The Transit Method: Results from the Ground - … Transit Method: Results from the Ground ......
Transcript of The Transit Method: Results from the Ground - … Transit Method: Results from the Ground ......
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The Transit Method: Results from the Ground•• Results from individual transit search programs• The Mass-Radius relationships (internal structure)• Global Properties• The Rossiter-McClaughlin Effect
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There are now 124 transiting extrasolar planets
First ones were detected by doing follow-up photometry of radial velocity planets. Now transit searches are discoveringexoplanets
Transiting Exoplanets
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Radial Velocity Curve for HD 209458
Period = 3.5 days
Msini = 0.63 MJup
The probability is 1 in 10 that a short periodJupiter will transit. HD 209458 was the 10th short period exoplanet searched for transits
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Charbonneau et al. (2000): The observations that started it all:
• Mass = 0.63 MJupiter
• Radius = 1.35 RJupiter
• Density = 0.38 g cm–3
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Hubble Space Telescope.
An amateur‘s light curve.
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HD 209458b has a radius larger than expected.Burrows et al. 2000
Evolution of theradius of HD 209458b and τ Boob
HD 209458b
Models I, C, and D are for isolated planetsModels A and B are for irradiated planets.
One hypothesis for the large radius is that the stellar radiation hinders thecontraction of the planet (it is hotter than it should be) so that it takeslonger to contract. Another is tidal heating of the core of the planet if youhave nonzero eccentricity
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The OGLE Planets
• OGLE: Optical Gravitational Lens Experiment (http://www.astrouw.edu.pl/~ogle/)
• 1.3m telescope looking into the galactic bulge
• Mosaic of 8 CCDs: 35‘ x 35‘ field
• Typical magnitude: V = 15-19
• Designed for Gravitational Microlensing
• First planet discovered with the transit method
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The first planet found with the transit method
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Konacki et al.
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Vsini = 40 km/s
K = 510 ± 170 m/s
i= 79.8 ± 0.3
a= 0.0308
Mass = 4.5 MJ
Radius = 1.6 RJ
Spectral Type = F3 V
OGLE transiting planets: These produce low quality transits, theyare faint, and they take up a large amount of 8m telescopetime..
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The OGLE PlanetsPlanet Mass
(MJup)Radius(RJup)
Period(Days)
Year
OGLE2-TR-L9 b 4.5 1.6 2.48
3.19
1.21
4.01
1.43
1.69
3.98
3.68
2007
OGLE-TR-10 b 0.63 1.26 2004
OGLE-TR-56 b 1.29 1.3 2002
OGLE-TR-111 b 0.53 1.07 2004
OGLE-TR-113 b 1.32 1.09 2004
OGLE-TR-132 b 1.14 1.18 2004
OGLE-TR-182 b 1.01 1.13 2007
OGLE-TR-211 b 1.03 1.36 2007
Prior to OGLE all the RV planet detections had periods greater thanabout 3 days.
The last OGLE planet was discovered in 2007. Most likely these will bethe last because the target stars are too faint.
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The TrES Planets
• TrES: Trans-atlantic Exoplanet Survey (STARE is a member of the networkhttp://www.hao.ucar.edu/public/research/stare/)
• Three 10cm telescopes located at Lowell Observtory, Mount Palomarand the Canary Islands
• 6.9 square degrees
• 4 Planets discovered
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TrEs 2b
P = 2.47 d
M = 1.28 MJupiter
R = 1.24 RJupiter
i = 83.9 deg
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The HAT Planets
• HATNet: Hungarian-made Automated Telescope(http://www.cfa.harvard.edu/~gbakos/HAT/
• Six 11cm telescopes located at two sites: Arizona and Hawaii
• 8 x 8 square degrees
• 13 Planets discovered
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HAT-P-12b
Star = K4 VPlanet Period = 3.2 daysPlanet Radius = 0.96 RJupPlanet Mass = 0.21 MJup (~MSat)ρ = 0.3 g cm–3
The best fitting model for HAT-P-12b has a core mass ≤ 10 Mearth and is still dominated by H/He (i.e. like Saturn and Jupiter and not like Uranus and Neptune). It is the lowest mass H/He dominated gas giant planet.
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The WASP Planets
WASP: Wide Angle Search for Planets (http://www.superwasp.org). Also known as SuperWASP
• Array of 8 Wide Field Cameras
• Field of View: 7.8o x 7.8o
• 13.7 arcseconds/pixel
• Typical magnitude: V = 9-13
• 38 transiting planets discovered so far
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The First WASP Planet
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Coordinates RA 00:20:40.07 Dec+31:59:23.7
Constellation PegasusApparent Visual Magnitude 11.79Distance from Earth 1234 Light YearsWASP-1 Spectral Type F7VWASP-1 PhotosphericTemperature 6200 K
WASP-1b Radius 1.39 Jupiter RadiiWASP-1b Mass 0.85 Jupiter MassesOrbital Distance 0.0378 AUOrbital Period 2.52 DaysAtmospheric Temperature 1800 KMid-point of Transit 2453151.4860 HJD
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WASP 12: Hottest Transiting Giant Planet
High quality light curve for accurate parameters
Discovery data
Doppler confirmation
Orbital Period: 1.09 dTransit duration: 2.6 hrsPlanet Mass: 1.41 MJupiter
Planet Radius: 1.79 RJupiter
Planet Temperature: 2516 KSpectral Type of Host Star: F7 V
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Comparison of WASP 12 to an M8 Main Sequence Star
Planet Mass: 1.41 MJupiter
Planet Radius: 1.79 RJupiter
Planet Temperature: 2516 K
Mass: 60 MJupiter
Radius: ~1 RJupiter
Teff: ~ 2800 K
WASP 12 has a smaller mass, larger radius, and comparableeffective temperature than an M8 dwarf. Its atmosphereshould look like an M9 dwarf or L0 brown dwarf. One difference: above temperature for the planet is only on the dayside because the planet does not generate its own energy
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GJ 436: The First Transiting Neptune
Host Star:
Mass = 0.4 Mּס (M2.5 V)Butler et al. 2004
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Special Transits: GJ 436
Butler et al. 2004
„Photometric transits of the planet across the star are ruled out for gas giantcompositions and are also unlikely for solid compositions“
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The First Transiting Hot Neptune!
Gillon et al. 2007
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GJ 436
StarStellar mass [ Mּס ] 0.44 ( ± 0.04) PlanetPeriod [days] 2.64385 ± 0.00009 Eccentricity 0.16 ± 0.02 Orbital inclination 86.5 0.2Planet mass [ ME ] 22.6 ± 1.9Planet radius [ RE ] 3.95 +0.41
-0.28
Mean density = 1.95 gm cm–3, slightly higher than Neptune (1.64)
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HD 17156: An eccentric orbit planet
M = 3.11 MJup
Probability of a transit ~ 3%
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Barbieri et al. 2007
R = 0.96 RJup
Mean density = 4.88 g/cm3
Mean for M2 star ≈ 4.3 g/cm3
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ρ = 4.44 (cgs)R = 1.03 RJupHD 80606: Long period and eccentric
a = 0.45 AU
dmin = 0.03 AU dmax = 0.87 AU
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MEarth-1b: A transiting Superearth
D Charbonneau et al. Nature 462, 891-894 (2009) doi:10.1038/nature08679
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Change in radial velocity of GJ1214.
D Charbonneau et al. Nature 462, 891-894 (2009) doi:10.1038/nature08679
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ρ = 1.87 (g/cm3)
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So what do all of these transiting planets tell us?
ρ = 1.24 g/cm3 ρ = 0.62 g/cm3
ρ = 1.25 g/cm3 1.6 g/cm3
5.5 g/cm3
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The density is the first indication of the internal structure of the exoplanet
Solar System Object ρ (g cm–3)Mercury 5.43Venus 5.24Earth 5.52Mars 3.94Jupiter 1.24Saturn 0.62Uranus 1.25Neptune 1.64Pluto 2Moon 3.34CarbonaceousMeteorites
2–3.5
Iron Meteorites 7–8Comets 0.06-0.6
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Take yourfavoritecompositionand calculatethe mass-radiusrelationship
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Masses and radii of transiting planets.
H/He dominated
Pure H20
75% H20, 22% Si
67.5% Si mantle32.5% Fe(earth-like)
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(Sasselov 2008)
CoRoT 7b
Cold & Hot Jupiters
Hot Neptunes
Super Earths
The mass-radius relationship of planets depends on their mass, composition and inner structure
The mass-radius relationship of planets depends on their mass, composition and inner structure
CoRoT 2b
CoRoT 9b
CoRoT 5b
CoRoT 6b
Kepler 7b
Kepler 6b
Kepler 8b
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N
JS
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HD 149026: A planet with a large core
Period = 2.87 d
Rp = 0.7 RJup
Mp = 0.36 MJup
Sato et al. 2005
Mean density = 2.8 gm/cm3
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~70 Mearth core mass is difficult to form with gravitational instability.
HD 149026 b provides strong supportfor the core accretion theory
10-13 Mearth core
Rp = 0.7 RJup
Mp = 0.36 MJup
Mean density = 2.8 gm/cm3
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Planet Radius
Most transiting planets tend to be inflated. Approximately 68% of all transiting planets have radii larger than 1.1 RJup.
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Possible Explanations for the Large Radii
1. Irradiation from the star heats the planet and slowsits contraction it thus will appear „younger“ than it isand have a larger radius
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Possible Explanations for the Large Radii
2. Slight orbital eccentricity (difficult to measure) causes tidal heating of core → larger radius
Slight Problem:
HD 17156b: e=0.68 R = 1.02 RJup
HD 80606b: e=0.93 R = 0.92 RJup
CoRoT 10b: e=0.53 R = 0.97RJup
Caveat: These planets all have masses 3-4 MJup, so it maybe the smaller radius is just due to the larger mass.
3. We do not know what is going on.
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Density Distribution
0
2
4
6
8
10
12
14
0.2 0.6 1.0 1.4 1.8 2.2 2.6 3.0
N
J/US N
Density (cgs)
Num
ber
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Comparison of Mean Densities
Giant Planets with M < 2 MJup : 0.78 cgs
HD 17156, P = 21 d, e= 0.68 M = 3.2 MJup, density = 3.8
HD 80606, P = 111 d, e=0.93, M = 3.9 MJup, density = 6.4
CoRoT 10b, P=13.2, e= 0.53, M = 2.7 MJup, density = 3.7
CoRoT 9b, P = 95 d, e=0.12, M = 1 MJup, density = 0.93
The three eccentric transiting planets have high massand high densities. Formed by mergers?
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02468
10121416
0.25 1.75 3.25 4.75 6.25 7.75 9.25
TransitsRV
Period (Days)
Num
ber
Period Distribution for short period Exoplanets
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Both RV and Transit Searches show a peak in thePeriod at 3 days
The ≈ 3 day period may mark the inner edge of theproto-planetary disk, => where migration stops?
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Mass-Radius Relationship
Kepler 11b
Radius is roughly independent of mass, until you get to small planets(rocks)
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Planet Mass Distribution
TransitingPlanets
RV Planets
Close in planetstend to havelower mass, as we have seenbefore.
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0
5
10
15
20
25
30
0.5 0.7 0.9 1.1 1.3 1.5
4050607080
Host Star Mass Distribution
Nm
ber
TransitingPlanets
RV Planets
0102030
0.5 0.7 0.9 1.1 1.3 1.5
Stellar Mass (solar units)
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Stellar Magnitude distribution of ExoplanetDiscoveries
0,00%
5,00%
10,00%
15,00%
20,00%
25,00%
30,00%
35,00%
0.5 4,50 8,50 12,50 16,50
TransitsRV
Perc
ent
V- magnitude
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Summary of Global Properties of Transiting Planets
1. Mass – Radius Diagram !!!! => internal composition
2. Transiting giant planets (close-in) tend to have inflated radii(much larger than Jupiter)
3. A significant fraction of transiting giant planets are found aroundearly-type stars with masses ≈ 1.3 Msun.
4. The period distribution of close-in planets peaks around P ≈ 3 days.
5. Most transiting giant planets have densities near that of Saturn. It is not known if this is due to their close proximity to the star(i.e. inflated radius)
6. Transiting planets have been discovered around stars fainterthan those from radial velocity surveys
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•
• Early indications are that the host stars of transitingplanets have different properties than non-transitingplanets (more details later).
• Most likely explanation: Transit searches are not as biased as radial velocity searches. One looks fortransits around all stars in a field, these are not pre-selected. The only bias comes with which ones arefollowed up with Doppler measurements
• Caveat: Transit searches are biased against smallerstars. i.e. the larger the star the higher probability thatit transits
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The Rossiter-McClaughlin Effect
1
1
2
3
4
2 3 4
+v
0
–v
The R-M effect occurs in eclipsing systems when the companion crosses in front of the star. This creates a distortion in the normal radial velocity of thestar. This occurs at point 2 in the orbit.
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The effect was discovered in 1924 independently by Rossiter and McClaughlin
Curves show Radial Velocity afterremoving the binary orbital motion
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The Rossiter-McLaughlin Effect or„Rotation Effect“
For rapidly rotating stars you can „see“ the planet in the spectral line
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The Rossiter-McClaughlin Effect
–v+v
When the companion covers thereceeding portion of the star, you seemore negatve velocities of the star rotatingtowards you. You thus see a displacementto negative RV.
–v +v
0
As the companion cosses the star theobserved radial velocity goes from + to –(as the planet moves towards you the staris moving away). The companion coverspart of the star that is rotating towardsyou. You see more positive velocities fromthe receeding portion of the star) you thussee a displacement to + RV.
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The Rossiter-McClaughlin Effect
What can the RM effect tell you?
Planet
a
1) The orbital inclination
a2
a2
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The Rossiter-McClaughlin Effect
2) The direction of the orbit
Planet
b
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The Rossiter-McClaughlin Effect
2) The alignment of the orbit
cd
Planet
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Orbital planeλ
What can the RM effect tell you?
3. Are the spin axes aligned?
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HD 209458
λ = –0.1 ± 2.4 deg
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What about HD 17156?
Narita et al. (2007) reported a large (62 ± 25 degree) misalignment between planet orbit and star spin axes!
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Cochran et al. 2008: λ = 9.3 ± 9.3 degrees → No misalignment!
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XO-3-bHebrard et al. 2008
λ = 70 degrees
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Winn et al. (2009) recent R-M measurements for X0-3
λ = 37 degrees
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Fabricky & Winn, 2009, ApJ, 696, 1230
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HAT-P7
λ = 182 deg!
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HIRES data: M. Endl HARPS data : F. Bouchy Model fit: F. PontLambda ~ 80 deg!
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Summary of R-M measurements:
0
2
4
6
8
10
12
14
-160 -80 0 80 160
Number
λ (deg)40% of Short Period Exoplanets show significant misalignments
20% of Short Period Exoplanets are even in retrograde orbits
What are the implications? Very violent past, probably due to gravitational scattering of 2 (or more) gas giant planets!