A systematic theoretical study of explosion energies in Core Collapse Supernovae

We suggest a new experimental approach to conduct a systematic study in core collapse supernovae (CCSNe) theory. We provide toy pre-supernova stages with controlled core and silicon sulfer (Si+S) layer masses solving NSE and QSE compostions respectively. We also demonstrated 1D hydrodynamic simulations with light bulb approximation using 6 models from core collapse to explosion in order to study the dependence of the interior structures of pre-supernova stages on both explosion energies and nickel masses. During the core collapse our simulation showed that Si+S layer masses are most important in deciding the time evolution of mass accretion rates after bounce. We also found that the lighter core mass models produce the more energetic explosions and larger amounts of nickel masses. When the Si+S layer masses are lighter, mass accretion rates are enhanced so that the heavy core mass models are prevented from producing powerful explosions. Our simulation shows neccesity of early time explosion to reproduce 10⁵¹ erg .