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The Physics of Binary Neutron Star merger: Insight from general relativistic numerical simulations
Roberto De Pietri
131 (Building C, ground floor)
Building C, ground floor
In the eve of Gravitational Wave physics the characterization of the gravitational wave signal emitted by compact binary source will be a prominent role. We present results for three-dimensional simulations of the dynamics of binary neutron star (BNS) mergers from the late inspiral stage and the post-merger up to ∼20 ms after the system has merged, either to form a hyper-massive neutron star (NS) or a rotating black hole (BH). We report here results for equal and un-equal-mass models and on the strength of the Gravitational Signal and its dependence on the EOS, the total ADM mass and the mass ratio of the two stars.
We use a semi-realistic descriptions of the equation of state (EOS) where the EOS is described by a seven-segment piece-wise polytropic with a thermal component given by Γth =1.8. One of the important characteristics of the present investigation is that it is entirely performed using only publicly available open source software, the Einstein Toolkit for the evolution and the LORENE code for the generation of the initial models.