The rate at which stars form is linked to the timescales involved in the dissipation of the non-thermal, turbulent, energy density. The deep understanding of the main physical processes driving the dissipation of interstellar turbulence can only be obtained through the interplay between observations of molecular clouds and numerical simulations.
To which extent are the interstellar and prestellar volatile reservoirs preserved during the star and planet formation sequence ? Timescales of the star formation process ? Physical and chemical conditions in the prestellar phase ?
Gas phase budgets of carbon, oxygen, nitrogen, sulphur ? What is the primary reservoir of volatile nitrogen at different stages from cores to disks ?