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

TL;DR

This study uses advanced 3D radiative transfer models to accurately determine the snow line's position in the protosolar nebula, revealing its sensitivity to dust properties and accretion rates, and refining previous estimates.

Contribution

It introduces a fully self-consistent 3D axisymmetric model with dust and ice sublimation, improving the understanding of snow line location in the early solar system.

Findings

The snow line's position is highly sensitive to dust opacities and accretion rates.

Previous approximate models are effective if viscous heating dominates the energy budget.

The solid surface density jump at the snow line is smaller than previously thought.

Abstract

The precise location of the water ice condensation front ('snow line') in the protosolar nebula has been a debate for a long time. Its importance stems from the expected substantial jump in the abundance of solids beyond the snow line, which is conducive to planet formation, and from the higher stickiness in collisions of ice-coated dust grains, which may help the process of coagulation of dust and the formation of planetesimals. In an optically thin nebula, the location of the snow line is easily calculated to be around 3 AU. However, in its first 5 to 10 million years, the solar nebula was optically thick, implying a smaller snow line radius due to shielding from direct sunlight, but also a larger radius because of viscous heating. Several models have attempted to treat these opposing effects. However, until recently treatments beyond an approximate 1+1D radiative transfer were unfeasible. We revisit the problem with a fully self-consistent 3D treatment in an axisymmetric disk model, including a density-dependent treatment of the dust and ice sublimation. We find that the location of the snow line is very sensitive to the opacities of the dust grains and the mass accretion rate of the disk. We show that previous approximate treatments are quite efficient at determining the location of the snow line if the energy budget is locally dominated by viscous accretion. We derive an analytic estimate of the location of the snow line that compares very well with results from this and previous studies. Using solar abundances of the elements we compute the abundance of dust and ice and find that the expected jump in solid surface density at the snow line is smaller than previously assumed. We further show that in the inner few AU the refractory species are partly evaporated, leading to a significantly smaller solid state surface density in the regions where the rocky planets were formed.