  The abundances of elements in the Earth and the terrestrial planets provide
the initial conditions for life and clues as to the history and formation of
the Solar System. We follow the pioneering work of Bond et al. (2010) and
combine circumstellar disk models, chemical equilibrium calculations and
dynamical simulations of planet formation to study the bulk composition of
rocky planets. We use condensation sequence calculations to estimate the
initial abundance of solids in the circumstellar disk with properties
determined from time dependent theoretical models. We combine this with
dynamical simulations of planetesimal growth that trace the solids during the
planet formation process. We calculate the elemental abundances in the
resulting planets and explore how these vary with the choice of disk model and
the initial conditions within the Solar Nebula.
  Although certain characteristics of the terrestrial planets in the Solar
System could be reproduced, none of our models could reproduce the abundance
properties of all the planets. We found that the choice of the initial
planetesimal disk mass and of the disk model has a significant effect on
composition gradients. Disk models that give higher pressure and temperature
result in larger variations in the bulk chemical compositions of the resulting
planets due to inhomogeneities in the element abundance profiles and due to the
different source regions of the planets in the dynamical simulations. We
observed a trend that massive planets and planets with relatively small
semi-major axes are more sensitive to these variations than smaller planets at
larger radial distance. Only these large variations in the simulated chemical
abundances can potentially explain the diverse bulk composition of the Solar
System planets, whereas Mercury's bulk composition can not be reproduced in our
approach.
