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

Understand

The subsequent observing runs of the advanced gravitational-wave detector network will likely provide us with various gravitational-wave observations of binary neutron star systems.

• For an accurate interpretation of these detections, we need reliable gravitational-wave models.
• To test and to point out how existing models could be improved, we perform a set of high-resolution numerical-relativity simulations for four different physical setups with mass ratios $q$ = $1.25$, $1.50$, $1.75$, $2.00$, and total gravitational mass $M = 2.7M_\odot$ .
• Each configuration is simulated with five different resolutions to allow a proper error assessment.