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Jean-Pierre needs to be brought up to date
on what’s really going on in astronomy
these days!
Extrasolar Planets
Caroline Terquem
Institut d’Astrophysique de Paris
Université Paris 6
Detection of extrasolar
planets
Transits (1999): 27
Radial velocity (Doppler)
(1995): 241
Gravitational lensing (2006): 4
Direct
imaging
(2004): 4
1995: First extrasolar planet around
a solar like star
inner solar system
51 Pegasi
249 planets
25 multiple systems
(October 11, 2007)
http://exoplanet.eu/
Masses of
extrasolar planets
Planet mass (Jupiter mass)
mass vs semi-major axis
10
1
0.1
0.01
0.01
0.1
1
Semi-major axis (UA)
10
Eccentricity
eccentricity vs mass
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0.01
0.1
1
Mass (Jupiter mass)
10
100
Giant planet formation
Accretion of a core
Capture of a gaseous envelope
 Critical core mass
Planet migration
(L. Cook)
Hot Jupiter and Neptunes:
in situ formation:
too hot
not enough material
Resonant planets:
capture
(G. Bryden)
Tidal torques
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(Goldreich & Tremaine ‘79)
Type I migration
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(Goldreich & Tremaine, Ward)
Type I migration
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1
1 / 2
2
M



r
H
 

pl
2

t ( yr )  108 
10




2 
M
g
/
cm
au
r
 
 earth
  
Type II migration
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(Goldreich & Tremaine, Papaloizou & Lin)
Type II migration
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2
2
1 r 
0.2  r   r 
t ( yr )      
   
H
  H   au 
3/ 2
Disk-planet interaction
Geoff Bryden
Migration rate
2D
3D
(Bate et al. ’03)
Planets around
pulsars
3 planets
resonance (3:2), with e ≈ 0
→ formation in a disk
Planets around pulsars
A. Wolszczan & D. Frail, 1992
Can a planet survive the supernova explosion?
 Red giant phase: the planet may be engulfed by the star
 Supernova explosion:
• Mass loss: if more than half the stellar mass is lost,
the planet escapes
• Shock wave: if Ekinetic » Ebinding, the planet is destroyed
Ekinetic = EpRp2/(4pD2) with E=1051 ergs
Ebinding = -GMp2/Rp = -10-2 Ec → ???
Conclusions
Come back in a few years.
(Maybe there will be some for
Jean-Pierre’s 70th birthday.)