We have performed a set of 11 three-dimensional magnetohydrodynamical
(MHD) core-collapse supernova simulations in order to investigate the
dependences of the gravitational wave signal on the progenitor’s initial
conditions. We study the effects of the initial central angular velocity and
different variants of neutrino transport. Our models are started up from a
15M progenitor and incorporate an effective general relativistic gravitational
potential and a finite temperature nuclear equation of state. Furthermore, the
electron flavour neutrino transport is tracked by efficient algorithms for the
radiative transfer of massless fermions. We find that non- and slowly rotating
models show gravitational wave emission due to prompt- and lepton driven
convection that reveals details about the hydrodynamical state of the fluid
inside the protoneutron stars. Furthermore we show that protoneutron stars
can become dynamically unstable to rotational instabilities at T/|W| values as
low as ∼2% at core bounce. We point out that the inclusion of deleptonization
during the postbounce phase is very important for the quantitative gravitational
wave (GW) prediction, as it enhances the absolute values of the gravitational
wave trains