The Impact of Stellar Feedback on Astrochemistry
In the local universe, star formation occurs entirely in molecular clouds: the densest and coldest phase of the interstellar medium (ISM). Research into the astrochemical evolution of molecular clouds is essential to understand molecular cloud observations from theory. Molecular cloud observations show that different molecules are sensitive to different physical parameters, especially temperature and density. Theoretical simulations, however, are still lacking in depth three dimensional calculations with networks large enough to accurately incorporate many of the molecules observed. I will present early results from a three-dimensional ray-tracing algorithm to calculate the FUV radiation in-situ with time dependent hydrodynamic simulations. The ray-tracing algorithm allows efficient calculations of FUV radiation from external, and internal, sources through arbitrary density distributions. We can model large chemical networks in post processing with higher accuracy than ever before using the time dependent radiation field calculated in-situ with the hydrodynamics. These theoretical predictions of time dependent chemical distributions can then be compared to the extensive observational work.