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 _ { TOV } and the maximum mass supported through uniform rotation M _ { max } = \left ( 1.20 ^ { +0.02 } _ { -0.05 } \right ) M _ { TOV } we set limits for the maximum mass to be 2.01 ^ { +0.04 } _ { -0.04 } \leq M _ { 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 .