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Galactic bars are important drivers of galactic evolution, and yet how theyimpact the interstellar medium and correspondingly star formation, remainsunclear. We present simulation results for two barred galaxies with differentformation mechanisms, bars formed in isolation or via a tidal interaction, toconsider the spatially and temporally varying trends of star formation. Wefocus on the early (< 1Gyr) epoch of bar formation so that the interaction isclearly identifiable. The nearby NGC 4303 (isolated) and NGC 3627 (interactionhistory) are selected as observational analogues to tailor these simulations.Regardless of formation mechanism, both models show similar internal dynamicalfeatures, although the interaction appears to promote bar-arm disconnection inthe outer disc velocity structure. Both bars trigger similar boosts in starformation (79%; 66%), while the interaction also triggers an earlier 31% burst.Significant morphological dependence is observed in the relation betweensurface gas and star formation rate. In both cases, the bar component isnotably steepest; the arm is similar to the overall disc average; and theinter-arm clearly the shallowest. A distinguishable feature of the tidal discis the presence of moderately dense, inefficiently star forming gas mostlyconfined to tidal debris outside the optical disc. The tidal disc also exhibitsa unique trend of radially increasing star formation efficiency and a cleardearth of star formation which persists along the bar between the centre andbar ends. These are potential signatures for identifying a barred systempost-interaction.

Differences in star formation activity between tidally triggered and isolated bars: a case study of NGC 4303 and NGC 3627