the 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 (Spectroscopic Transits). - PowerPoint PPT PresentationTRANSCRIPT
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The Transit Method: Results from the Ground
I. Results from individual transit search programsII. The Mass-Radius relationships (internal structure)
Global Properties
III. The Rossiter-McClaughlin Effect (Spectroscopic Transits)
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The first time I gave this lecture (2003) there were 2 transiting extrasolar planets.
There are now 127 transiting extrasolar planets detected from ground-based programs
First ones were detected by doing follow-up photometry of radial velocity planets. Now transit searches are discovering exoplanets
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Radial Velocity Curve for HD 209458
Period = 3.5 days
Msini = 0.63 MJupThe probability is 1 in 10 that a short period Jupiter 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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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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K = 510 ± 170 m/s
i= 79.8 ± 0.3
a= 0.0308
Mass = 4.5 MJ
Radius = 1.6 RJ
Spectral Type Star = F3 V
Vsini = 40 km/s
OGLE transiting planets: These produce low quality transits, they are faint, and they take up a large
amount of 8m telescope time..
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Planet Mass
(MJup)
Radius
(RJup)
Period
(Days)
Year
OGLE2-TR-L9 b 4.5 1.6 2.48 2007
OGLE-TR-10 b 0.63 1.26 3.19 2004
OGLE-TR-56 b 1.29 1.3 1.21 2002
OGLE-TR-111 b 0.53 1.07 4.01 2004
OGLE-TR-113 b 1.32 1.09 1.43 2004
OGLE-TR-132 b 1.14 1.18 1.69 2004
OGLE-TR-182 b 1.01 1.13 3.98 2007
OGLE-TR-211 b 1.03 1.36 3.68 2007
Prior to OGLE all the RV planet detections had periods greater than about 3 days.
The last OGLE planet was discovered in 2007. Most likely these will be the last because the target stars are too faint.
The OGLE Planets
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The TrES Planets
• TrES: Trans-atlantic Exoplanet Survey (STARE is a member of the network http://www.hao.ucar.edu/public/research/stare/)
• Three 10cm telescopes located at Lowell Observtory, Mount Palomar and the Canary Islands
• 6.9 square degrees
• 5 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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Report that the transit duration is increasing with time, i.e. the inclination is changing:
However, Kepler shows no change in the inclination!
Discrepancy most likely due to wavelength depedent limb darkening
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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
• 36 Planets discovered
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HAT-P-12b
Star = K4 VPlanet Period = 3.2 days
Planet Radius = 0.96 RJup
Planet Mass = 0.21 MJup (~MSat)= 0.3 gm 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
• 2 sites: La Palma, South Africa
• 65 transiting planets discovered so far
In a field of 400.000 stars WASP finds 12 candidates for a rate of 1 in 30.000 stars. If 10% are real planets the rate is 1 planet for every 300.000
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The First WASP Planet
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CoordinatesRA 00:20:40.07 Dec +31:59:23.7
Constellation Pegasus
Apparent Visual Magnitude 11.79
Distance from Earth 1234 Light Years
WASP-1 Spectral Type F7V
WASP-1 Photospheric Temperature
6200 K
WASP-1b Radius 1.39 Jupiter Radii
WASP-1b Mass 0.85 Jupiter Masses
Orbital Distance 0.0378 AU
Orbital Period 2.52 Days
Atmospheric Temperature 1800 K
Mid-point of Transit 2453151.4860 HJD
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WASP 12b: The Hottest Transiting Giant Planet
Discovery data
High quality light curve for accurate parameters
Doppler confirmation
Orbital Period: 1.09 d
Transit duration: 2.6 hrs
Planet Mass: 1.41 MJupiter
Planet Radius: 1.79 RJupiter
Planet Temperature: 2516 K
Spectral Type of Host Star: F7 V
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Mass: 60 MJupiter
Radius: ~1 RJupiter
Teff: ~ 2800 K
Planet Mass: 1.41 MJupiter
Planet Radius: 1.79 RJupiter
Planet Temperature: 2516 K
Comparison of WASP 12 to an M8 Main Sequence Star
WASP 12 has a smaller mass, larger radius, and comparable effective temperature than an M8 dwarf. Its atmosphere should look like an M9 dwarf or L0 brown dwarf. One difference: above temperature for the planet is only on the day side because the planet does not generate its own energy
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Although WASP-33b is closer to the planet than WASP-12 it is not as hot because the host star is cooler (4400 K) and it has a smaller radius
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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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„Photometric transits of the planet across the star are ruled out for gas giant compositions and are also unlikely for solid compositions“
Special Transits: GJ 436
Butler et al. 2004
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The First Transiting Hot Neptune!
Gillon et al. 2007
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Star
Stellar mass [ Mּס ] 0.44 ( ± 0.04)
Planet
Period [days] 2.64385 ± 0.00009
Eccentricity 0.16 ± 0.02
Orbital inclination 86.5 0.2
Planet mass [ ME ] 22.6 ± 1.9
Planet radius [ RE ] 3.95 +0.41-0.28
GJ 436
Mean density = 1.95 gm cm–3, slightly higher than Neptune (1.64)
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M = 3.11 MJup
HD 17156: An eccentric orbit planet
Probability of a transit ~ 3%
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R = 0.96 RJup
Barbieri et al. 2007
Mean density = 4.88 gm/cm3
Mean for M2 star ≈ 4.3 gm/cm3
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HD 80606: Long period and eccentric
a = 0.45 AU
dmin = 0.03 AU dmax = 0.87 AU
R = 1.03 RJup = 4.44 (cgs)
Probability of having a favorable orbital orientation is only 1%!
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D Charbonneau et al. Nature 462, 891-894 (2009) doi:10.1038/nature08679
MEarth-1b: A transiting Superearth
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D Charbonneau et al. Nature 462, 891-894 (2009) doi:10.1038/nature08679
Change in radial velocity of GJ1214.
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= 1.87 (cgs)
Neptune like
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So what do all of these transiting planets tell us?
= 1.24 gm/cm3 = 0.62 gm/cm3
= 1.25 gm/cm3 1.6 gm/cm3
5.5 gm/cm3
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Solar System Object (gm cm–3)
Mercury 5.43
Venus 5.24
Earth 5.52
Mars 3.94
Jupiter 1.24
Saturn 0.62
Uranus 1.25
Neptune 1.64
Pluto 2
Moon 3.34
Carbonaceous Meteorites
2–3.5
Iron Meteorites 7–8
Comets 0.06-0.6
The density is the first indication of the internal structure of the exoplanet
Rocks
He/H
Ice
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D Charbonneau et al. Nature 462, 891-894 (2009) doi:10.1038/nature08679
Masses and radii of transiting planets.
GJ 1214b is shown as a red filled circle (the 1σ uncertainties correspond to the size of the symbol), and the other known transiting planets are shown as open red circles. The eight planets of the Solar System are shown as black diamonds. GJ 1214b and CoRoT-7b are the only extrasolar planets with both well-determined masses and radii for which the values are less than those for the ice giants of the Solar System. Despite their indistinguishable masses, these two planets probably have very different compositions. Predicted16 radii as a function of mass are shown for assumed compositions of H/He (solid line), pure H2O (dashed line), a hypothetical16 water-dominated world (75% H2O, 22% Si and 3% Fe core; dotted line) and Earth-like (67.5% Si mantle and a 32.5% Fe core; dot-dashed line). The radius of GJ 1214b lies 0.49 ± 0.13 R above the water-world curve, indicating that even if the planet is predominantly water in composition, it ⊕probably has a substantial gaseous envelope
H/He dominated
Pure H20
75% H20, 22% Si67.5% Si mantle
32.5% Fe
(earth-like)
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Take your favorite composition and calculate the mass-radius relationship
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Period = 2.87 d
Rp = 0.7 RJup
Mp = 0.36 MJup
Sato et al. 2005
HD 149026: A planet with a large core
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 support for the core accretion theory
Rp = 0.7 RJup
Mp = 0.36 MJup
Mean density = 2.8 gm/cm3
10-13 Mearth core
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Lower bound
= 0.15 gm cm–3
Upper bound
= 3 gm cm–3
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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 slows its contraction it thus will appear „younger“ than it is and have a larger radius
Models I, C, and D are for isolated planets
Models A and B are for irradiated planets.
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There is a slight correlation of radius with planet temperature (r = 0.37)
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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:
3. We do not know what is going on.
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 may be the smaller radius is just due to the larger mass.
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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 Distribution
Density (cgs)
Nu
mb
er
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Comparison of Mean Densities of eccentric planets
Giant Planets with M < 2 MJup : 0.78 cgs
HD 17156, P = 21 d, e= 0.68 M = 3.2 MJup, density = 4.8
HD 80606, P = 111 d, e=0.93, M = 3.9 MJup, density = 4.4
CoRoT 10b, P=13.2, e= 0.53, M = 2.7 MJup, density = 3.7
The three eccentric transiting planets have high mass and high densities. Formed by mergers?
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0
2
4
6
8
10
12
14
16
0.25 1.75 3.25 4.75 6.25 7.75 9.25
Transits
RV
Period (Days)
Nu
mb
erPeriod Distribution for short period Exoplanets
p = 7%
p = 13%
p = probability of a favorable orbit
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The ≈ 3 day period may mark the inner edge of the proto-planetary disk
Both RV and Transit Searches show a peak in the Period at 3 days
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Mass-Radius Relationship
Radius is roughly independent of mass, until you get to small planets (rocks)
Rad
ius
(RJ)
Mass (MJ)
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Modified From H. Rauer
CoRoT-3b : Radius = Jupiter, Mass = 21.6 Jupiter
CoRoT-1b : Radius = 1.5 Jupiter, Mass = 1 Jupiter
OGLE-TR-133b: Radius = 1.33 Jupiter, Mass = 85 Jupiter
CoRoT-1b
CoRoT-3b
OGLE-TR-133b
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Planet Mass Distribution
Transiting Planets
RV Planets
Close in planets tend to have lower mass, as we have seen before.
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0
2
4
6
8
10
12
14
16
18
-0.45 -0.25 -0.05 0.15 0.35
Transits
[Fe/H]
Num
ber 0
10
20
30
40
50
60
70
-0.45 -0.25 -0.05 0.15 0.35
RV
Metallicity Distribution
[Fe/H] Doppler result: Recall that stars with higher metal content seem to have a higher frequency of planets. This is not seen in transiting planets.
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0
5
10
15
20
25
30
0.5 0.7 0.9 1.1 1.3 1.5
0
10
20
30
40
50
60
70
80
0.5 0.7 0.9 1.1 1.3 1.5
Host Star Mass Distribution
Stellar Mass (solar units)
Nu
mb
erTransiting Planets
RV Planets
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V- magnitude
Per
cen
t
Stellar Magnitude distribution of Exoplanet Discoveries
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
Transits
RV
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Summary of Global Properties of Transiting Planets
1. Transiting giant planets (close-in) tend to have inflated radii (much larger than Jupiter)
2. A significant fraction of transiting giant planets are found around early-type stars with masses ≈ 1.3 Msun.
3. There appears to be no metallicity-planet connection among transiting planets or at most a weak one.
4. The period distribution of close-in planets peaks around P ≈ 3 days for both RV and transit discovered planets.
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 fainter than those from radial velocity surveys
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• Early indications are that the host stars of transiting planets have slightly different properties than non-transiting planets.
• Most likely explanation: Transit searches are not as biased as radial velocity searches. One looks for transits around all stars in a field, these are not pre-selected. The only bias comes with which ones are followed up with Doppler measurements
• Caveat: Transit searches are biased against smaller stars. i.e. the larger the star the higher probability that it transits
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Spectroscopic Transits:
The Rossiter-McClaughlin Effect
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The Rossiter-McClaughlin Effect
1
1
0
+v
–v
2
3
4
2 3 4
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 the star. This occurs at point 2 in the orbit.
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From Holger Lehmann
The Rossiter-McLaughlin Effect in an Eclipsing Binary
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Curves show Radial Velocity after removing the binary orbital motion
The effect was discovered in 1924 independently by Rossiter and McClaughlin
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Spectral Type
Vequator (km/s)
O5 190
B0 200
B5 210
A0 190
A5 160
F0 95
F5 25
G0 12
Average rotational velocities in main sequence stars
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The Rossiter-McClaughlin Effect
–v +v
0
As the companion cosses the star the observed radial velocity goes from + to – (as the planet moves towards you the star is moving away). The companion covers part of the star that is rotating towards you. You see more possitive velocities from the receeding portion of the star) you thus see a displacement to + RV.
–v
+v
When the companion covers the receeding portion of the star, you see more negatve velocities of the star rotating towards you. You thus see a displacement to negative RV.
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The Rossiter-McClaughlin Effect
What can the RM effect tell you?
Planet
1) The orbital inclination or impact parameter
a
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
Planet
cd
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What can the RM effect tell you?
3. Are the spin axes aligned?
Orbital plane
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Summary of Rossiter-McClaughlin „Tracks“
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Amplitude of the R-M effect:
ARV = m s–
1
Note:
1. The Magnitude of the R-M effect depends on the radius of the planet and not its mass.
2. The R-M effect is proportional to the rotational velocity of the star. If the star has little rotation, it will not show a R-M effect.
rRJup
( )2
RRּס
( )–2Vs
5 km s–1 ( )ARV is amplitude after removal of orbital mostion
Vs is rotational velocity of star in km s–1
r is radius of planet in Jupiter radii
R is stellar radius in solar radii
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= –0.1 ± 2.4 deg
HD 209458
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= –1.4 ± 1.1 deg
HD 189733
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HD 147506
Best candidate for misalignment is HD 147506 because of the high eccentricity
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Two possible explanations for the high eccentricities seen in exoplanet orbits:
• Scattering by multiple giant planets
• Kozai mechanism
On the Origin of the High Eccentricities
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Planet-Planet Interactions
Initially you have two giant planets in circular orbits
These interact gravitationally. One is ejected and the remaining planet is in an eccentric orbit
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Kozai Mechanism
Two stars are in long period orbits around each other.
A planet is in a shorter period orbit around one star.
If the orbit of the planet is inclined, the outer planet can „pump up“ the eccentricity of the planet. Planets can go from circular to eccentric orbits.
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Winn et al. 2007: HD 147506b (alias HAT-P-2b)
If either mechanism is at work, then we should expect that planets in eccentric orbits not have the spin axis aligned with the stellar rotation. This can be checked with transiting planets in eccentric orbits
Spin axes are aligned within 14 degrees (error of measurement). No support for Kozai mechanism or scattering
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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: = 9.3 ± 9.3 degrees → No misalignment!
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XO-3-b
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Hebrard et al. 2008
= 70 degrees
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Winn et al. (2009) recent R-M measurements for X0-3
= 37 degrees
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Fabricky & Winn, 2009, ApJ, 696, 1230
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= 182 deg!
HAT-P7
= 182 deg!
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HD 80606
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= 32-87 deg
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HARPS data : F. Bouchy Model fit: F. Pont Lambda ~ 80 deg!
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Distribution of spin-orbit axes
Red: retrograde orbits
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0
2
4
6
8
10
12
14
16
18
-160 -80 0 80 160
Number
35% of Short Period Exoplanets show significant misalignments
~10-20% of Short Period Exoplanets are in retrograde orbits
Basically all angles are covered
(deg)
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2.
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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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For stars whose spectral line profiles are dominated by rotational broadening there is a one to one mapping between location on the star and location in the line profile:
V = –Vrot V = +Vrot
V = 0
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For slowly rotationg stars you do not see the distortion, but you measure a radial velocity displacement due to the distortion.
A „Doppler Image“ of a Planet
Prograde orbit
Retrograd orbit
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HD 15082 = WASP-33
No RV variations are seen. A companion of radius 1.5 RJup is either a planet, brown dwarf, or low mass star. The RV variations exclude BD
and stellar companion.
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The Line Profile Variations of HD 15082 = WASP-33
Pulsations
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Summary
1. There are 2 ways from spectroscopy to measure the angle between the spin axis and the orbital axis of the star:
a) Rossiter-McClaughlin effect (most successful)
b) Doppler tomography
2. No technique can give you the mass
3. Exoplanets show all possible obliquity angles, but most are aligned (even in eccentric orbits)
4. Implications for planet formation (problems for migration theory)