# Multiple paths of deuterium fractionation in protoplanetary disks

## TL;DR

This study explores multiple pathways of deuterium fractionation in protoplanetary disks, emphasizing the roles of grain size, turbulence, and cosmic rays in molecular chemistry and isotope ratios.

## Contribution

It introduces a comprehensive model of deuterium chemistry coupled with nuclear spin-state chemistry, highlighting the effects of grain growth and turbulence on molecular abundances.

## Key findings

- Deuterium fractionation occurs via multiple pathways, including exchange reactions with D atoms.
- Grain size influences molecule freeze-out and gas-phase abundances, with larger grains reducing freeze-out.
- Turbulence affects the distribution and abundance of deuterated molecules and other species across the disk.

## Abstract

We investigate deuterium chemistry coupled with the nuclear spin-state chemistry of H$_2$ and H$_3^+$ in protoplanetary disks. Multiple paths of deuterium fractionation are found; exchange reactions with D atoms, such as HCO$^+$ + D, are effective in addition to those with HD. In a disk model with grain sizes appropriate for dark clouds, the freeze-out of molecules is severe in the outer midplane, while the disk surface is shielded from UV radiation. Gaseous molecules, including DCO$^+$, thus become abundant at the disk surface, which tends to make their column density distribution relatively flat. If the dust grains have grown to millimeter size, the freeze-out rate of neutral species is reduced, and the abundances of gaseous molecules, including DCO$^+$ and N$_2$D$^+$, are enhanced in the cold midplane. Turbulent diffusion transports D atoms and radicals at the disk surface to the midplane, and stable ice species in the midplane to the disk surface. The effects of turbulence on chemistry are thus multifold; while DCO$^+$ and N$_2$D$^+$ abundances increase or decrease depending on the regions, HCN and DCN in the gas and ice are much reduced at the innermost radii, compared with the model without turbulence. When cosmic rays penetrate the disk, the ortho-to-para ratio (OPR) of H$_2$ is found to be thermal in the disk, except in the cold ($\lesssim 10$ K) midplane. We also analyze the OPR of H$_3^+$ and H$_2$D$^+$, as well as the main reactions of H$_2$D$^+$, DCO$^+$, and N$_2$D$^+$ to analytically derive their abundances in the cold midplane.