The chemistry of disks around T Tauri and HerbigAe/Be stars

Context. Infrared and (sub-) millimeter observations of disks around T Tauri and HerbigAe/Be stars point to a chemical differentiation, with a lower detection rate of molecules in disks around hotter stars. Aims. We aim to investigate the underlying causes of the chemical differentiation indicated by observations and perform a comparative study of the chemistry of T Tauri and HerbigAe/Be disks. This is one of the first studies to compare the chemistry in the outer regions of these two types of disk. Methods. We developed a model to compute the chemical composition of a generic protoplanetary disk, with particular attention to the photochemistry, and applied it to a T Tauri and a HerbigAe/Be disk. We compiled cross sections and computed photodissociation and photoionization rates at each location in the disk by solving the far-ultraviolet (FUV) radiative transfer in a 1+1D approach using the Meudon PDR code and adopting observed stellar spectra. Results. The warmer disk temperatures and higher ultraviolet flux of Herbig stars compared to T Tauri stars induce some differences in the disk chemistry. In the hot inner regions, H2O, and simple organic molecules like C2H2, HCN, and CH4 are predicted to be very abundant in T Tauri disks and even more in HerbigAe/Be disks, in contrast with infrared observations that find a much lower detection rate of water and simple organics toward disks around hotter stars. In the outer regions, the model indicates that the molecules typically observed in disks, like HCN, CN, C2H, H2CO, CS, SO, and HCO+, do not have drastic abundance differences between T Tauri and HerbigAe disks. Some species produced under the action of photochemistry, like C2H and CN, are predicted to have slightly lower abundances around HerbigAe stars due to a narrowing of the photochemically active layer. Observations indeed suggest that these radicals are somewhat less abundant in HerbigAe disks, although in any case, the inferred abundance differences are small, of a factor of a few at most. A clear chemical differentiation between both types of disks concerns ices. Owing to the warmer temperatures of HerbigAe disks, one expects snow lines lying farther away from the star and a lower mass of ices compared to T Tauri disks. Conclusions. The global chemical behavior of T Tauri and HerbigAe/Be disks is quite similar. The main differences are driven by the warmer temperatures of the latter, which result in a larger reservoir or water and simple organics in the inner regions and a lower mass of ices in the outer disk.