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The strong time-dependence of the dynamics of galactic bars yields a complexand rapidly evolving distribution of dense gas and star forming regions.Although bars mainly host regions void of any star formation activity, theirextremities can gather the physical conditions for the formation of molecularcomplexes and mini-starbursts. Using a sub-parsec resolution hydrodynamicalsimulation of a Milky Way-like galaxy, we probe these conditions to explore howand where bar (hydro-)dynamics favours the formation or destruction ofmolecular clouds and stars. The interplay between the kpc-scale dynamics (gasflows, shear) and the parsec-scale (turbulence) is key to this problem. We finda strong dichotomy between the leading and trailing sides of the bar, in termof cloud fragmentation and in the age distribution of the young stars. Afterorbiting along the bar edge, these young structures slow down at theextremities of the bar, where orbital crowding increases the probability ofcloud-cloud collision. We find that such events increase the Mach number of thecloud, leading to an enhanced star formation efficiency and finally theformation of massive stellar associations, in a fashion similar togalaxy-galaxy interactions. We highlight the role of bar dynamics in decouplingyoung stars from the clouds in which they form, and discuss the implications onthe injection of feedback into the interstellar medium, in particular in thecontext of galaxy formation.

Environmental regulation of cloud and star formation in galactic bars