actuality of exoplanets search · 20 multiple systems ~ 25 % of the exoplanets. seems to favor the...
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Actuality of Actuality of ExoplanetsExoplanets SearchSearch
François BouchyOHP - IAP
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How detect extrasolar planets ?
Two main difficulties :
1 – A tiny angular separation
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Sun – Jupiter at 4 light years4”
Sun – Jupiter at 100 light years0.15”
Sun – Earth at 100 light years0.03”
0.75 arcsec
0.12 arcsec
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How detect extrasolar planets ?
Two main difficulties :
1 – A tiny angular separation2 – A huge contrast in luminosity
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The star is up to 1 billion timesbrighter than the planet
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109 105
Fp/Fstar ~ (Rp/a)2
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One solution : detect the dynamicalperturbation induced of the star
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Period : 11.9 ansDistance : 5.2 auVelocity : 13 km.s-1
Period : 11.9 yearsDistance : 0.005 auVelocity : 12 m.s -1
Sun displacement
Jupiter orbit
Dynamical pertubation of Jupiter on the Sun
C.G.
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Detection by radial velocityBased on the Doppler-Fizeau Effect
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Keplerian orbit parameters
Orbital fit 6 parameters of keplerian orbit :V0, K, P, e, Tp, w
[ ]wewteP
iamM
mVrad cos))(cos(1sin2
2++
−⋅
+=
∗
νπ
[ ]wewtKVVrad cos))(cos(0 ++⋅+= ν
]M[*]AU[
sin]M[45.28]/[
SUNMa
imsmK Jup
⋅⋅=
][][
sin][203]/[ 3/13/2 dPMM
iMmsmK
SUN
Jup
⋅⋅=
∗
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3 km/s
1 CCD pixel = 15 μm = 800 m/s1 m/s 20 nm
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Improvement of Doppler techniques
1
10
100
1000
1965 1970 1975 1980 1985 1990 1995 2000 2005
years
m/s
CORAVEL
HARPS
CORALIE
ELODIE
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Another solution : Detect the shadow of the planet
- photometric transit -
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Transit ProbabilityaRp *=
For 1 Rsun and 1 Msun ][24[%] 3/2 daysP
p =
p = 3 days 11 % p = 10 days 5 % p = 100 days 1 % p = 365 days 0.47 %
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Duration ΔT ~ R P1/3(m+M)-1/3 √1-b2
Ingress/Egress
dt ~ ΔT r / R √1-b2
Depth
d ~ (r/R)2
r, m R, M
b
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3 relations :
ΔT ~ R P1/3 M-1/3 √1-b2
d ~ (r/R)2
dt ~ ΔT r / R √1-b2
…. but 5 unknowns :
r, R, m, M, b
Light curve fit:
r/R
R M-1/3
b
Radial velocity
m / M2/3
Spectroscopy
M, R
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Gravitational microlensing
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Pulsar timing
][][
][6.1][ 3/2
3/4 yearPMM
MMms
Sunpulsar
Earthp ⋅⋅=τ
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1995 : discovery of 51 Peg bFirst extrasolar planet orbiting a solar-type star
K = 59 m.s-1
P = 4.23 daysmp.sini = 0.47 MJa = 0.05 AU
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Status : 200 known extrasolar planets
Earth
Jup
Sat51 Pegb
188 RV10 transit4 microlensing4 imaging4 pulsar
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0) A huge diversity of orbital parameters (P, a, e)
1) no massive planets (> 2MJup) with short period (P<100d)
2) maximum mass increases with orbital distance
3) Lack of planets between 10 et 100 days
4) Lack of planets less massive than Jupiter with long period (P>100d)
5) Peak of planets with short period (3-10 d)
6) Nb of planets increases with period (for P>100 d)
Main properties of orbital parameters
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Migration of HJ due to tidal interaction with diskMore efficient for low mass planets
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Some evidences of planetary fall
Some evidences of planetary evaporation
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Ups And b
Ups And c
Ups And d
20 multiple systems ~ 25 % of the exoplanets
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Seems to favor the eccentricity
Some resonant systems
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Properties of exoplanet-host stars
Stars with planets
Stars without planets
1) Planet host stars have higher metallicity
2) Probability to find a planete increase with metallicity
Over metallicity seems to favour the planetary formation
! This is not the case for Neptune and Big-Earth like planets
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19 planets around binaries
1) Massive planets (msini > 2 MJup) with short periods are around binaries
2) Short period planets orbiting binaries have low eccentricity
Migration process is different in binaries
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Stellar mass [Msun]
Plan
et m
ass [
Mju
p]Mass of the central star
Only 5 planets detected around M dwarves (M < 0.6 Msun) including 3 Hot Neptunes.
Smaller disk around M dwarves do not favor the formation and the migration of giant planet
3 massive planets detected around F stars
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Toward the low-mass planets
Earth
Jup
Sat
188 RV10 transit4 microlensing4 imaging4 pulsar
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51 Peg ELODIE
K = 59 m/sP = 4.23 j
m = 0.47 MJa = 0.05 UA
K = 107 m/sP = 3.39 j
m = 0.62 MJa = 0.039 UA
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All stars are singing
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Venus of mu Arae
P = 9.55 dK = 4.1 m/s m.sini = 14 Meartha = 0.09 AUO-C = 0.9 m/s
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The trio of Neptunes
P = 8.7 / 31.6 / 197 daysa = 0.08 / 0.19 / 0.63 AU
m.sini = 10.2 / 11.8 / 18.1 MEarth
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Main limitations of RV method
1. Instrumental limitations
2. Stellar limitations
3. Photon noise limitations
- Guiding noise - Wavelength calibration - CCD defaults
-Seismic activity -Photospheric activity -Blend
Possibility to reach 30 cm/s these next years
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4 exoplanets found by microlensingincluding 2 big-earth planets
OGLE235-MOA53bm ~ 2.6 Mjup
a ~ 5.1 UA
OGLE05-071Lm ~ 0.9 Mjup
a ~ 1.8 UA
OGLE05-390Lm ~ 5.5 Mearth
a ~ 2.1 UA
OGLE05-169Lm ~ 13 Mearth
a ~ 2.8 UA
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First image of a young giant planet orbiting a brown dwarf
0.78 arcsec55 A.U.
5 MJup
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~ 2 RJup1 - 42 MJup
0.7 arcsec98 A.U.
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10 characterized planets
Earth
Jup
Sat
188 RV10 transit4 microlensing4 imaging4 pulsar
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10 transiting extrasolar planetsCharacterized by photometry and radial velocity
VHJ
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HD189733b detected and characterized at OHP
P = 2.22 daysm = 1.15 MJupr = 1.2 RJup
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Spectroscopic transit of HD189733(Rossiter - McLaughlin effect)
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Mass – radius relation of the 10 transiting extrasolar planets
VHJ
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Atmosphere Evaporation of HD209458b
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Spitzer IR anti-transits of HD209458b, Tres-1 and HD189733b
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From planets to low-mass stars
OGLE-TR-122b :A planet-size star
Sun1000 MJup
OGLE-TR-122b100 MJup
Jupiter1 MJup
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Photometry + Radial Velocity + Spectroscopy Fully complementary methods
a, P, e, T0, b, α
mp, rp, ρ, mcore , T, evap. , …
R*, M*, [Fe/H], vsini, R’HK , …
Constraints for processes of formation and evolution Constraints for composition and internal structure
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--- 0--- 0--- 0--- 0--- 1--- 0--- 0--- 0--- 0--- 0--- 0--- 0--- 0--- 0--- 0--- 0--- 0--- 5--- 0--- 0--- 0--- 0--- 0--- 6
Lack of efficiency of photometric surveys
More than 200 planets per month were expected
Up to day a total of only 7 detections
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Transit Depth
OGLE-113 2.9% Tres-1 2.3%Xo-1 2.0%OGLE-111 1.9%OGLE-10 1.9%OGLE-56 1.3 %OGLE-132 1.1 %
No transiting planet detected with a depth < 1.1%
1) Insufficient time coverage 2) Difficulties to reach the mmag precision
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Photometric transit of HD209458b
1.4 RJup0.69 MJup0.31 g.cm-3
0.047 A.U.3.524 days
From groundFrom space
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COROT
Space photometric detection of planetary transiting candidates
~100’000 stars observed during 150 days
~ 100 Hot Jupiters~ 10 Hot Neptunes
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SOPHIE
New spectrograph on the 193-cm telescope
North Counter part of HARPS (R~70’000)~ 2 mag more efficient than ELODIE~ 1-2 m/s expected precision
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First laboratory spectrum
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First stellar spectrum[51Peg]
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Expected performances
H.E.H.R.
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Schedule
31 July – 7 August : 1th commissioning21 – 28 August : 2d commissioningSeptember – October : Science verification1th November : Opening to community
Consortium Exoplanet Search in North Hemisphere22 Co-Is from France and Switzerland 200 nights per years
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Next steps
Earth
Jup
Sat