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| Author(s): |
Luiz Alberto de Paula
Total Authors: 1
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| Document type: | Master's Dissertation |
| Press: | São Paulo. |
| Institution: | Universidade de São Paulo (USP). Instituto Astronômico e Geofísico (IAG/SBD) |
| Defense date: | 2014-05-09 |
| Examining board members: |
Tatiana Alexandrovna Michtchenko;
Cristian Andrés Giuppone;
Sylvio Ferraz de Mello
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| Advisor: | Tatiana Alexandrovna Michtchenko |
| Abstract | |
The aim of this paper is to model the planetary formation and migration of a solid core. Therefore, it was used a model of planetesimal accretion, based on the paper of Inaba et al. (2000), in which the average accretion tax depends on the inclination and eccentricity of that planetesimals. These parameters were obtained through the balance situation between the interaction with the protoplanet and gas draft (Fortier et al., 2013). In order to complete this scenario, the migration type I, which occurs due to an interaction of the planet with the gas disc, was included. The analytical model that describes this migration has its basis on (Tanaka et al., 2002). The density of solids and gas profile was based on three different models for the disc. The first one is a classical of Nebulosa Solar, in which the density profile varies r^3/2 , the second is a hybrid model that uses observational measures of the gas superficial density (Andrews et al., 2010) and an analytical formula for the gas volumetric density; at last, the third model is an accretion disc which uses the parameterization of (Shakura e Sunyaev, 1973) with constant. Using these three different disc profiles, it was possible to explore the variation of the model free parameters and the possibility of the solid cores formation with 10M Earth within time smaller than 10 × 10^6 years, which is the estimated limit lifetime of the disc. In general, migration type I is very fast, so that the protoplanet falls on the star before acquiring enough mass to begin the gas accretion. However, the analysis has revealed, for the hybrid disc, the possibility to obtain masses up to 10MEarth within time 2 × 10^6 , for distance up to 3.5 AU. In conclusion, more complete models of accretion as well as the more coherent density gas and solid profiles of the protoplanet obtained may explain the formation of solid coreswithin a useful time for the giant planets formation, not using numerical factors that reduce the migration type I tax. (AU) | |
| FAPESP's process: | 12/01369-5 - DISK-PLANET INTERACTIONS |
| Grantee: | Luiz Alberto de Paula |
| Support Opportunities: | Scholarships in Brazil - Master |