First simulations of planetary formation with planet-disc interaction

CIONCO, R. G.; BRUNINI, A

La Plata

Congreso; 47 Reunión Anual de la Asociación Argentina de Astronomía; 2003

In the standard model, the four giant solar planets are formed by concurrent accretion of gas and solids. The growth of massive proto-planets implies the apparition of density waves in the primordial nebula. As a result, planetary embryos of > 0.1 M⊕ migrate to the central star. In this work, numerical simulation of formation process in an standard nebular environment (gas accretion is allowed for embryos > 10 M⊕) are made, taking into account, by first time, type I and II migratory planets. Icy giant planets are the most probable byproduct (they will be observable as soon as the refinement of the exoplanets detection techniques). In one of the models (four embryos of 1 M⊕ with enlarged radius, and ~ 103 planetesimals) two protoplanets growth toward 10 M⊕ in short time-scales (a few 104 yr.)