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Context. Interstellar dust particles, which represent 1% of the total mass,are recognized to be very powerful interstellar catalysts in star-formingregions. The presence of dust can have a strong impact on the chemicalcomposition of molecular clouds. While observations show that many species thatformed onto dust grains populate the gas phase, the process that transformssolid state into gas phase remains unclear. Aims. The aim of this paper is toconsider the chemical desorption process, i.e. the process that releases solidspecies into the gas phase, in astrochemical models. These models allowdetermining the chemical composition of star-forming environments with anaccurate treatment of the solid-phase chemistry. Methods. In paper I we deriveda formula based on experimental studies with which we quantified theefficiencies of the chemical desorption process. Here we extend these resultsto astrophysical conditions. Results. The simulations of astrophysicalenvironments show that the abundances of gas-phase methanol and H2O2 increaseby four orders of magnitude, whereas gas-phase H2CO and HO2 increase by oneorder of magnitude when the chemical desorption process is taken into account.The composition of the ices strongly varies when the chemical desorption isconsidered or neglected. Conclusions. We show that the chemical desorptionprocess, which directly transforms solid species into gas-phase species, isvery efficient for many reactions. Applied to astrophysical environments suchas Rho Oph A, we show that the chemical desorption efficiencies derived in thisstudy reproduce the abundances of observed gas-phase methanol, HO2, and H2O2,and that the presence of these molecules in the gas shows the last signs of theevolution of a cloud before the frost.

Dust as interstellar catalyst - II. How chemical desorption impacts the gas