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Combining the co-evolving chemistry, hydrodynamics and radiative transfer isan important step for star formation studies. It allows both a better link toobservations and a self-consistent monitoring of the magnetic dissipation inthe collapsing core. Our aim is to follow a chemo-dynamical evolution ofcollapsing dense cores with a reduced gas-grain chemical network. We presentthe results of radiative hydrodynamic (RHD) simulations of 1 M$_\odot$ isolateddense core collapse. The physical setup includes RHD and dynamical evolution ofa chemical network. To perform those simulations, we merged themulti-dimensional adaptive-mesh-refinement code RAMSES and the thermo-chemistryParis-Durham shock code. We simulate the formation of the first hydro-staticcore (FHSC) and the co-evolution of 56 species describing mainly H-C-Ochemistry. Accurate benchmarking is performed, testing the reduced chemicalnetwork against a well-establiched complex network. We show that by using acompact set of reactions, one can match closely the CO abundances with resultsof a much more complex network. Our main results are: (a) We find thatgas-grain chemistry post-processing can lead to one order of magnitude lower COgas-phase abundances compared to the dynamical chemistry, with strongest effectduring the isothermal phase of collapse. (b) The free-fall time has littleeffect on the chemical abundances for our choice of the parameters. (c)Dynamical chemical evolution is required to describe the CO gas phase abundanceas well as the CO ice formation for the mean grain size larger then 1$\mu{}$m.(d) Furthermore, dust mean size and size distribution have a strong effect onchemical abundances and hence on the ionization degree and magneticdissipation. We conclude that dust grain growth in the collapse simulations canbe as important as coupling the collapse with chemistry.

3D radiative hydrodynamic simulations of protostellar collapse with H-C-O dynamical chemistry