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We perform fully relativistic calculations of binary neutron stars inquasi-equilibrium circular orbits. We integrate Einstein's equations togetherwith the relativistic equation of hydrostatic equilibrium to solve the initialvalue problem for equal-mass binaries of arbitrary separation. We constructsequences of constant rest mass and identify the innermost stable circularorbit and its angular velocity. We find that the quasi-equilibrium maximumallowed mass of a neutron star in a close binary is slightly larger than inisolation.Comment: 4 pages, 3 figures, RevTe

Binary Neutron Stars in General Relativity: Quasiequilibrium Models