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

2. 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

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

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

5. 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

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

7. Mass-radius relation
Jupiter

8. Equations of state
Stevenson 1982 AREPS 10, 257

9. Composition of solar system planets
Stevenson 1982 AREPS 10, 257

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

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

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

13. Tidal model
Stephen Oxley

14. Minimum Mass Solar Nebula
Hayashi 1981
Duncan Forgan

15. 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

16. Condensation by temperature
Condensation temperature
Materials
Examples K
Ca Al Ti compounds
Al2O3 CaTiO3
refractory elements
common elements 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

17. Growth of solids
Blum et al 1998
Blum & Wurm 2008

18. Gas drag and planetesimal migration
Rice et al 2004

19. Gas accretion
Pollack et al 1996

20. Disc evaporation
Duncan Forgan

21. Single-slit diffraction

23. Spectrum of a planet

24. 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