Water and volatile abundances on Earth-like planets in low-mass disks

MARÍA PAULA RONCO; AMAURY THIABAUD; ULYSSE MARBOEUF; YANN ALIBERT; GONZALO CARLOS DE ELÍA; OCTAVIO MIGUEL GUILERA

Foz do Iguacú

Simposio; 2nd COSPAR Symposium - Water and life in the Universe; 2015

Grupo de Dinâmica Orbital e Planetologia - Brasil

The study of the chemical composition, especially the amounts of water of extrasolar planets, is a topic of current interest since it is partly responsible for their potential habitability. It is particularly interesting to study the chemical composition of Earth-like planets formed within the habitable zone of low-mass protoplanetary disks, which are incapable of forming giant planets. According to observational and theoretical studies, planetary systems composed by only rocky planets seem to be the most common in the universe and owing to that they result to be targets of significative interest.In this work, we present results of numerical simulations aimed to analyzing planetary formation processes and distribution of volatile elements around a solar-type star and assuming low-mass protoplanetary disks. In particular, we study protoplanetary disks with and without irradiation. For each of such scenarios, we calculate the condensation sequences of the different volatile elements (H2O, CO, CO2, CH4, H2S, N2, NH3 and CH3OH) and then, we incorporate them in a semi-analytical model, which calculates the evolution of planetary embryos and planetesimals during the gaseous phase. Once the gas is dissipated, the distributions of embryos and planetesimals obtained with the semi-analytical model are used as initial conditions to develope N-body simulations, which describe the main dynamical processes associated to the planetary formation. The main goal of the present work is to analyze the final chemical composition of the planets that remain in the habitable zone for both the irradiated and the non-irradiated disk. In particular, we are interested in studying the differences between both scenarios of work. Moreover, we focus on the discrepancies obtained between the chemical compositions of the planets resulting of our simulations and those associated to the planets of our Solar System. This investigation will allow us to strengthen our understanding about the formation and evolution of a planetary system around solar-type stars.