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 Direct imaging (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 planets 25 multiple systems (October 11, 2007)

Masses of extrasolar planets

mass vs semi-major axis Planet mass (Jupiter mass) Semi-major axis (UA)

eccentricity vs mass Eccentricity Mass (Jupiter mass) 100

Giant planet formation Accretion of a core Capture of a gaseous envelope  Critical core mass

(L. Cook) (G. Bryden) Hot Jupiter and Neptunes: in situ formation: too hot not enough material Resonant planets: capture Planet migration

( Goldreich & Tremaine ‘79) Tidal torques

Type I migration ( Goldreich & Tremaine, Ward)

Type I migration

Type II migration ( Goldreich & Tremaine, Papaloizou & Lin)

Type II migration

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 E kinetic » E binding, the planet is destroyed E kinetic = E  R p 2 /(4  D 2 ) with E=10 51 ergs E binding = -GM p 2 /R p = E c → ???

Conclusions Come back in a few years. (Maybe there will be some for Jean-Pierre’s 70th birthday.)