Evolution of a snow line in an optically thick protoplanetary disk is investigated with numerical simulations. The ice-condensing region in the disk is obtained by calculating the temperature and the density with the 1+1D approach. The snow line migrates as the mass accretion rate () in the disk decreases with time. Calculations are carried out from an early phase with high disk accretion rates (?yr–1) to a later phase with low disk accretion rates (?yr–1) using the same numerical method. It is found that the snow line moves inward for ?yr–1, while it gradually moves outward in the later evolution phase with ?yr–1. In addition to the silicate opacity, the ice opacity is taken into consideration. In the inward migration phase, the additional ice opacity increases the distance of the snow line from the central star by a factor of 1.3 for dust grains 10 μm in size and of 1.6 for 100 μm. It is inevitable that the snow line comes inside Earth's orbit in the course of the disk evolution if the viscosity parameter α is in the range 0.001-0.1, the dust-to-gas mass ratio is higher than a tenth of the solar abundance value, and the dust grains are smaller than 1 mm. The formation of water-devoid planetesimals in the terrestrial planet region seems to be difficult throughout the disk evolution, which imposes a new challenge to planet formation theory.
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