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The main features of the gravitational dynamics of binary neutron starsystems are now well established. While the inspiral can be precisely describedin the post-Newtonian approximation, fully relativistic magneto-hydrodynamicalsimulations are required to model the evolution of the merger and post-mergerphase. However, the interpretation of the numerical results can often benon-trivial, so that toy models become a very powerful tool. Not only do theysimplify the interpretation of the post-merger dynamics, but also allow to gaininsights into the physics behind it. In this work, we construct a simple toymodel that is capable of reproducing the whole angular momentum evolution ofthe post-merger remnant, from the merger to the collapse. We validate the modelagainst several fully general-relativistic numerical simulations employing agenetic algorithm, and against additional constraints derived from the spectralproperties of the gravitational radiation. As a result, from the remarkablyclose overlap between the model predictions and the reference simulationswithin the first milliseconds after the merger, we are able to systematicallyshed light on the currently open debate regarding the source of thelow-frequency peaks of the gravitational wave power spectral density.Additionally, we also present two original relations connecting the angularmomentum of the post-merger remnant at merger and collapse to initialproperties of the system.

Shedding light on the angular momentum evolution of binary neutron star merger remnants: a semi-analytic model