Monday, September 9, 2013, 1:30 PM 385E

Inflence of Precollapse Angular Momentum Distribution on Stellar Collapse and it's Gravitational Wave Signature

Alexandra DeMaio (Rutgers University and TAPIR, CalTech)

Core-collapse supernovae (CCSN) are theorized to produce gravitational waves that can be detected by observatories such as Advanced LIGO. We present results from detailed 2D, axisymmetric, equatorially symmetric, general relativistic simulations of core-collapse supernovae in the bounce and post-bounce phases, investigating the effects of precollapse differential rotation and central angular velocity on post-bounce stellar dynamics and gravitational wave signals. We conclude that the distribution of angular momentum is only detectable in CCSN from rapidly rotating progenitor stars. Principle component analysis via singular value decomposition is used in conjunction with Bayesian techniques to determine the potency of observed disparities among the model waveforms.