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Formation and composition of extrasolar planets

Formation and composition of extrasolar planets. LINZ - SEPT. 5, 2013. A. Thiabaud - U. Marboeuf - Y. Alibert - N. Cabral I. Leya - K. Mezger. Introduction. WHAT COMPOSITION CAN TELL US. Composition of planets is linked to its structure. Knowing it can provide informations on :

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Formation and composition of extrasolar planets

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  1. Formation and composition of extrasolar planets LINZ - SEPT. 5, 2013 • A. Thiabaud - U. Marboeuf - Y. Alibert - N. Cabral • I. Leya - K. Mezger

  2. Introduction WHAT COMPOSITION CAN TELL US • Composition of planets is linked to its structure. Knowing it can provide informations on : • Equation of state • mean molecular weight • density • Radius of the planet (see, eg. Swift et al. 2012) • Atmosphere • Better understanding of planet formation and evolution • Chemistry will also induce changes in the disc properties (temperature, pressure, and opacity especially) 2

  3. Introduction DEFINITIONS • Refractory : Tc>TcH2O • Volatile : Tc<TcH2O

  4. Planete THE BERN PLANET FORMATION MODEL • Initial planet formation model by Alibert et al. 2005 => Giant planets • Improvements: • Population Synthesis (Mordasini et al.,2009 a,b) • Accretion rate of planetesimals (Fortier et al. 2013) • Formation of planetary systems (Alibert et al. 2013) • Surface density:

  5. Planete MIGRATION OF PLANETS 5

  6. Assumptions • Composition of the solar nebula. • Atoms in gaseous phase. • Volatiles : CO2, CO, NH3, N2, H2O, CH4, CH3OH, H2S. • Abundances of Lodders 2003. • Non-irradiated disk. • no chemical reactions.  

  7. Refractory elements SOME THERMODYNAMICS • Formation of refractory elements based on condensation sequence at equilibrium. • Minimization of Gibbs energy : • Computation of the condensation sequence for T(r), P(r) provided by the planet formation model.

  8. Volatile elements COOLING CURVES

  9. Results REFRACTORY ELEMENTS IN THE DISK

  10. Results VOLATILE SPECIES - ICE LINE

  11. Results REFRACTORY MASS FRACTION IN PLANETS

  12. Results MEAN COMPOSITION OF PLANETS Rocky planets Giant/icy planets All numbers in wt%

  13. Results CHANGES WITH INITIAL SURFACE DENSITY

  14. Conclusions • Every planet of the Solar System can be chemically reproduced by our model. (Even Mercury !) • Giant planets are depleted in volatile elements, compared to icy or Neptune/Saturne-like planets. • A relation between the disc parameters and the position of the iceline was derived. • The use of self-consistent models, with a population of discs, is needed to form a large diversity ofplanets.

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