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We present calculations of quasiequilibrium sequences of irrotational binaryneutron stars based on realistic equations of state (EOS) for the whole neutronstar interior. Three realistic nuclear EOSs of various softness and based ondifferent microscopic models have been joined with a recent realistic EOS ofthe crust, giving in this way three different EOSs of neutron-star interior.Computations of quasiequilibrium sequences are performed within theIsenberg-Wilson-Mathews approximation to general relativity. For allevolutionary sequences, the innermost stable circular orbit (ISCO) is found tobe given by mass-shedding limit (Roche lobe overflow). The EOS dependence onthe last orbits is found to be quite important: for two 1.35 M_sol neutronstars, the gravitational wave frequency at the ISCO (which marks the end of theinspiral phase) ranges from 800 Hz to 1200 Hz, depending upon the EOS. Detailedcomparisons with 3rd order post-Newtonian results for point-mass binariesreveals a very good agreement until hydrodynamical effects (dominated byhigh-order functions of frequency) become important, which occurs at afrequency ranging from 500 Hz to 1050 Hz, depending upon the EOS.Comment: 11 pages, 10 EPS figures, minor revisions, accepted for publication  in A&

Impact of the nuclear equation of state on the last orbits of binary neutron stars