  In our solar system, terrestrial planets and meteoritical matter exhibit
various bulk compositions. To understand this variety of compositions,
formation mechanisms of meteorites are usually investigated via a thermodynamic
approach that neglect the processes of transport throughout the protosolar
nebula. Here, we investigate the role played by rocklines
(condensation/sublimation lines of refractory materials) in the innermost
regions of the protosolar nebula to compute the composition of particles
migrating inward the disk as a function of time. To do so, we utilize a
one-dimensional accretion disk model with a prescription for dust and vapor
transport, sublimation and recondensation of refractory materials (ferrosilite,
enstatite, fayalite, forsterite, iron sulfide, metal iron and nickel). We find
that the diversity of the bulk composition of cosmic spherules, chondrules and
chondrites can be explained by their formation close to rocklines, suggesting
that solid matter is concentrated in the vicinity of these
sublimation/condensation fronts. Although our model relies a lot on the number
of considered species and the availability of thermodynamic data governing
state changes, it suggests that rocklines played a major role in the formation
of small and large bodies in the innermost regions of the protosolar nebula.
Our model gives insights on the mechanisms that might have contributed to the
formation of Mercury's large core.
