Modeling the Progenitor Stars of Observed IIP Supernovae

The luminosity of Type IIP supernovae (SNe IIP) primarily arises from the recombination of hydrogen ionized by the explosion shock and the radioactive decay of . However, the physical connections between SNe IIP and their progenitor stars remain unclear. This paper presents a comprehensive grid of stellar evolution models and their corresponding supernova light curves (LCs) to investigate the physical properties of observed SNe IIP. The study employs the one-dimensional stellar evolution code, . Our models consider the effects of stellar metallicity, mass, and rotation in the evolution of massive stars, as well as explosion energy and production in modeling supernovae. To elucidate the observed LCs of SNe IIP and to probe their progenitor stars, we fit the observed SNe IIP with our multi-color LCs and discuss their physical origins. Furthermore, we investigate the impact of stellar parameters on LCs. Factors such as the progenitor star's mass, rotation, metallicity, explosion energy, and production influence the light curve's shape and duration. We find that higher-mass stars exhibit longer plateaus due to increased photon diffusion time caused by massive ejecta, impacting the duration of the light curve. Rapid rotation affects internal stellar structures, enhancing convective mixing and mass loss, potentially affecting the plateau's brightness and duration. Higher metallicity leads to increased opacity, altering energy transport and luminosity. Higher explosion energy results in brighter but shorter plateaus due to faster ejecta. production affects late-time luminosity and plateau duration, with larger masses leading to slower declines.