Self-consistent Modeling of the Dynamics and Chemistry of Molecular Clouds in Different Evolutionary Stages

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The process of star formation covers a tremendous range of physical conditions and size scales. It also involves a variety of dynamical processes. Due to the difficulty of direct observations of the most abundant molecule H2, we are forced to assess the dynamical state of star-forming regions through observations of trace species that are not necessarily well mixed with molecular hydrogen. Thus, to interpret adequately results of observations, self-consistent models of the dynamical and chemical evolution are required. We intend to create such a model in which all relevant processes are taken into account, including up-to-date information about the chemical reaction rates, cooling and heating rates, diffusion, and grain surface reactions. This model will be coupled with 1D- and 2D-hydrodynamical models and compared with other chemical codes and observational data.