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Abstract

We perform a set of two-dimensional, non-relativistic, hydrodynamics
simulations for supernova-like explosion associated with stellar core collapse
of rotating massive stars to a system of a black hole and a disk connected by
the transfer of matter and angular momentum. Our model of the central engine
also includes the contribution of the disk wind. In this work, we specifically
investigate the wind-driven explosion of rotating, large-mass progenitor stars
with the zero-age main-sequence mass of $M_\mathrm{ZAMS}=20\,M_\odot$ from
arXiv:2008.09132 . This study is carried out using the open-source hydrodynamic
code Athena++, for which we implement a method to calculate self-gravity for
axially symmetric density distributions. We, then, investigate the explosion
properties and the $^{56}$Ni production as a function of (varying) some
features of the wind injection. We find a large variety of explosion energy
with $E_\mathrm{expl}$ ranging from $\sim 0.049\times10^{51}$~erg to $\sim
34\times10^{51}$~erg and ejecta mass $M_\mathrm{ej}$ from 0.58 to 6 $M_\odot$,
which shows a bimodal distribution in high- and low-energy branches. We
demonstrate that the resulting outcome of a highly- or sub-energetic explosion
for a certain stellar structure is mainly determined by the competition between
the ram pressure of the injected matter and that of the infalling envelope. In
the nucleosynthesis analysis the $^{56}$Ni mass produced in our models goes
from $< 0.2~M_\odot$ in the sub-energetic explosions to $2.1~M_\odot$ in the
highly-energetic ones. These results are consistent with the observational data
of stripped-envelope and high-energy SNe such as broad-lined type Ic SNe.
However, we find a tighter correlation between the explosion energy and the
ejecta mass than that observationally measured.