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• W2000491621 endingPage "141" @default.
• W2000491621 startingPage "141" @default.
• W2000491621 abstract "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 (dot{M}) in the disk decreases with time. Calculations are carried out from an early phase with high disk accretion rates (dot{M} sim 10^{-7} M_sun/yr) to a later phase with low disk accretion rates (dot{M} sim 10^{-12} M_sun/yr) using the same numerical method. It is found that the snow line moves inward for dot{M} > 10^{-10} M_sun/yr, while it gradually moves outward in the later evolution phase with dot{M} < 10^{-10} M_sun/yr. 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 micro-meter in size and 1.6 for > 100 micro-meter. It is inevitable that the snow line comes inside the Earth's orbit in the course of the disk evolution, if the alpha viscosity parameter is in a 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." @default.
• W2000491621 created "2016-06-24" @default.
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• W2000491621 date "2011-08-19" @default.
• W2000491621 modified "2023-09-25" @default.
• W2000491621 title "EVOLUTION OF SNOW LINE IN OPTICALLY THICK PROTOPLANETARY DISKS: EFFECTS OF WATER ICE OPACITY AND DUST GRAIN SIZE" @default.
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• W2000491621 doi "https://doi.org/10.1088/0004-637x/738/2/141" @default.
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