1. 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) &

2. 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)

3. Phase diagram (hydrogen):
Guillot (2005)

4. 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)

5. 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)

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

7. 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 b? Seager et al ‘05)

8. 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)

9. 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 b (Vidal-Madjar et al. 2003) ?
Overall Z enrichment:
After the initial ~1 Gyr leads to more contraction.

10. 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.

11. 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)