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High-mass stars are expected to form from dense prestellar cores. Theirprecise formation conditions are widely discussed, including their virialcondition, which results in slow collapse for super-virial cores with strongsupport by turbulence or magnetic fields, or fast collapse for sub-virialsources. To disentangle their formation processes, measurements of thedeuterium fractions are frequently employed to approximately estimate the agesof these cores and to obtain constraints on their dynamical evolution. We herepresent 3D magneto-hydrodynamical simulations including for the first time anaccurate non-equilibrium chemical network with 21 gas-phase species plus dustgrains and 213 reactions. With this network we model the deuteration process infully depleted prestellar cores in great detail and determine its response tovariations in the initial conditions. We explore the dependence on the initialgas column density, the turbulent Mach number, the mass-to-magnetic flux ratioand the distribution of the magnetic field, as well as the initialortho-to-para ratio of H2. We find excellent agreement with recent observationsof deuterium fractions in quiescent sources. Our results show that deuterationis rather efficient, even when assuming a conservative ortho-to-para ratio of 3and highly sub-virial initial conditions, leading to large deuterium fractionsalready within roughly a free-fall time. We discuss the implications of ourresults and give an outlook to relevant future investigations.

Deuterium fractionation and H2D+ evolution in turbulent and magnetized cloud cores