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Fully general-relativistic binary-neutron-star (BNS) merger simulations withquark-hadron crossover (QHC) equations of state (EOSs) are studied for thefirst time. In contrast to EOSs with purely hadronic matter or with afirst-order quark-hadron phase transition (1PT), in the transition region QHCEOSs show a peak in sound speed, and thus a stiffening. We study the effects ofsuch stiffening in the merger and post-merger gravitational (GW) signals.Through simulations in the binary-mass range $2.5 < M/M_{\odot} < 2.75$,characteristic differences due to different EOSs appear in the frequency of themain peak of the post-merger GW spectrum ($f_2$), extracted through Bayesianinference. In particular, we found that (i) for lower-mass binaries, since themaximum baryon number density ($n_{\rm max}$) after the merger stays below$3\text{--}4$ times the nuclear-matter density ($n_0$), the characteristicstiffening of the QHC models in that density range results in a lower $f_2$than that computed for the underlying hadronic EOS and thus also than that forEOSs with a 1PT, (ii) for higher-mass binaries, where $n_{\rm max}$ may exceed$4\text{--}5 n_0$ depending on the EOS model, whether $f_2$ in QHC models ishigher or lower than that in the underlying hadronic model depends on theheight of the sound-speed peak. Comparing the values of $f_2$ for differentEOSs and BNS masses gives important clues on how to discriminate differenttypes of quark dynamics in the high-density end of EOSs and is relevant tofuture kilohertz GW observations with third-generation GW detectors.

Merger and post-merger of binary neutron stars with a quark-hadron crossover equation of state