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We have simulated a set of 26 rotationnal supernova core collapse models
in axisymmetry. For a summary of the
assumptions and approximations of our core collapse simulations, please
go to current projects, Authors:
These figures contain the time evolution of the maximum density and the signal amplitude for all 26 simulated models. The solid and dashed lines denote the simulations in relativistic and Newtonian gravity, respectively. The signal amplitude AE220 can be converted to the strain hTT in the equatorial plane at a distance r from the source by the following expression:
The vertical dotted lines mark the time of reak maximum density (time of bounce), and the horizontal dotted lines in the density plots mark nuclear matter density, which we define as 2.0 . 1014 g/cm3. For non-toroidal models, the maximum density is identical to the central density.
These figures contain the time evolution of the maximum density and the signal amplitude for all 26 simulated models. The solid and dashed lines denote the simulations in relativistic and Newtonian gravity, respectively. The signal amplitude AE220 can be converted to the strain hTT in the equatorial plane at a distance r from the source by the following expression:
The vertical dotted lines mark the time of reak maximum density (time of bounce), and the horizontal dotted lines in the density plots mark nuclear matter density, which we define as 2.0 . 1014 g/cm3. For non-toroidal models, the maximum density is identical to the central density.
ewald@mpa-garching.mpg.de
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