Peter Wheatley (PS009) p.j.wheatley@warwick.ac.uk PX437 EXOPLANETS Peter Wheatley (PS009) p.j.wheatley@warwick.ac.uk

Materials Outline Introduction (Solar system and planet formation) Research papers: See list on module page. Book (not essential): The Exoplanet Handbook, Perryman, CUP, 2012, £30 Outline Introduction (Solar system and planet formation) Protoplanetary and debris discs Indirect detection by reflex motion of star Transiting exoplanets Microlensing and direct imaging Extra-terrestrial life

IAU Asteroid belt Kuiper belt Terrestrial planets Gas giants Ice giants IAU

Planets, dwarf planets, small solar-system bodies Ceres: dwarf planet Typical asteroid: small solar-system body HST

Evolutionary tracks - luminosity Burrows et al. 1997, ApJ 491, 856 Burrows et al. 2001, RvMP, 73, 719 Stars Brown dwarfs Planets Jupiter Saturn Evolutionary tracks - luminosity

Evolutionary tracks - radius Stars Brown dwarfs Burrows et al. 2001, RvMP, 73, 719 Planets Evolutionary tracks - radius

Mass-radius relation Jupiter

Equations of state Stevenson 1982 AREPS 10, 257

Composition of solar system planets Stevenson 1982 AREPS 10, 257

IAU Asteroid belt Kuiper belt Terrestrial planets Gas giants Ice giants IAU

Nebula hypothesis Rich Townsend, UCL Believe Sun and planets formed from a Solar Nebula, rotation + collapse => disk. Rich Townsend, UCL

Protoplanetary disc Image: NASA/JPL-Caltech/T. Pyle (SSC)

Tidal model Stephen Oxley

Minimum Mass Solar Nebula Hayashi 1981 Duncan Forgan

Cosmic abundance (by number) Element Abundance (per 100,000) Common molecules H 92,700 H2 (He) 7,200 O 50 H20 (Ne) 20 N 15 NH3 C 8 CH4 Si 2 Mg2SiO4 Mg Fe 1 Fe3O4

Condensation by temperature Condensation temperature Materials Examples 1400-1700 K Ca Al Ti compounds Al2O3 CaTiO3 refractory elements common elements 1300-1400 K Mg, Si compounds Mg2SiO4 MgSiO3 1350 K metallic iron alloys Fe 370 K magnetite Fe3O4 180 K water ice H20 volatile Elements 130 K ammonia hydrate NH3·H20 40-80 K methane, methane ices CH4 CH4·7H20

Growth of solids Blum et al 1998 Blum & Wurm 2008

Gas drag and planetesimal migration Rice et al 2004

Gas accretion Pollack et al 1996

Disc evaporation Duncan Forgan

Single-slit diffraction

Spectrum of a planet

So the problem is imaging a v faint object v close to a bright star So the problem is imaging a v faint object v close to a bright star. It is a problem of contrast. Example here does have a planet, but detected in directly. 51 Peg in DSS-II