3 Years3 Years

Planets or Brown DwarfsPlanets or Brown Dwarfsin Unclosed, Long-Period Orbits:in Unclosed, Long-Period Orbits:

Targets for CoronagraphsTargets for Coronagraphs

44

SepSep ~~ 0.3 0.3 ““

SepSep ~ 0.2 ~ 0.2 ““

55

Sep ~ 0.2Sep ~ 0.2””

Examples ofExamples ofJupiter-massJupiter-mass

&&Saturn massSaturn mass

Planets Detected Planets Detected by RVby RV

66

Jupiter MassJupiter Mass Extrasolar Extrasolar PlanetsPlanets

P = 5.3 yrP = 5.3 yre = 0.47e = 0.47

Jupiter MassJupiter Mass Extrasolar Extrasolar PlanetsPlanets

P = 1.3 yrP = 1.3 yr

77

Msini Msini = 32 = 32 MMEarthEarth

Msini Msini = 57 = 57 MMEarthEarth

Msini Msini = 37 = 37 MMEarthEarth

Sub-Saturn Masses: Sub-Saturn Masses: 30 - 100 30 - 100 MMEarthEarth

Old Doppler Precision: 3 m/sOld Doppler Precision: 3 m/s

Sub-Saturn Masses:Sub-Saturn Masses: Detectable for P < 2 MonthDetectable for P < 2 Month

Multiple - Planet SystemsMultiple - Planet Systems

88

Weak Interactions2.5 MJ1.9 MJ

HD 12661: Sun-like StarHD 12661: Sun-like Star

2 - Planet Model2 - Planet Model

Velo

city

(m

eter

s/se

c)

Time (years)

HD 128311HD 128311 2:1 Resonance 2:1 Resonance

Inner OuterInner OuterPer (d)Per (d) 458 918 458 918MMsinisini 2.3 3.12.3 3.1ecc ecc 0.23 0.23 0.22 0.22ωω 119 119 212 212

PPc c / / PPbb = 2.004= 2.004Dynamical ResonanceDynamical Resonance(Laughlin)(Laughlin)

K0V, 1Gy, 16 pcK0V, 1Gy, 16 pc

99

Msini Msini = 1.4 M= 1.4 MJJ

M Dwarfs haveM Dwarfs have distant giant planets.distant giant planets.

5 Mean-Motion5 Mean-MotionResonancesResonances

Implies:Implies: Orbital MigrationOrbital Migration Capture intoCapture into

ResonancesResonances Eccentrcity Eccentrcity PumpingPumping

CoronagraphsCoronagraphs cancanexpect expect planets at 20 AUplanets at 20 AUaccompanied byaccompanied byinner giant planetsinner giant planets

1010

Giant Planets:Giant Planets: Mass Distribution Mass Distribution

Detection Limit:Detection Limit:~ 0.2 M~ 0.2 MJUP JUP @ 1 AU@ 1 AU

Rise towardRise toward lower masseslower masses

to 1 Mto 1 MSATSAT

Sub-SaturnsSub-Saturns

13/138 have13/138 haveMMplpl > 5 M> 5 MJJ= 10% of planets= 10% of planets

Poor

Detect-

ability

IfIf ddN N / / ddllogog a = const:a = const: ΔΔ6% of stars have6% of stars have planets planets 3 - 20 AU .3 - 20 AU .

LogLog

Semimajor Semimajor AxisAxis DistributionDistribution 6.5 % 6.5 % OccurrenceOccurrence

12 % of stars12 % of starsHarborHarborGiant PlanetsGiant Planets

1111

OrbitalOrbital Period DistributionPeriod DistributionCorrection for IncompletenessCorrection for Incompleteness

Period (days)Period (days)

Num

ber

Num

ber

dN /dlog dN /dlog P ~ PP ~ Pββ

ββ = +0.26 = +0.26

Cumming et al. 2007Cumming et al. 2007

27 yr27 yr9 AU9 AU

dN/dlogdN/dlog1010PP = 6.5%= 6.5%

Take Home:Take Home:

Occurrence of Long Period OrbitsOccurrence of Long Period OrbitsCumming et al. 2007Cumming et al. 2007

a < 3 AU 5 AU a < 3 AU 5 AU 10 AU 20 AU10 AU 20 AU

8.5% 8.5% 11% 11% 14% 19%14% 19%

For: 0.3 < For: 0.3 < MMplpl < 15 M< 15 MJJ

Cumulative percentage of stars with a Cumulative percentage of stars with a palnetpalnetN (<P), based on a power law extrapolation beyond P = 2000 d.N (<P), based on a power law extrapolation beyond P = 2000 d.

1212

Poor

Detect-

ability

IfIf ddN N / / ddllogog a = const:a = const: ΔΔ6% of stars have6% of stars have planets planets 3 - 20 AU .3 - 20 AU .

Most Models ==> Most Models ==> Reservoir of Reservoir of Jupiters Jupiters at 5-20 AU.at 5-20 AU.

Few Few Jupiters Jupiters a> 20 AU.a> 20 AU.LogLog

Semimajor Semimajor AxisAxis DistributionDistribution 6.5 % 6.5 % OccurrenceOccurrence

If If dN/dloga dN/dloga = const,= const,6%6% 20-120 AU20-120 AU

Inward Migration.Inward Migration. Planets left in placePlanets left in place as disk vanishes .as disk vanishes .

ArmitageArmitage,, Livio Livio,, Lubow Lubow, Pringle (2002), Pringle (2002)Trilling, Benz,Trilling, Benz, Lunine Lunine (2002)(2002)Lin & Ida 2004Lin & Ida 2004Alibert Alibert & Benz& Benz

Spectral SynthesisModeling

1) LTE radiative transferwith Kurucz modelatmospheres.

2) Least-Squares fit tospectral lines.

ChemicalChemicalAbundancesAbundancesOf StarsOf StarsFischer &Fischer & Valenti Valenti

1313

Planet Planet –– Metalicity Metalicity CorrelationCorrelation

Chem.Abund.Analysis of1000 stars onplanet search .

22PPplanetplanet ~ ~ ((NN

FeFe/ N/ N

HH))

Previous Planet-Previous Planet-Metallicity CorrMetallicity Corr::G.Gonzales, N.SantosG.Gonzales, N.Santos

Fischer & Fischer & Valenti Valenti 20052005

Metalicity Metalicity Models:Models:Core-Accretion Model:Core-Accretion Model:More Dust -->More Dust -->Planet growth ratePlanet growth rateIda & Lin (2005)Ida & Lin (2005) Kornet Kornet et al. (2005)et al. (2005) Ed Ed Thommes Thommes 20062006

Exoplanets Exoplanets as a function ofas a function ofStellar MassStellar Mass

- 120 M dwarfs (0.3-0.6 M- 120 M dwarfs (0.3-0.6 MOO)) - - 200 200 ““A-typeA-type”” Stars Stars (1.5-2.0 M(1.5-2.0 MOO))

1414

Retired A-Stars and Their PlanetsRetired A-Stars and Their Planets

John Johnson et al. (2007)

HD 210702: HD 210702: MM** = 1.85 M = 1.85 M

John Johnson 2007John Johnson 2007

1515

Jupiter Occurrence Jupiter Occurrence vs vs Stellar MassStellar MassFor a < 2.0 AU, Mpsini > 0.8 MJup, Nobs > 8

5/58 @Lick

3/31 @Keck

InclIncl. . SubgiantsSubgiants::1.5-2.5 1.5-2.5 M_sunM_sun

BewareBewareMetallicityMetallicityEffects.Effects.

JohnJohnJohnsonJohnson20072007

Orbital EccentricitiesOrbital Eccentricities

<e> = 0.25<e> = 0.25 Origin of Origin of eccenteccent.. controversial .controversial .

Ecc Ecc still highstill high

beyondbeyond 2.5 AU 2.5 AU

<e>=0.25<e>=0.25

Tidal Circ.:Tidal Circ.: a < 0.1 AU a < 0.1 AU

1616

Origin of EccentricitiesOrigin of EccentricitiesPlanet - Planet InteractionsPlanet - Planet Interactions

Ford & Ford & Rasio Rasio 20062006

Super-Earths: 1 - 14 Super-Earths: 1 - 14 MMEarthEarthPoorly Understood Planet DomainPoorly Understood Planet Domain

Earth - Uranus:Earth - Uranus: Gap in Mass: Factor 14 Gap in Mass: Factor 14

Intermediate MassesIntermediate Masses::

Do theyDo they Form?Form? Or do planet embryosOr do planet embryos accrete gas ala Neptune ?accrete gas ala Neptune ?

If They Form:If They Form: - - TerrTerr-like: CO-like: CO22 AtmAtm. ?. ? - Neptune-like H&He - Neptune-like H&He env env ??

Density: Density: 1 or 5 g cm1 or 5 g cm-3 -3 ??

Terrestrial

Ice & Gas giantsIce & Gas giants

Super-Super-EarthsEarths

??

1717

Gliese Gliese 436 (M2.5 V)436 (M2.5 V)

Gl Gl 436:436: Periodogram Periodogram

P = 2.643 dayP = 2.643 day

1818

Gliese Gliese 436:436:

22 Earth Masses22 Earth Masses

MsinMsinii = 22 M= 22 MEarthEarth

Tidal LockTidal Lock P = 2.64 dP = 2.64 d

Composition ?Composition ? Gaseous ? Gaseous ? Rock + ice ? Rock + ice ? Rock + Fe core? Rock + Fe core?

LLSTARSTAR= 1/50 L= 1/50 LOO

Atmosphere?Atmosphere? T Tfrontfront = 650 K ?= 650 K ? TTbackback< 200 K ?< 200 K ?

..

Butler et al. 2004; Maness et al. 2007Butler et al. 2004; Maness et al. 2007

Gliese Gliese 436 Transits436 TransitsR = 3.95 R = 3.95 RREarthEarth

Gillon Gillon et al 2007et al 2007

pp

ρρ = 2.0 gm/cc = 2.0 gm/cc

1919

Model from Fortney, Marley, & Jones 2007Model from Fortney, Marley, & Jones 2007

or liquid?

ρρ = 2.0 gm/cc = 2.0 gm/cc

Possible:Possible:Rocky coreRocky core&&H/He H/He EnvEnv..

Requires unlikely Requires unlikely 17 17 M_Earth of rockM_Earth of rockwithin 1 AU.within 1 AU.

““It seems likely that planets with masses within an order ofIt seems likely that planets with masses within an order ofmagnitude of the Earthmagnitude of the Earth’’s mass will be composed primary ofs mass will be composed primary of……ices, rocks, and iron.ices, rocks, and iron.””

Gliese Gliese 876 (M3V)876 (M3V)

Star Mass = 0.32 Star Mass = 0.32 MMsunsun

d = 4 pcd = 4 pc Two Two JupitersJupiters in 2:1 in 2:1 resres..

2020

Gliese Gliese 876: 2-Planet Fit876: 2-Planet FitVe

loci

ty (

m s

Ve

loci

ty (

m s

-1-1 ) )

TimeTime

GL 876GL 8762:1 Mean-Motion Resonance2:1 Mean-Motion Resonance

&&Apsidal LockApsidal Lock

Inner Outer Inner OuterPP 30.1 61.0 d 30.1 61.0 dMsiniMsini 0.56 1.89 M0.56 1.89 MJJ

ee 0.27 0.10 0.27 0.10

ωω 330 333 330 333οο

Resonance Work: Laughlin & Chambers Lissauer & Rivera Man Hoi Lee & S.Peale

2121

Gliese Gliese 876876

2:12:1Mean MotionMean Motion

ResonanceResonance

PrecessionPrecessionPeriod: 9 yrPeriod: 9 yr

Man Hoi LeeMan Hoi Lee

GJ 876: VelocitiesGJ 876: Velocities Two-PlanetTwo-PlanetModelModel

Laughlin et al. 2004

2222

3-Planet Fit3-Planet Fit

Rivera &Rivera &LissauerLissauer

Velocity Residuals toVelocity Residuals to2-Planet fit2-Planet fit

Period = 1.94 dPeriod = 1.94 d

M M sinsinii = 5.9 = 5.9 MMEarthEarth

For i = 50 deg,For i = 50 deg,MMPLPL = 7.5 = 7.5 MMEarthEarthVe

loci

tyVe

loci

ty

Orbital PhaseOrbital PhaseInward oInward off habitable zonehabitable zone

2323

Gliese Gliese 581581 Orbit Orbit Min.Mass Min.Mass Likely Mass (x 4/Likely Mass (x 4/ππ)) Radius(AU) Radius(AU) (Earths) (Earths) (Earths)(Earths)------------------------------------------------------------------------------------------ b 0.041 b 0.041 15.2 15.2 19 19 c c 0.073 0.073 5.0 5.0 6.46.4 ””T = 0-40 CT = 0-40 C”” d d 0.25 0.25 8.2 8.2 10.410.4--------------------------------------------------------------------------------------------

Planet Planet ““cc”” ::1) Actual Habitable Zone:1) Actual Habitable Zone: 0.10-0.20 AU0.10-0.20 AU Efficient IR opacity -> heating inEfficient IR opacity -> heating in any atmosphere (any atmosphere (SasselovSasselov, , SelsisSelsis,, KastingKasting, , SeagerSeager, , BlohBloh, , CuntzCuntz, 2007), 2007) (Potsdam preprint)(Potsdam preprint)

2) 2) Mass: Arguably an Ice Giant:Mass: Arguably an Ice Giant:~ ~ Gliese Gliese 436 b, Uranus, Neptune436 b, Uranus, Neptune

See Xavier See Xavier Bonfils Bonfils talk.talk.

2424

In a In a protoplanetary protoplanetary disk,disk,ifif 6 6 MMearth earth of silicates accumulate into planetof silicates accumulate into planet

does itdoes it normally acquire ices too?normally acquire ices too?

Outside snow line: Outside snow line: Yes.Yes.

Witness Solar SystemWitness Solar System’’s - s - icy giants, icy moons, icy giants, icy moons, plutopluto, , KBOsKBOsAllAll have comparablehave comparable:: silicate & water silicate & water

Formation Within Snow Line:Formation Within Snow Line:Water Delivery to Rocky PlanetsWater Delivery to Rocky Planetsby hydrated asteroids & cometsby hydrated asteroids & comets

Water Delivery: Comets &Water Delivery: Comets &hydrated asteroidshydrated asteroids

HH22O contentO content vs r vs rorborb fromfrommeteoritesmeteorites

N-body: collisions deliver HN-body: collisions deliver H22OO Jupiter ejects asteroids,Jupiter ejects asteroids,

preventing their delivery of waterpreventing their delivery of waterto the terrestrial planets at 1 AU.to the terrestrial planets at 1 AU.

Continuous HContinuous H22O deliveryO delivery Loss of HLoss of H22O by impacts ? ? ?O by impacts ? ? ?

Water-rich worlds common ?:Water-rich worlds common ?: 10 - 100 10 - 100 ““Earth-OceansEarth-Oceans””

N-Body Planet Growth with Water DeliveryN-Body Planet Growth with Water DeliveryRaymond, Quinn, Raymond, Quinn, Lunine Lunine 20042004

Water Content (Earth Oceans)Water Content (Earth Oceans)

2525

Solve Interior Solve Interior EqnsEqns.. Include EOS of water +Include EOS of water +

Rock mantle + Fe coreRock mantle + Fe core Water is Water is liquidliquid at high at high

pressure (pressure (~Europa~Europa) .) .

Phase Diagram of WaterPhase Diagram of Water

Super EarthsSuper EarthsFormationFormation beyondbeyond 2 AU2 AU

Leger et al. 2004Leger et al. 2004

Ice-rock Ice-rock planetesimal planetesimal growthgrowth Europa Europa/Neptune Composition:/Neptune Composition:

Ice - rock : 50-50Ice - rock : 50-50 Migration inward of 1 AUMigration inward of 1 AU

StructureStructure

10 - 50% H10 - 50% H22OO

HH22O Atmosphere +O Atmosphere + HH22O Ocean +O Ocean + Ice Envelope (ala Neptune) Ice Envelope (ala Neptune)

Lower Density than rocky planetsLower Density than rocky planets

Distinguish water worlds from rockyDistinguish water worlds from rockyworlds:worlds:

Radial velocity and transit ---> M Radial velocity and transit ---> M, R ., R .

oceanocean

66 M MEarthEarth Planets:Planets:50% H50% H22O O No H No H22OO

Fe, Ni

Silicates

““iceice””

ρρ = 4.3 g cm = 4.3 g cm-3-3 ρρ = 7.7 g cm = 7.7 g cm-3-3

PPcc = 1600 = 1600 GPaGPa

ss

Leger 2004, Raymond 2005Leger 2004, Raymond 2005

2626

Detecting Detecting Rocky PlanetsRocky Planetsby Doppler Measurements of Starsby Doppler Measurements of StarsStarStar’’s Wobble Velocity:s Wobble Velocity: K = 0.1 m/s [K = 0.1 m/s [MMplpl/M/Mstar star 1/a1/aAUAU

1/21/2]] ((MMplpl in Min MEE))

Benchmark:Benchmark: Earth induces 0.1 m/s (at 1 AU)Earth induces 0.1 m/s (at 1 AU)

Strategy:Strategy: Achieve Doppler Precision of 1 m/sAchieve Doppler Precision of 1 m/s Choose Low Mass StarsChoose Low Mass Stars Search for Short Periods (small a)Search for Short Periods (small a) Low mass stars haveLow mass stars have lower surface turbulence and lower oscillationslower surface turbulence and lower oscillations

Lyot Lyot ConferenceConference

SummarySummary Mass Distribution: Rises to lower massesMass Distribution: Rises to lower masses Semimajor Semimajor Axis Axis DistribDistrib.: Rises toward 5 AU - Beyond?.: Rises toward 5 AU - Beyond? Planets correlate withPlanets correlate with Metalicity Metalicity & Stellar mass& Stellar mass

Concern:Concern: <5% have giant planets beyond <5% have giant planets beyond 20 AU20 AU ~10%~10% of giant planets haveof giant planets have M>5 M>5 MjupMjup

Occurrence of M>5 Occurrence of M>5 Mjup Mjup beyond 20 AU < 0.5% ??beyond 20 AU < 0.5% ??

F and A starsF and A stars gold vein: Young, Massive, Metal-Rich Starsgold vein: Young, Massive, Metal-Rich Stars