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High-mass gravitational-wave events in the neutron-star mass range, such asGW190425, have recently started to be detected by the LIGO/Virgo detectors. Ifthe masses of the two binary components fall in the neutron-star mass range,such a system is typically classified as a binary neutron-star system, althoughthe detected gravitational-wave signal may be too noisy to clearly establish aneutron-star nature of the high-mass component in the binary and rule out ablack hole--neutron star system for such an event. We here show that high-massbinary neutron-star mergers with a very massive neutron-star primary close tothe maximum-mass limit, $m_1 \gtrsim 2.2 \, M_\odot$, produce fast dynamicalmass ejecta from the spin-up of the primary star at merger. By simulating themerger of black hole--neutron star systems of exactly the same masses andspins, we show that these fast ejecta are entirely absent, if the primary isinstead a black hole. In addition, we find that both systems leave almostidentical amounts of baryon mass behind, which is not immediately accreted bythe black hole. This implies that both systems will likely have comparableelectromagnetic afterglow emission stemming from the remnant disk. Hence, fastejecta at merger have the potentialto distinguish neutron stars from blackholes in high-mass mergers, although these ejecta may be challenging to detectobservationally.

Fast ejecta as a potential way to distinguish black holes from neutron stars in high-mass gravitational-wave events