  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 and
spatially-resolved areas into star-forming and retired according to their
ionization processes. We confirm the existence of a Star-Forming Main Sequence
(SFMS) for galaxies and spatially-resolved areas, and show that they have the
same nature, with the global as a consequence of the local one. The latter
presents 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 their
respective SFMS's, by $\sim -1.5$ dex on average. We explore how the
global/local SFMS's depend on galaxy morphology, finding that for star-forming
galaxies and SFAs, there is a trend to lower values of star-formation activity
with 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 with
earlier types, but also affects the local SF process. Our results suggest that
the local SF at all radii is established by some universal mechanism partially
modulated by morphology. Morphology seems to be connected to the slow aging and
sharp decline of the SF process, and on its own it may depend on other
properties as the environment.
