Core-collapse supernova from a possible progenitor star of 100 M⊙\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$M_{\odot }$$\end{document}

In this work, we study the synthetic explosions of a massive star. We take a 100 M⊙\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$M_{\odot }$$\end{document} zero-age main-sequence (ZAMS) star and evolve it until the onset of core-collapse using MESA. Then, the resulting star model is exploded using the publicly available stellar explosion code, STELLA. The outputs of STELLA calculations provide the bolometric light curve and photospheric velocity evolution along with other physical properties of the underlying supernova. In this paper, the effects of having a large Hydrogen-envelope on the supernova light curve have been explored. We also explore the effects of the presence of different amounts of nickel mass and the variation of the explosion energy of the supernovae from such heavy progenitors, on the bolometric light curves and photospheric velocities.