ormation of Solar System Analogues through N-body simulations and water delivery on potentially habitable planets

GONZALO CARLOS DE ELÍA; MARÍA PAULA RONCO

La Serena

Congreso; Second Binational Meeting SOCHIAS - AAA; 2018

Sociedad Chilena de Astronomía

This work is the second part of a project that attempts to analyse theformation of Solar system analogues (SSAs) from the gaseous to thepost-gas phase, in a self-consistently way. In the first paper (PI) wepresented our model of planet formation during the gaseous phase whichprovided us with embryo distributions, planetesimal surface density,eccentricity, and inclination profiles of SSAs, considering differentplanetesimal sizes and type I migration rates at the time the gasdissipates. In this second work we focus on the late accretion stage ofSSAs using the results obtained in PI as initial conditions to carry outN-body simulations. One of our interests is to analyse the formation ofrocky planets and their final water contents within the habitable zone.Our results show that the formation of potentially habitable planets(PHPs) seems to be a common process in this kind of scenarios. However,the efficiency in forming PHPs is directly related to the size of theplanetesimals. The smaller the planetesimals, the greater the efficiencyin forming PHPs. We also analyse the sensitivity of our results toscenarios with type I migration rates and gap-opening giants, findingthat both phenomena act in a similar way. These effects seem to favourthe formation of PHPs for small planetesimal scenarios and to bedetrimental for scenarios formed from big planetesimals. Finally,another interesting result is that the formation of water-rich PHPsseems to be more common than the formation of dry PHPs.