For decades, studies of galaxy evolution have relied on the global properties. Some scaling relations and evolutionary trends in the global scale have been revealed from these studies. Nowadays, there is a growing interest on studying spatially resolved properties of galaxies with various techniques and instruments (such as IFU and grism spectroscopy) to reveal evolution of the spatially resolved properties of galaxies and get more insight on physical mechanism of the galaxy evolution. In this presentation, I will introduce results of our study on the spatially resolved properties of massive disk galaxies at z~0 and z~1 using our established spatially resolved SED fitting technique. From this study, we found a fundamental sub-galactic (~1 kpc scale) SFMS, namely spatially resolved SFMS, which hold in both of our z~1 and z~0 samples. Evolution of this relation shows a decreasing local sSFR and increasing prominence of a “flattening” at high-mass end from z~1 star-forming to z~0 quiescent samples which indicates a decreasing sSFR in entire galaxy region and the formation and growth of bulge. We also studied evolution of the radial profiles of SFR, stellar mass, and sSFR and made an empirical model that could connect the observed radial profiles at z~1 and z~0. Overall, our study revealed that massive disk galaxies tend to built their stellar mass and quenched their star formation activities from central region first, then propagates toward outskirt, i.e. inside-out stellar mass buildup and quenching.