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Time-dependent and direction-dependent neutrino and gravitational-wave (GW)signatures are presented for a set of 3D hydrodynamic models of parametrized,neutrino-driven supernova explosions of non-rotating 15 and 20 solar massstars. We employ an approximate treatment of neutrino transport. Due to theexcision of the high-density core of the proto-neutron star and the use of anaxis-free overset grid, the models can be followed from the post-bounceaccretion phase for more than one second without imposing any symmetryrestrictions. GW and neutrino emission exhibit the generic time-dependentfeatures known from 2D models. Non-radial hydrodynamic mass motions in theaccretion layer and their interaction with the outer layers of theproto-neutron star together with anisotropic neutrino emission give rise to aGW signal with an amplitude of ~5-20 cm and frequencies 100--500 Hz. The GWemission from mass motions reaches a maximum before the explosion sets in.Afterwards the GW signal exhibits a low-frequency modulation, in some casesdescribing a quasi-monotonic growth, associated with the non-sphericalexpansion of the explosion shock wave and the large-scale anisotropy of theescaping neutrino flow. Variations of the mass-quadrupole moment due toconvective activity inside the nascent neutron star contribute a high-frequencycomponent to the GW signal during the post-explosion phase. The GW signalsexhibit strong variability between the two polarizations, different explosionsimulations and different observer directions, and does not possess anytemplate character. The neutrino emission properties show fluctuations over theneutron star surface on spatial and temporal scales that reflect the differenttypes of non-spherical mass motions. The modulation amplitudes of themeasurable neutrino luminosities and mean energies are significantly smallerthan predicted by 2D simulations.

Parametrized 3D models of neutrino-driven supernova explosions: Neutrino emission asymmetries and gravitational-wave signals