Contribution Contributed Talk
Connecting the composition of exoplanets and their atmospheres with protostellar disk chemistry
The chemical composition of exoplanets and their atmospheres is arguably the most important ingredient in determining their mass-radius relation and their atmospherics properties. The initial chemical composition of exoplanets is a consequence of their accretion history as they migrate through their natal protoplanetary disks accreting both solids and gases as they build and move through their host disks. We have recently constructed a theory of planet formation that emphasizes the role of planet traps in regulating the slow inward drift of accreting planets. These dynamical traps are disk inhomogeneities in density and temperature such as ice lines, dead zone boundaries, and heat transition radii where disk heating switches from disk viscosity to radiative heating from the central star. In this contribution we present results on both the solid and gaseous composition of planets such as warm Jupiters and SuperEarths as they move along "evolutionary tracks" in the mass- semimajor axis diagram that has come to characterize exoplanetary populations. We show that the solid composition of planets depends to a large degree on whether or not they formed on particular traps (eg. ice lines). We compute the non-equilibrium chemistry of protoplanetary disk models and show how the initial protoplanetary atmospheres depend on their accretion history in protoplanetary disks. We link our models with observations of planetary atmospheres associated with hot Jupiter and SuperEarths.