Constraining the TOV mass of neutron stars with observation of GW170817

The first detection of the gravitational wave signal from a binary neutron star merger, GW170817, together with its electromagnetic counterparts, GRB170817A and AT2017gfo, has provided very important clues in the equation of state of dense matter at supra-nuclear densities and the internal structure of neutron stars. On one hand, the tidal deformability of the merging objects is encoded in the late inspiral signal which can be used to constrain the radius of neutron stars. On the other hand, the electromagnetic counterparts is closely related to the fate of the post-merger remnant, which is determined by the maximum mass of a spherical static neutron star (TOV maximum mass). In my talk, I will concentrate on the second point and introduce a recently established self-consistent analysis which includes the conservation of baryonic mass, energy and angular momentum at the same time. With such a new analysis, we actually found that the TOV mass range allowed by the observation of GW170817 and its electromagnetic counterparts are larger than several previous studies.