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We compare gravitational-wave (GW) signals from eight three-dimensionalsimulations of core-collapse supernovae, using two different progenitors withzero-age main sequence masses of 9 and 20 solar masses. The collapse of eachprogenitor was simulated four times, at two different grid resolutions and withtwo different neutrino transport methods, using the Aenus-Alcar code. The maingoal of this study is to assess the validity of recent concerns that theso-called "Ray-by-Ray+" (RbR+) approximation is problematic in core-collapsesimulations and can adversely affect theoretical GW predictions. Therefore,signals from simulations using RbR+ are compared to signals from correspondingsimulations using a fully multidimensional (FMD) transport scheme. The 9solar-mass progenitor successfully explodes, whereas the 20 solar-mass modeldoes not. Both the standing accretion shock instability and hot-bubbleconvection develop in the postshock layer of the non-exploding models. In theexploding models, neutrino-driven convection in the postshock flow isestablished around 100 ms after core bounce and lasts until the onset of shockrevival. We can, therefore, judge the impact of the numerical resolution andneutrino transport under all conditions typically seen in non-rotatingcore-collapse simulations. We find excellent qualitative agreement in all GWfeatures. We find minor quantitative differences between simulations, but findno systematic differences between simulations using different transportschemes. Resolution-dependent differences in the hydrodynamic behaviour oflow-resolution and high-resolution models have a greater impact on the GWsignals than consequences of the different transport methods. Furthermore,increasing the resolution decreases the discrepancies between models withdifferent neutrino transport.

Gravitational-wave Signals From Three-dimensional Supernova Simulations With Different Neutrino-Transport Methods