Summary of the simulations presented in this study. The first column specifies the type of system simulated. Second column denotes if the space–time was fixed or evolved dynamically. Third column indicates if the mesh was moving during the simulation. The fourth column contains information about the symmetry of the initial grids, which we employ in the different simulations. Fifth column indicates whether we employ cell refinement and derefinement in the respective simulation. In the sixth column, we provide an estimate for the resolution. In moving-mesh simulations, the resolution changes dynamically (see main text for more details on each simulation). In the case of the BNS systems, the resolution refers to the high-density regime in the post-merger phase. Columns seven and eight list the EOS and masses of the systems. Finally, the last column reports the characteristic frequency extracted in every simulation. In the case of TOV stars this refers to the frequency of the radial mode (f₀), while for the BNS systems it is the dominant frequency in the post-merger phase. The seventeenth row ‘pert. TOV star’ provides the perturbative result of the isolated TOV star for comparison. The TOV simulations marked with * and ^† refer to the simulation with arepo’s standard slope-limited gradient and the run with the regularization parameters set to (f_shaping, β) = (0.5, 3), respectively. The systems marked with ^‡ refer to the simulations discussed in Appendix D2. For the BNS simulation labelled with ^‡ we do not provide a characteristic frequency, because we evolve the system for <5 ms in the post-merger phase. For simulations labelled ‘case (i)’, ‘case (ii)’, and ‘case (iii)’ see Appendix D1.