  We present the results of an extensive study of the final stage of
terrestrial planet formation in disks with different surface density profiles
and for different orbits of Jupiter and Saturn. We carried out simulations for
disk densities proportional to r^-0.5, r^-1, and r^-1.5, and also for partially
depleted disks as in the recent model of Mars formation by Izidoro et al
(2014). The purpose of our study is to determine how the final assembly of
planets and their physical properties are affected by the total mass of the
disk and its radial profile. Because of the important roles of secular
resonances in orbits and properties of the final planets, we studied the
effects of these resonances as well. We have divided this study into two parts.
In Part 1, we are interested in examining the effects of secular resonances on
the formation of Mars and orbital stability of terrestrial planets. In Part 2,
our goal is to determine trends that may exist between the disk surface density
profile and the final properties of terrestrial planets. In the context of the
depleted disk model, results show that the nu_5 resonance does not have a
significant effect on the final orbits of terrestrial planets. However, nu_6
and nu_16 resonances play important roles in clearing their affected areas
ensuring that no additional mass will be scattered into the accretion zone of
Mars so that it can maintain its mass and orbital stability. In Part 2, our
results indicate that despite some small correlations, in general, no trend
seems to exist between the disk surface density profile and the mean number of
the final planets, their masses, time of formation, and distances to the
central star. We present the results of our simulations and discuss their
implications for the formation of Mars and other terrestrial planets, as well
as the physical properties of these objects such as their masses and water
contents.
