3D Collapse of Rotating Stellar Iron Cores in General Relativity Including Deleptonization and a Nuclear Equation of State
Christian D. OttMax-Planck-Institut für Gravitationsphysik, Albert-Einstein-Institut, Am Mühlenberg 1, D-14476 Potsdam, GermanyHarald DimmelmeierMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85741 Garching, GermanyAndreas MarekMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85741 Garching, GermanyHans‐Thomas JankaMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85741 Garching, GermanyIan HawkeSchool of Mathematics, University of Southampton, Southampton SO17 1BJ, UKBurkhard ZinkCenter for Computation and Technology, Louisiana State University, Baton Rouge, Louisiana 70803, USAErik SchnetterCenter for Computation and Technology, Louisiana State University, Baton Rouge, Louisiana 70803, USA
2007en
ABI
Аннотация
We present 2D and 3D simulations of the collapse of rotating stellar iron cores in general relativity employing a nuclear equation of state and an approximate treatment of deleptonization. We compare fully general relativistic and conformally flat evolutions and find that the latter treatment is sufficiently accurate for the core-collapse supernova problem. We focus on gravitational wave (GW) emission from rotating collapse, bounce, and early postbounce phases. Our results indicate that the GW signature of these phases is much more generic than previously estimated. We also track the growth of a nonaxisymmetric instability in one model, leading to strong narrow-band GW emission.
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