Hydrogen-rich supernovae (SNe II) show a wide diversity in their light curves and spectral evolution, shaped by differences in the progenitor stars that produce them, the explosion, and their immediate environment. In this talk, I'll dive into the main factors that contribute to this diversity, including the star’s hydrogen envelope mass and radius, explosion energy, metallicity, circumstellar material (CSM), and the amount of radioactive nickel (56Ni) synthesized, as well as the extent of 56Ni mixing within the ejecta. Drawing results from work on several SNe II, I’ll look at how these aspects influence early flux excess, light curve decline rates, color evolution, and spectroscopic evolution of line widths and line profiles. I’ll also discuss insights from polarimetric observations, which reveal explosion asymmetries, and consider how interactions with the surrounding CSM create distinctive spectral and light curve signatures. Using observational data along with theoretical models, this presentation aims to shed light on the factors that drive the heterogeneity in SNe II and the characteristics of their progenitor systems.
Zoom ID: 622 1126 9644