Gravitational Wave Analysis as a Tool to Investigate Core Collapse Supernovae

Gravitational waves (GWs) offer the unique opportunity to observe the dynamics of the most extreme regions deep within a core collapse supernova (CCSN). Using 2D and 3D simulations from the massively parallel CCSN code, CHIMERA, I will present the GW strains computed for a range of progenitors varying in mass, metallicity, and internal structure. Using these strains, spectrograms are produced with features that relate directly to the evolution of the CCSN. In particular, the dynamics of the proto-neutron star (PNS) and its contraction are tracked well by the so-called high-frequency feature (HFF). I will present the results of spatially decomposing GW generation into regions within and around the PNS and highlight the differences observed between 2D and 3D simulations. Additionally, for 2D simulations I discuss how a CCSN GW detection can be used to discern effects of differing nuclear equations of state, with current generation detectors, using real interferometric noise. Finally, using linear perturbative analysis consistent with the treatment of gravity in CHIMERA, I determine the PNS vibrational modes that contribute most strongly to GW generation. Combining this analysis with the spatial decomposition of GW generation within the CCSN allows for in-depth investigation of the sources of GWs and the potential for parameter estimation of the PNS mass and radius.