Fedrow_Ott_GR21_poster.pdf

We present gravitational wave predictions from new 3D simulations of rotating core-collapse supernovae. These simulations employ realistic progenitor models, a microphysical finite-temperature nuclear equation of state, and full general relativity. We explore the dependence of 3D dynamics and the associated gravitational wave emission as a function of the precollapse rotation rate. For rapid precollapse rotation resulting in protoneutron stars spinning at millisecond periods, we find the development of an m=1 instability that drives nonaxisymmetry and dramatically enhances the gravitational wave emission. We analyze the gravitational waveforms and provide detectability estimates for second and third generation gravitational wave observatories.<div><br>