  Type IIP supernovae (SNe IIP) are thought to originate from the explosion of
massive stars > 10 Msun. Their luminosity is primarily powered by the explosion
energy and the radioactive decay energy of 56Co, with the photosphere location
regulated by hydrogen recombination. However, the physical connections between
SNe IIP and their progenitor stars remain unclear. This paper presents a
comprehensive study of SNe IIP and their progenitor stars by using the
one-dimensional stellar evolution code, MESA. Our model grids consider the
effects of stellar metallicity, mass, and rotation in the evolution of massive
stars, as well as explosion energy and 56Ni production in modeling supernovae.
To elucidate the observed SNe IIP and their origins, we compare their light
curves (LCs) with our models. Furthermore, we investigate the impact of stellar
parameters on LCs by considering stellar mass metallicity, rotation, explosion
energy, and 56Ni production. We find that more massive stars exhibit longer
plateaus due to increased photon diffusion time caused by massive ejecta.
Higher metallicity leads to increased opacity and mass loss of progenitor
stars. Rapid rotation affects internal stellar structures, enhancing convective
mixing and mass loss, potentially affecting the plateau's brightness and
duration. Higher explosion energy results in brighter but shorter plateaus due
to faster-moving ejecta. 56Ni mass affects late-time luminosity and plateau
duration, with larger masses leading to slower declines.
