Enhanced molecular abundances in low-mass star-forming cores

The outflow from a young stellar object interacts with the dense core in which it is embedded to create anomalously high abundances of HCO+ that under high resolution show a 'butterfly' morphology. It has been suggested that the high HCO+ abundance and its morphology arose in a photochemistry induced in the highly turbulent interface induced between the outflow and the core. In this paper we use a very large chemical network to explore the molecular nature of this interface, and demonstrate that, beside HCO+, many other molecular tracers should be anomalously enhanced in this interface and should under high resolution show the same morphology as HCO+. We predict that particularly abundant species should include H2S, CS, H2CS, SO, SO2, CH3OH, and recommend that a study for these species and their morphologies be made in star-forming cores. Such observations should help to define the fluid interaction in the interface. The range of molecules predicted here should more generally represent a chemical signature of energetic turbulent mixing of hot and cold interstellar fluids, and our models developed may be able to interpret observations to determine the nature of the fluids and their interaction.