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

Abstract

In order to explain the main characteristics of the observed population of extrasolar planets and the giant planets in the Solar System, we need to get a clear understanding of which are the initial conditions that allowed their formation. To this end we develop a semi-analytical model for computing planetary systems formation based on the core instability model for the gas accretion 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 similarity solutions for viscous accretion discs, but we also consider different initial conditions to generate a variety of planetary systems assuming a large range of discs masses and sizes according to the last results in protoplanetary discs observations. We form a large population of planetary systems in order to explore the effects in the formation of assuming different discs and also the effects of type I and II regimes of planetary migration, which were found to play fundamental role in reproducing the distribution of observed exoplanets. Our results show that the observed population of exoplanets and the giant planets in the Solar System are well represented when considering a surface density profile with a power law in the inner part characterized by an exponent of -1, which represents a softer profile when compared with the case most similar to the MMSN model case.

14 pages, 12 figures, MNRAS, 412, 2113

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• Grain opacity and the bulk composition of extrasolar planets. I. Results from scaling the ISM opacity
• Observations of Solids in Protoplanetary Disks
• Global models of planetary system formation in radiatively-inefficient protoplanetary discs
• Giant planet formation at the pressure maxima of protoplanetary disks II. A hybrid accretion scenario
• Diverse outcomes of planet formation and composition around low-mass stars and brown dwarfs
• Simultaneous formation of Solar System giant planets
• The Diversity of Planetary Systems Architectures: Contrasting Theory with Observations
• Planet Formation In Highly Inclined Binary Systems I. Planetesimals Jump Inwards And Pile Up
• Setting the Stage: Planet formation and Volatile Delivery
• Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario
• Planetary formation and water delivery in the habitable zone around solar-type stars in different dynamical environments
• Quantifying the Impact of the Dust Torque on the Migration of Low-mass Planets
• Migrating Jupiter up to the habitable zone: Earth-like planet formation and water delivery
• DIPSY: A new Disc Instability Population SYnthesis, II. The Populations of Companions Formed Through Disc Instability
• Zero Age Planetary Orbit of Gas Giant Planets Revisited: Reinforcement of the Link with Stellar Metallicity
• Planetesimal fragmentation and giant planet formation: the role of planet migration