Radial Gradients in Dust-to-Gas Ratio Lead to Preferred Region for Giant Planet Formation

Abstract

The Rosseland mean opacity of dust in protoplanetary disks is often calculated assuming the interstellar medium (ISM) size distribution and a constant dust-to-gas ratio. However, the dust size distribution and the dust-to-gas ratio in protoplanetary disks are distinct from those of the ISM. Here, we use simple dust evolution models that incorporate grain growth and transport to calculate the time evolution of mean opacity of dust grains as a function of distance from the star. Dust dynamics and size distribution are sensitive to the assumed value of the turbulence strength $\alpha_{\rm t}$ and the velocity at which grains fragment $v_{\rm frag}$. For moderate-to-low turbulence strengths of $\alpha_{\rm t} \lesssim 10^{-3}$ and substantial differences in $v_{\rm frag}$ for icy and ice-free grains, we find a spatially non-uniform dust-to-gas ratio and grain size distribution that deviate significantly from the ISM values, in agreement with previous studies. The effect of a non-uniform dust-to-gas ratio on the Rosseland mean opacity dominates over that of the size distribution. This spatially varying -- that is non-monotonic -- dust-to-gas ratio creates a region in the protoplanetary disk that is optimal for producing hydrogen-rich planets, potentially explaining the apparent peak in gas giant planet occurrence rate at intermediate distances. The enhanced dust-to-gas ratio within the ice line also suppresses gas accretion rates onto sub-Neptune cores, thus stifling their tendency to undergo runaway gas accretion within disk lifetimes. Finally, our work corroborates the idea that low mass cores with large primordial gaseous envelopes (`super-puffs') originate beyond the ice line.