Planetary arcs, the densest parts of a planetary ring, can be found in the planetary systems of Saturn and Neptune. In Neptune, these arcs (Fraternité, Egalité, Courage and Egalité) are located in the tenuous Adams ring. To constrain the spreading of the arcs, due to keplerian shear and dissipative forces, a recent confinement mechanism proposed that the azimuthal confinement is due to coorbital satellites while its radial confinement is caused by a resonance with the close satellite Galatea (Renner et al., 2014). Giuliatti Winter et al (submitted to Monthly Notices of the Royal Astronomical Society) showed how and why these arcs are fading away (de Pater et al., 2005). One model to explain the origin of the arcs and the coorbital satellites claimed that these bodies have been formed due to material located in the L4 and L5 Lagrangian equilibrium points (de Pater et al., 2018). In the light of this model we intend to study the formation of the Neptune's arcs taking into account a system composed of coorbital satellites and protosatellites confined by these coorbitals. The Smooth Particle Hidrodynamic Code (SPH code) will be used to compute the collision between protosatellites and external debris by assuming different parameters. The four galilean satellites of Jupiter could be formed in the circumplanetary disc, during the late stages of the planet formation. One of the recent models of the formation of these satellitesis described in the paper by Moraes et al. (2017) which propose that the galilean satellites are formed in a low mass disc composed of gas, embryos and satelitesimals with ejected material from the protoplanetary disc. By the other hand, Cilibrasi et al. (2018) proposed a circumplanetary disc with such temperature and gas distribution profiles that the material, located in the inner part of the disc, migrates outward while the material located in the outer part migrates inward. As a consequence, large bodies can be formed in the limit of these two regimes. Both models propose the formation of these large satellites by accretion of satelitesimals. Although these models can not explain either the mass distribution of these satellites or their mean motion resonances. Levison et al. (2015) showed that embryos with similar sizes of Pluto can reach the same mass of Earth in a time span of 1000 years through the accretion of pebbles. Therefore, taking into account the profiles present in Cilibrasi et al. (2018), the formation of the galilean satellites will be analysed by using the accretion of pebbles. The parameters, such as the viscosity of the gas, dispersion time and mass distribution, will be the same as the values assumed in Raymond e Izidoro (2017).
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