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We report on the gravitational wave signal computed in the context of athree-dimensional simulation of a core collapse supernova explosion of a 15Solar mass star. The simulation was performed with our neutrino hydrodynamicscode Chimera. We detail the gravitational wave strains as a function of time,for both polarizations, and discuss their physical origins. We also present thecorresponding spectral signatures. Gravitational wave emission in our model hastwo key features: low-frequency emission (< 200 Hz) emanates from the gainlayer as a result of neutrino-driven convection and the SASI and high-frequencyemission (> 600 Hz) emanates from the proto-neutron star due to Ledouxconvection within it. The high-frequency emission dominates the gravitationalwave emission in our model and emanates largely from the convective layeritself, not from the convectively stable layer above it, due to convectiveovershoot. Moreover, the low-frequency emission emanates from the gain layeritself, not from the proto-neutron star, due to accretion onto it. We provideevidence of the SASI in our model and demonstrate that the peak of ourlow-frequency gravitational wave emission spectrum corresponds to it. Given itsorigin in the gain layer, we classify the SASI emission in our model as p-modeemission and assign a purely acoustic origin, not a vortical-acoustic origin,to it. Our dominant proto-neutron star gravitational wave emission is not wellcharacterized by emission from surface g-modes, complicating the relationshipbetween peak frequencies observed and the mass and radius of the proto-neutronstar expressed by analytic estimates under the assumption of surface g-modeemission. We present our frequency normalized characteristic strain along withthe sensitivity curves of current- and next-generation gravitational wavedetectors.

Gravitational-wave signal of a core-collapse supernova explosion of a 15 Solar mass star