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We present the gravitational wave analysis from rotating (model s15g) andnearly non-rotating (model s15h) 3D MHD core collapse supernova simulations atbounce and the first couple of ten milliseconds afterwards. The simulations arelaunched from 15M_{\odot} progenitor models stemming from stellar evolutioncalculations. Gravity is implemented by a spherically symmetric effectivegeneral relativistic potential. The input physics uses the Lattimer-Swestyequation of state for hot, dense matter and a neutrino parametrisation schemethat is accurate until the first few ms after bounce. The 3D simulations allowus to study features already known from 2D simulations as well asnonaxisymmetric effects. In agreement with recent results we find only type Igravitational wave signals at core bounce. In the later stage of thesimulations, one of our models (s15g) shows nonaxisymmetric gravitational waveemission caused by a low T/|W| dynamical instability, while the other modelradiates gravitational waves due to a convective instability in theprotoneutron star. The total energy released in gravitational waves within theconsidered time intervals is 1.52\times10^{-7}M_{\odot} (s15g) and4.72\times10^{-10}M_{\odot} (s15h). Both core collapse simulations indicatethat corresponding events in our Galaxy would be detectable either by the LIGOor Advanced LIGO detector.

Gravitational waves from 3D MHD core collapse simulations