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The subsequent observing runs of the advanced gravitational-wave detectornetwork will likely provide us with various gravitational-wave observations ofbinary neutron star systems. For an accurate interpretation of thesedetections, we need reliable gravitational-wave models. To test and to pointout how existing models could be improved, we perform a set of high-resolutionnumerical-relativity simulations for four different physical setups with massratios $q$ = $1.25$, $1.50$, $1.75$, $2.00$, and total gravitational mass $M =2.7M_\odot$ . Each configuration is simulated with five different resolutionsto allow a proper error assessment. Overall, we find approximately 2nd orderconverging results for the dominant $(2,2)$, but also subdominant $(2,1)$,$(3,3)$, $(4,4)$ modes, while, generally, the convergence order reducesslightly for an increasing mass ratio. Our simulations allow us to validatewaveform models, where we find generally good agreement betweenstate-of-the-art models and our data, and to prove that scaling relations forhigher modes currently employed for binary black hole waveform modeling alsoapply for the tidal contribution. Finally, we also test if the current NRTidalmodel to describe tidal effects is a valid description for high-mass ratiosystems. We hope that our simulation results can be used to further improve andtest waveform models in preparation for the next observing runs.

High-accuracy high-mass ratio simulations for binary neutron stars and their comparison to existing waveform models