![]() We present the results of our simulations and discuss their The final planets, their masses, time of formation, and distances to theĬentral star. Seems to exist between the disk surface density profile and the mean number of ![]() Results indicate that despite some small correlations, in general, no trend Mars so that it can maintain its mass and orbital stability. However, nu_6Īnd nu_16 resonances play important roles in clearing their affected areasĮnsuring that no additional mass will be scattered into the accretion zone of Significant effect on the final orbits of terrestrial planets. In the context of theĭepleted disk model, results show that the nu_5 resonance does not have a Profile and the final properties of terrestrial planets. Our goal is to determine trends that may exist between the disk surface density The formation of Mars and orbital stability of terrestrial planets. In Part 1, we are interested in examining the effects of secular resonances on We have divided this study into two parts. Resonances in orbits and properties of the final planets, we studied theĮffects of these resonances as well. Because of the important roles of secular Planets and their physical properties are affected by the total mass of theĭisk and its radial profile. The purpose of our study is to determine how the final assembly of We carried out simulations forĭisk densities proportional to r^-0.5, r^-1, and r^-1.5, and also for partiallyĭepleted disks as in the recent model of Mars formation by Izidoro et al Terrestrial planet formation in disks with different surface density profilesĪnd for different orbits of Jupiter and Saturn. We present the results of an extensive study of the final stage of
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