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Jean-Pierre needs to be brought up to dateon what’s really going on in astronomy these days!

Extrasolar Planets

Caroline TerquemInstitut d’Astrophysique de Paris

Université Paris 6

Detection of extrasolar planets

Transits (1999): 27

Directimaging (2004): 4

Gravitational lensing (2006): 4

Radial velocity (Doppler)(1995): 241

1995: First extrasolar planet around

a solar like star

inner solar system

51 Pegasi

249 planets25 multiple systems

(October 11, 2007)http://exoplanet.eu/

Masses of extrasolar planets

mass vs semi-major axis

0.01

0.1

1

10

Pla

net

mass

(Ju

pit

er

mass

)

0.01 0.1 1 10

Semi-major axis (UA)

eccentricity vs massE

ccen

tric

ity

0.01 0.1 1 10

Mass (Jupiter mass)

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100

Giant planet formation

Accretion of a coreCapture of a gaseous envelope

Critical core mass

(L. Cook)

(G. Bryden)

Hot Jupiter and Neptunes: in situ formation:too hotnot enough material

Resonant planets:capture

Planet migration

(Goldreich & Tremaine ‘79)

Tidal torques

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Type I migration

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(Goldreich & Tremaine, Ward)

Type I migration

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22

2/11

28 10

/10)( ⎟

⎠

⎞⎜⎝

⎛⎟⎠

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⎛ Σ=

−−

rH

aur

cmgMM

yrtearth

pl

Type II migration

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(Goldreich & Tremaine, Papaloizou & Lin)

Type II migration

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2/3222.01

)( ⎟⎠

⎞⎜⎝

⎛⎟⎠

⎞⎜⎝

⎛=Ω⎟⎠

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⎛= 1−

aur

Hr

Hr

yrtαα

Disk-planet interaction

Geoff Bryden

(Bate et al. ’03)

2D

3D

Migration rate

Planets around pulsars

3 planets

resonance (3:2), with e ≈ 0

→ formation in a disk

Planets around pulsars

Can a planet survive the supernova explosion?

Red giant phase: the planet may be engulfed by the star

A. Wolszczan & D. Frail, 1992

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 = ERp2/(4D2) 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.)