Prospects for optical detections from binary neutron star mergers with the next-generation multi-messenger observatories

Open Access

Fig. 3.

Mass of the first component (left) and the second component (right) of the ejecta, as defined in Eqs. (12) and (14), respectively, for the EOS BLh. The solid and the dashed black lines mark the chirp mass of GW170817 and GW190425, respectively.

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