The thermal structure and the location of the snow line in the protosolar nebula: Axisymmetric models with full 3-D radiative transfer

► We compute the thermal- and condensation structure of the early Solar nebula. ► The snow line location depends on the accretion rate and the dust properties. ► The increase in solid matter by ice is substantially lower than currently assumed. ► There is a hot inner region with a thermostat at the dust evaporation temperature. ► In this region, sintering of materials will strongly influence grain growth.