Non-radial instabilities during the violent birth of neutron stars

Despite interesting and exiting discoveries achieved so far, our 3D simulations have not (yet) provided successful supernova explosions, different from corresponding 2D models. Higher grid resolution is therefore demanded to reduce the still worrisome influence of numerical viscosity. Stellar core rotation, even on a low level, can play an important role for the growth rate of the spiral SASI. Also uncertain microphysics like the high-temperature, high-density equation of state of neutron star matter need to be tested for their impact on the development of the explosion. More computer time for a larger number and for better resolved models is therefore urgently needed. (orig.)