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

Second release of the CoRe database of binary neutron star merger waveforms

“…The database contains waveforms from binaries with total masses ranging from 2.4 M to around ∼3.4 M with 45 datasets reaching mass ratios larger than q 1.4 and up to q = 2.1 [45,56,62]. EOS effect can be summarized to some extent § by the quadrupolar tidal polarizability parameters Λ 1,2 [68], where larger (smaller) values of Λ i are associated to stiffer (softer) EOSs.…”

“…Extreme mass ratios q ∼ 2 and NS rotation close to the breakup limit remain challenging to simulate as well as to obtain clean convergence in GW higher (subdominant) modes like ( , m) = (2, 1), (3,3) and (4,4). Work in these directions is ongoing [56,60,62,63]. For example, clear fourth order convergence in the subdominant (3, 2) and (4, 4) modes for q = 1 has been shown in [63].…”

“…The new data were computed in simulations presented in Refs. [52][53][54][55][56][57][58][59][60][61][62][63][64] and include BNS waveforms consistent with the GW events GW170817 [54,56,57,65] and GW190425 [64,66].…”