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The first multimessenger observation attributed to a merging neutron starbinary provided an enormous amount of observational data. Unlocking the fullpotential of this data requires a better understanding of the merger processand the early post-merger phase, which are crucial for the later evolution thateventually leads to observable counterparts. In this work, we perform standardhydrodynamical numerical simulations of a system compatible with GW170817. Wefocus on a single equation of state (EOS) and two mass ratios, while neglectingmagnetic fields and neutrino radiation. We then apply newly developedpostprocessing and visualization techniques to the results obtained for thisbasic setting. The focus lies on understanding the three-dimensional structureof the remnant, most notably the fluid flow pattern, and its evolution untilcollapse. We investigate the evolution of mass and angular momentumdistribution up to collapse, as well as the differential rotation along andperpendicular to the equatorial plane. For the cases that we studied, theremnant cannot be adequately modeled as a differentially rotating axisymetricNS. Further, the dominant aspect leading to collapse is the GW radiation andnot internal redistribution of angular momentum. We relate features of thegravitational wave signal to the evolution of the merger remnant, and make thewaveforms publicly available. Finally, we find that the three-dimensionalvorticity field inside the disk is dominated by medium-scale perturbances andnot the orbital velocity, with potential consequences for magnetic fieldamplification effects.

Numerical Inside View of Hypermassive Remnant Models for GW170817