More diversity than expected ?... Some of the Hot Jupiters do not match well models based on Jupiter & Saturn: Laughlin et al. (2005) models; Charbonneau et al (2006) w Bodenheimer et al.(2003), and Burrows et al. (2003) Gaudi (2005) &

Interiors of Giant Planets Our own Solar System: Jupiter & Saturn Constraints: M, R, age, J2, J4, J6 EOS is complicated: mixtures of molecules, atoms, and ions; partially degenerate & partially coupled. EOS Lab Experiments (on deuterium): Laser induced - LLNL-NOVA Gas gun (up to 0.8 Mbar only) Pulsed currents - Sandia Z-machine Converging explosively-driven - Russia (up to 1.07 Mbar)

Phase diagram (hydrogen): Guillot (2005)

Interiors of Giant Planets EOS Experiment Breakthrough ? Russian Converging explosively-driven system (CS) Boriskov et al. (2005): matches Gas gun & Pulsed current (Z-machine) results deuterium is monatomic above 0.5 Mbar - no phase transition consistent with Density Functional Theory calculation (Desjarlais)

Interiors of Giant Planets Jupiter’s core mass and mass of heavy elements: For MZ - the heavy elements are mixed in the H/He envelope Saumon & Guillot (2004)

Interiors of Giant Planets Saturn’s core mass and mass of heavy elements: Saumon & Guillot (2004)

Interiors of Giant Planets Core vs. No-Core: How well is a core defined? Saturn: metallic region can mimic ‘core’ in J2 fit (Guillot 1999); Core dredge-up - 20 MEarth in Jupiter, but MLT convection… ? Overall Z enrichment: Jupiter ~ 6x solar Saturn ~ 5x solar a high C/O ratio from Cassini ?? (HD 209458b? Seager et al ‘05)

Hot Jupiters: Different Interiors ?... Most Hot Jupiters will require large cores and Z or/and Y enrichment: Gaudi (2005) w Bodenheimer et al.(2003), Laughlin et al. (2005) models; and Burrows et al. (2003)

Interiors of Hot Jupiters Core vs. No-Core: Core - leads to faster contraction at any age; the case of OGLE-TR-132b > high-Z and large core needed ? the star OGLE-TR-132 seems super-metal-rich… (Moutou et al.) Cores: nature vs. nurture ? - capturing planetesimals. Evaporation ? - before planet interior becomes degenerate enough - implications for Very Hot Jupiters; the case of HD 209458b (Vidal-Madjar et al. 2003) ? Overall Z enrichment: After the initial ~1 Gyr leads to more contraction.

Summary: Hot Jupiters Our gas giants - Jupiter & Saturn: have very small cores are enriched in elements heavier than H (and He) The Hot Jupters we know: six need cores & enrichment three are on a diet or have a secret affair with another planet … Is the core-accretion model in trouble ? not yet, but we should understand Jupiter and Saturn better.

Conclusions Sizes of extrasolar planets are already precise beware of biases & systematic errors Models are based on Jupiter & Saturn Perhaps, Hot & Very Hot Jupiters are more Z enriched: because of history - excessive migration through disk, or because of orbit - manage to capture more planetesimals ? Implications for the core-accretion model: it requires at least ~6 ME for Mcore of Jupiter & Saturn invoke Jupiter core erosion (e.g. Guillot 2005), use the He settling for Saturn (Fortney & Hubbard 2003)