http://arxiv.org/abs/1406.2415
We present an overview of axisymmetric core-collapse supernova simulations employing neutrino transport scheme by the isotropic diffusion source approximation. Studying 101 solar-metallicity progenitors covering zero-age main sequence mass from 10.8 to 75.0 solar masses, we systematically investigate how the differences in the structures of these multiple progenitors impact the hydrodynamics evolution. By following a long-term evolution over 1.0 s after bounce, most of the computed models exhibit neutrino-driven revival of the stalled bounce shock at about 200 – 800 ms postbounce, leading to the possibility of explosion. Pushing the boundaries of expectations in previous one-dimensional studies, our results show that the time of shock revival, evolution of shock radii, and diagnostic explosion energies are tightly correlated with the compactness parameter xi which characterizes the structure of the progenitors. Compared to models with low xi, models with high xi undergo high ram pressure from the accreting matter onto the stalled shock and it takes longer time before the shock expansion is initiated under the influence of neutrino-driven convection and the standing accretion-shock instability. We find that the accretion luminosity becomes higher for models with high xi, which makes the diagnostic energy higher and the synthesized nickel mass bigger. We point out that these explosion characteristics tend to show a monotonic increase as a function of the compactness parameter xi.
K. Nakamura, T. Takiwaki, T. Kuroda, et. al.
Wed, 11 Jun 14
10/68
Comments: 6 pages, 5 figures, ApJL submitted
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