Figure 14: Dimensionless GW strain , where is the distance to the source and
the total mass of the binary, versus time for four different NS-NS merger calculations. The different
merger types become apparent in the post-merger GW signal, clearly indicating how BH formation
rapidly drives the GW signal down to negligible amplitudes. Image reproduced by permission from
Figures 5 and 6 of [134], copyright by APS.
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