Статья

Rotating collapse of stellar iron cores in general relativity

Christian D. OttJINA Postdoctoral Fellow, Department of Astronomy and Steward Observatory, The University of Arizona, Tucson, AZ 85721, USAHarald DimmelmeierMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, GermanyAlexander MarekMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, GermanyH-T JankaMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, GermanyBurkhard ZinkCenter for Computation and Technology, Louisiana State University, 216 Johnston Hall, Baton Rouge, LA 70803, USAIan HawkeSchool of Mathematics, University of Southampton, Southampton SO17 1BJ, UKErik SchnetterCenter for Computation and Technology, Louisiana State University, 216 Johnston Hall, Baton Rouge, LA 70803, USA

2007en

ABI

Аннотация

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.

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Идентификаторы

DOI: 10.1088/0264-9381/24/12/s10

Цитирования и источники

Цитирований: 2Использованных источников: 0

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