Protostars and Planets VI, Heidelberg, July 15-20, 2013

Poster 2B037

Structure and migration in stellar irradiated Discs

Bitsch, Bertram (OCA)
Alessandro, Morbidelli (OCA)

Structure of evolving stellar irradiated discs The evolution of the protoplanetary disc is of crucial importance to explain the growth and formation of planets inside the disc. In a recent work, we have shown that the disc structure is crucially dependent on the stellar heating and on the opacity (Bitsch et al., 2013). In particular, some self shadowed regions in the disc form, which are dependent on the opacity transitions in the disc. Inside these shadowed regions, small mass planets can migrate outwards and gather at the zero- migration radius, where they can form bigger objects through collisions. The structure of the disc is dependent on the mass-flux through the disc, which determines the evolution of the density profile. The metallicity and grain sizes determine the value and the shape of the opacity profile, which influence the temperature structure of the disc. We will show in our 2D models the interplay between these different parameters and what their influence on the disc structure are. We will also address how these different disc structures influence the zero-migration radius inside a disc, which will give important indications where the cores of giant planets in a disc potentially form.

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