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We estimate the current extinction-corrected H$\alpha$ star formation rate(SFR) of the different morphological components that shape galaxies (bulges,bars, and disks). We use a multi-component photometric decomposition based onSDSS imaging to CALIFA Integral Field Spectroscopy datacubes for a sample of219 galaxies. This analysis reveals an enhancement of the central SFR andspecific SFR (sSFR $=$ SFR/$M_{\star}$) in barred galaxies. Along the MainSequence, we find more massive galaxies in total have undergone efficientsuppression (quenching) of their star formation, in agreement with manystudies. We discover that more massive disks have had their star formationquenched as well. We evaluate which mechanisms might be responsible for thisquenching process. The presence of type-2 AGNs plays a role at damping the sSFRin bulges and less efficiently in disks. Also, the decrease in the sSFR of thedisk component becomes more noticeable for stellar masses around 10$^{10.5}$M$_{\odot}$; for bulges, it is already present at $\sim$10$^{9.5}$ M$_{\odot}$.The analysis of the line-of-sight stellar velocity dispersions ($\sigma$) forthe bulge component and of the corresponding Faber-Jackson relation shows thatAGNs tend to have slightly higher $\sigma$ values than star-forming galaxiesfor the same mass. Finally, the impact of environment is evaluated by means ofthe projected galaxy density, $\Sigma$$_{5}$. We find that the SFR of bothbulges and disks decreases in intermediate-to-high density environments. Thiswork reflects the potential of combining IFS data with 2D multi-componentdecompositions to shed light on the processes that regulate the SFR.

Star formation in the local Universe from the CALIFA sample. II. Activation and quenching mechanisms in bulges, bars, and disks