Evolution of Extrasolar Giant Planets

This page is still under construction...

The next links will lead you to directories containing the following ASCII files:

README
evol.des: evolution with time of the global variables
evolution.des: interior models at various epochs
exo.asc: final interior model (with comments in french and list of parameters)

(example: 1mj = 1 mass of Jupiter = 1.8986E+30 g; 1200k = Teq [equilibrium effective temperature]; 10me=10 Earth mass rock core)

egp_5mj_1200k
egp_2mj_1200k
egp_1mj_1200k

Caveat: close-in low-mass giant planets of solar composition are never fully convective and contract on timescales > 10Myr
        => If present, they had to either first accrete a MASSIVE central core
                or most probably they had to form further out in the nebula, and then migrate inward
              In the latter case, the evolution track would be a combination of evolutions at various Teq...

egp_0,5mj_1200k
egp_0,5mj_1200k_10me
egp_0,5mj_600k_10me

Note:

The radii predicted by these calculations are to be generally considered as upper limits because
    1) migration is not included (yields faster contraction)
    2) assumed solar composition (Jupiter and Saturn are enriched in heavy elements)
    3) atmospheric models assume that most of the incoming stellar flux is absorbed at the 10 bar level (whereas detailled calculations predict that it should be absorbed higher in the atmosphere)...

(But point 3 has to be reexamined...)

Any comments? E-mail me at guillot@obs-nice.fr

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