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We study the global star-formation rate (SFR) vs. stellar mass (M$_*$)correlation, and the spatially-resolved SFR surface density ($\Sigma_{SFR}$)vs. stellar mass surface density (\Sm) correlation, in a sample of $\sim2,000$galaxies from the MaNGA MPL-5 survey. We classify galaxies andspatially-resolved areas into star-forming and retired according to theirionization processes. We confirm the existence of a Star-Forming Main Sequence(SFMS) for galaxies and spatially-resolved areas, and show that they have thesame nature, with the global as a consequence of the local one. The latterpresents a bend below a limit \Sm value, $\approx 3\times 10^7$M$_\odot$kpc$^{-2}$, which is not physical. Using only star-forming areas(SFAs) above this limit, a slope and a scatter of $\approx1$ and $\approx0.27$dex are determined. The retired galaxies/areas strongly segregate from theirrespective SFMS's, by $\sim -1.5$ dex on average. We explore how theglobal/local SFMS's depend on galaxy morphology, finding that for star-forminggalaxies and SFAs, there is a trend to lower values of star-formation activitywith earlier morphological types, which is more pronounced for the local SFMS.The morphology not only affects the global SFR due to the diminish of SFAs withearlier types, but also affects the local SF process. Our results suggest thatthe local SF at all radii is established by some universal mechanism partiallymodulated by morphology. Morphology seems to be connected to the slow aging andsharp decline of the SF process, and on its own it may depend on otherproperties as the environment.

SDSS-IV MaNGA: Effects of Morphology in the global and local Star Formation Main Sequences