: The role of the initial surface density profiles of the disc on giant planet formation: comparing with observations

MIGUEL, Y.; GUILERA, O. M.; BRUNINI, A.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Lugar: Londres; Año: 2011 vol. 412 p. 2113 - 2124

0035-8711

In order to explain the main characteristics of the observed population of extrasolar planetsand the giant planets in the Solar system, we need to get a clear understanding of which are theinitial conditions that allowed their formation. To this end we develop a semi-analytical modelfor computing planetary systems formation based on the core instability model for the gasaccretion of the embryos and the oligarchic growth regime for the accretion of the solid cores.With this model we explore not only different initial discs profiles motivated by similaritysolutions for viscous accretion discs, but also consider different initial conditions to generatea variety of planetary systems assuming a large range of discs masses and sizes according tothe last results in protoplanetary discs observations. We form a large population of planetarysystems in order to explore the effects in the formation of assuming different discs and also theeffects of type I and II regimes of planetary migration, which were found to play fundamentalrole in reproducing the distribution of observed exoplanets. Our results show that the observedpopulation of exoplanets and the giant planets in the Solar system are well represented whenconsidering a surface density profile with a power law in the inner part characterized by anexponent of −1, which represents a softer profile when compared with the case most similarto the minimum mass solar nebula model case.