2006/12/31 by Christian D. Ott, Harald Dimmelmeier, Andreas Marek +6
Physics and Astronomy · #Astrophysics #Classical mechanics #Gamma-ray bursts and supernovae #General relativity #Gravitational collapse #Gravitational wave #Instability #Mechanics #Numerical relativity #Physics #Pulsars and Gravitational Waves Research #Stellar, planetary, and galactic studies #Supernova #Type II supernova #astro-ph #gr-qc
paper · pdf · doi:10.1088/0264-9381/24/12/s10
published as Class.Quant.Grav.24:S139-S154,2007 · 19 pages, 6 figures, minor corrections and additions; accepted for publication in the Proceedings of the New Frontiers in Numerical Relativity Conference, AEI Golm, Germany, 2006
arxiv created 2007/04/03 · openalex publication_date 2007/05/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present results from the first 2 + 1 and 3 + 1 simulations of the collapse of rotating stellar iron cores in general relativity employing a finite-temperature equation of state and an approximate treatment of deleptonization during collapse. We compare full 3 + 1 and conformally-flat spacetime evolution methods and find that the conformally-flat treatment is sufficiently accurate for the core-collapse supernova problem. We focus on the gravitational wave (GW) emission from rotating collapse, core bounce and early postbounce phases. Our results indicate that the GW signature of these phases is much more generic than previously estimated. In addition, we track the growth of a nonaxisymmetric instability of dominant m = 1 character in two of our models that leads to prolonged narrow-band GW emission at ∼920–930 Hz over several tens of milliseconds.