  We analyse a sample of massive disk galaxies selected from the SDSS-IV/MaNGA
survey to investigate how the evolution of these galaxies depends on their
stellar and halo masses. We applied a semi-analytic spectral fitting approach
to the data from different regions in the galaxies to derive several of their
key physical properties. From the best-fit model results, together with direct
observables such as morphology, colour, and the Mgb/$\langle$Fe$\rangle$ index
ratio measured within $1 R_{\rm e}$, we find that for central galaxies both
their stellar and halo masses have a significant influence in their evolution.
For a given halo mass, galaxies with higher stellar mass accumulate their
stellar mass and become chemically enriched earlier than those with smaller
stellar mass. Furthermore, at a given stellar mass, galaxies living in more
massive halos have longer star-formation timescales and are delayed in becoming
chemically enriched. In contrast, the evolution of massive satellite galaxies
is mostly determined by their stellar mass. The results indicate that both the
assembled halo mass and the halo assembly history impact the evolution of
central galaxies. Our spatially resolved analysis indicates that only the
galaxy properties in the central region ($0.0$--$0.5 R_{\rm e}$) show the
dependencies described above. This fact supports a halo-driven formation
scenario since the galaxies' central regions are more likely to contain old
stars formed along with the halo itself, keeping a memory of the halo formation
process.
