Evolution models of Pegasids

("51 Peg b-like" planets)

Animation of the transiting system HD209458a+b

Masses of heavy elements vs. star metallicity for the known transiting planets

Figure: Mass of heavy elements in transiting Pegasids known by 2006
as a function of the metal content of the parent star relative to the
Sun. The mass of heavy elements required to fit the measured radii
is calculated on the basis of evolution models including an additional
heat source slowing the cooling of the planet. This heat source is assumed
equal to 0.5% of the incoming stellar heat flux (Showman &
Guillot 2002). Horizontal error bars correspond to the 1¾ errors on
the [Fe/H] determination. Vertical error bars are a consequence of the
uncertainties on the measured planetary radii and ages. The metallicity
of recently discovered planets WASP-1 and WASP-2 (right
panel) is not precisely known. The dotted line corresponds to a best
fit model. [See Guillot et al. A&A (2006), Fressin et al. A&A, in press].


Parameters: Equilibrium temperatures between 100 and 2000 K, Planetary masses between 100 and 3178 Earth masses, Core masses between 0 and 100 Earth masses.
All models assume that 0.5% of the incoming stellar luminosity is absorbed deep in the planet's interior.

The yield of planetary transit surveys

Figure: Mass-radius relation for a very large number of Monte-Carlo trials using a model to reproduce the population
of transiting planets according to present observational data from radial velocimetry surveys, photometric surveys,
and using up-to-date evolution models of extrasolar planets.
The curves show the ensemble of planets with masses of heavy elements between 0 and 25,
25 and 50, 50 and 75, 75 and 100MEarth, respectively. The coloured discs are known transiting planets.
[From Fressin et al. A&A, in press]

DOWNLOAD EVOLUTION MODELS OF HD209458b (From Guillot & Showman, A&A 2002)

Articles & Preprints

  • Fressin F., Guillot T., Morello V. & Pont F. 2007, ``Interpreting and predicting the yield of transit surveys: Giant planets in the OGLE fields", A&A, in press [pdf file]
  • Guillot T., Santos N., Pont F., Iro N., Melo C. & Ribas I. 2006, ``A correlation between the heavy element content of transiting extrasolar planets and the metallicity of their parent stars", A&A, 453, L21-L24 [pdf file]
  •  Guillot T., & Showman A.P. 2002, ``Evolution of "51 Peg b-like" Planets", A&A, 385, 156-165 [ps file]
  • Showman A.P., & Guillot T. 2002, ``Atmospheric Circulation and Tides of "51 Peg b-like" Planets", A&A, 385, 166-180 [ps file]
  • Guillot T. 2001, "Atmospheric Circulation of Hot Jupiters", IAU 202, Planetary Systems in the Universe: Observation, Formation and Evolution, ASP Conf. series, A. Penny et al. eds. (Manchester, UK, August 2000), in press[ps file]

  • Possible atmospheric circulation in a Pegasi planet

    Derniere Modification: 3 avril 2007
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