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The detection of the binary events GW170817 and GW190814 has providedinvaluable constraints on the maximum mass of nonrotating configurations ofneutron stars, $M_{_{\rm TOV}}$. However, the large differences in theneutron-star masses measured in GW170817 and GW190814 has also lead to asignificant tension between the predictions for such maximum masses, withGW170817 suggesting that $M_{_{\rm TOV}} \lesssim 2.3\,M_{\odot}$, and GW190814requiring $M_{_{\rm TOV}} \gtrsim 2.5\,M_{\odot}$ if the secondary was a (non-or slowly rotating) neutron star at merger. Using a genetic algorithm, wesample the multidimensional space of parameters spanned by gravitational-waveand astronomical observations associated with GW170817. Consistent withprevious estimates, we find that all of the physical quantities are inagreement with the observations if the maximum mass is in the range $M_{_{\rmTOV}} = 2.210^{+0.116}_{-0.123} \,M_{\odot}$ within a $2\textrm{-}\sigma$confidence level. By contrast, maximum masses with $M_{_{\rm TOV}} \gtrsim2.5\,M_{\odot}$, not only require efficiencies in the gravitational-waveemission that are well above the numerical-relativity estimates, but they alsolead to a significant under-production of the ejected mass. Hence, the tensioncan be released by assuming that the secondary in GW190814 was a black hole atmerger, although it could have been a rotating neutron star before.

GW170817 and GW190814: tension on the maximum mass