  Combining the GW observations of merging systems of binary neutron stars and
quasi-universal relations, we set constraints on the maximum mass that can be
attained by nonrotating stellar models of neutron stars. More specifically,
exploiting the recent observation of the GW event GW 170817 and drawing from
basic arguments on kilonova modeling of GRB 170817A, together with the
quasi-universal relation between the maximum mass of nonrotating stellar models
$M_{\rm TOV}$ and the maximum mass supported through uniform rotation $M_{\rm
max}=\left(1.20^{+0.02}_{-0.05}\right) M_{\rm TOV}$ we set limits for the
maximum mass to be $ 2.01^{+0.04}_{-0.04}\leq M_{\rm TOV}/M_{\odot}\lesssim
2.16^{+0.17}_{-0.15}$, where the lower limit in this range comes from pulsar
observations. Our estimate, which follows a very simple line of arguments and
does not rely on the modeling of the electromagnetic signal in terms of
numerical simulations, can be further refined as new detections become
available. We briefly discuss the impact that our conclusions have on the
equation of state of nuclear matter.
