More diversity than expected ?...

1
More diversity than expected ?...
Some of the Hot Jupiters do not match well models
based on Jupiter Saturn

Gaudi (2005) Charbonneau et al (2006) w
Bodenheimer et al.(2003), Laughlin et al. (2005)
models and Burrows et al. (2003)
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
Jupiters 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
Saturns core mass and mass of heavy elements

Saumon Guillot (2004)
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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)

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)
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Interiors of Hot Jupiters

• Core vs. No-Core
• Core - leads to faster contraction at any age
• the case of OGLE-TR-132b gt 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.

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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.

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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)