All Tables

Table 1: Location of chemical interfaces in our progenitor model at 20 ms after core bounce.
Table 2: Computational setup for the 2D AMR calculation T310a. (see Sect. 6.2). The initial and final times over which the inner and outer grid boundaries were held fixed at $r_{\rm in}$ and $r_{\rm out}$ , are denoted by $t_{\rm i}$ and $t_{\rm f}$ , respectively. $\Delta r$ is the (absolute) resolution and $N^{\rm eff}_{\rm r}$ the number of equidistant radial zones that would have been required to cover the entire star in order to achieve a resolution of $\Delta r$ . Exponents are given in brackets.
Table 3: Parameters of Models O310 and T310. The (baryonic) mass of the inner core, $M_{\rm core}$ , that has been excluded from the simulation, and the final neutron star mass, $M_{\rm ns}$ , are given in solar masses. The initial and final radius of the inner core, $R_{\rm core}^{0}$ and $R_{\rm core}^{\infty }$ , respectively, are given in km, and its initial velocity of contraction, $\dot R_{\rm core}^{0}$ , in km s^-1. The initial neutrino luminosities of different flavours, $L_{\nu _{\rm e},52}^0$ , $L_{\bar \nu_{\rm e},52}^0$ , and $L_{\nu _x,52}^0$ (see also the main text), are given in units of $\rm 10^{52}~erg/s$ , and the energy loss of the inner core, $\Delta \varepsilon$ , in units of ${M_{\odot }} c^2$ . The explosion energy, $E_{\rm exp,51}$ , and the explosion time scale, $t_{\rm exp}$ , are given in $\rm 10^{51}~erg$ and in ms, respectively.
Table 4: Final total elemental yields (in ${M_{\odot }}$ ) for Models O310 and T310. Exponents are given in brackets.