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To understand star formation in galaxies, we investigate the star formationrate (SFR) surface density ($\Sigma_{\rm SFR}$) profiles for galaxies, based ona well-defined sample of 976 star-forming MaNGA galaxies. We find that thetypical $\Sigma_{\rm SFR}$ profiles within 1.5Re of normal SF galaxies can bewell described by an exponential function for different stellar mass intervals,while the sSFR profile shows positive gradients, especially for more massive SFgalaxies. This is due to the more pronounced central cores or bulges ratherthan the onset of a `quenching' process. While galaxies that lie significantlyabove (or below) the star formation main sequence (SFMS) show overall anelevation (or suppression) of $\Sigma_{\rm SFR}$ at all radii, this centralelevation (or suppression) is more pronounced in more massive galaxies. Thedegree of central enhancement and suppression is quite symmetric, suggestingthat both the elevation and suppression of star formation are following thesame physical processes. Furthermore, we find that the dispersion in$\Sigma_{\rm SFR}$ within and across the population is found to be tightlycorrelated with the inferred gas depletion time, whether based on the stellarsurface mass density or the orbital dynamical time. This suggests that we areseeing the response of a simple gas-regulator system to variations in theaccretion rate. This is explored using a heuristic model that canquantitatively explain the dependence of $\sigma(\Sigma_{\rm SFR})$ on gasdepletion timescale. Variations in accretion rate are progressively more dampedout in regions of low star-formation efficiency leading to a reduced amplitudeof variations in star-formation.

On the Elevation and Suppression of Star Formation within Galaxies