Speaker
Description
At the end of its evolution, the collapse of a massive star's core into a proto-neutron star is the starting point for a complex sequence of events with many possible outcomes.
Specifically, very compact and rotating stars with a high mass ($M_*>16 \,M_\odot$), are likely to create a so-called ``failed core-collapse supernova'', forming a black hole surrounded by an accreting disk. It has been shown that the disk wind generated through viscous dissipation inside the disk may be the source of high energy ($E_\mathrm{expl}>10^{52}$ erg) supernovae with a high $^{56}$Ni mass (M$_{^{56}{Ni}}\ge 0.1\, M_\odot$).
In this scenario, the properties of the ejecta and the $^{56}$Ni production are strongly related to the wind injection from the accretion disk. In this talk, I will analyze these properties, investigating the impact of the disk mass and energy injected from the system on the final ejecta. I will focus on observational properties such as the explosion energy, the ejecta mass, and the $^{56}$Ni mass produced for different progenitor model. I will then show the strong correlation between the explosion energy and the ejecta mass, and compare our results for the $^{56}$Ni mass distribution with observational data.
