All Tables

Table 1: Parameters of computed 2D models for progenitor stars with different masses. $\Omega _{{\rm i}}$ is the angular velocity of the Fe-core, which is assumed to rotate uniformly, prior to collapse, $\theta _0$ and $\theta _1$ are the polar angles of the lateral grid boundaries, and $N_{\theta }$ is the number of grid points in the lateral direction. $t_{\rm 2D}$ denotes the time (relative to the bounce time) when the simulation was started or continued in 2D.
Table A.1: List of progenitors used in the simulations. $M_{{\rm Fe-Si}}$ and $M_{{\rm Si-O}}$ are the enclosed masses at composition interfaces defined by entropy jumps. With (e) we denote that a shell interface is connected with a gradual enrichment of the lighter nucleus, i.e. these cases are Fe-FeSi and Si-SiO interfaces where the mass fractions of Si or O grows gradually outwards. The underlined numbers indicate an entropy increase of more than $1~\ensuremath{k_{\rm B}}$ per nucleon in case of an Fe-Si interface and an entropy increase of more than $2~\ensuremath{k_{\rm B}}$ /by in case of a Si-O interface.
Table B.1: Characteristic parameters of the 1D models for the phases of collapse, prompt shock propagation, and neutrino burst. $t_{\rm coll}$ is the time between the moment when the collapsing core reaches a central density of $10^{11}~\ensuremath{{\rm g}~{\rm cm}^{-3}}$ and the moment of shock creation (which is nearly identical with the time of core bounce), i.e. the time when the entropy behind the shock first reaches a value of $3~\ensuremath{k_{\rm B}}$ /by. The shock creation radius $r_{\rm sc}$ and enclosed mass $M_{\rm sc}$ are defined by the radial position where this happens. The energy loss $E_{\rm coll}^{\nu ,{\rm loss}}$ via neutrinos during the collapse phase is evaluated by integrating the total neutrino luminosity (for an observer at rest at r=400 km) over time from the moment when the core reaches $\rho_{\rm c} = 10^{11}~\ensuremath{{\rm g}~{\rm cm}^{-3}}$ until the moment when the dip in the $\nu _{{\rm e}}$ luminosity is produced around 2.5 ms after shock formation. We call the time when the velocities behind the shock drop below $10^7~~\ensuremath{{\rm cm}~{\rm s}^{-1}}$ the end of the prompt shock propagation phase. This time, $t_{\rm pse}$ , is measured relative to the moment of shock creation. At the end of the prompt shock propagation phase, the shock is at radius $r_{\rm pse}$ and its enclosed mass is $M_{\rm pse}$ . The time of the $\nu _{{\rm e}}$ burst, $t_{{\nu _{\rm e}}-{\rm burst}}$ , is defined as the post-bounce time when the $\nu _{{\rm e}}$ luminosity maximum is produced at the shock, which then is located at the radius $r_{{\nu _{\rm e}}-{\rm burst}}$ and mass $M_{{\nu _{\rm e}}-{\rm burst}}$ . Finally, the energy emitted during the prompt $\nu _{{\rm e}}$ burst is defined as the time-integrated $\nu _{{\rm e}}$ luminosity for the FWHM of the burst, $E_{\rm burst}^\nu$ , evaluated at 400 km for an observer at rest.