  We present calculations of quasiequilibrium sequences of irrotational binary
neutron stars based on realistic equations of state (EOS) for the whole neutron
star interior. Three realistic nuclear EOSs of various softness and based on
different microscopic models have been joined with a recent realistic EOS of
the crust, giving in this way three different EOSs of neutron-star interior.
Computations of quasiequilibrium sequences are performed within the
Isenberg-Wilson-Mathews approximation to general relativity. For all
evolutionary sequences, the innermost stable circular orbit (ISCO) is found to
be given by mass-shedding limit (Roche lobe overflow). The EOS dependence on
the last orbits is found to be quite important: for two 1.35 M_sol neutron
stars, the gravitational wave frequency at the ISCO (which marks the end of the
inspiral phase) ranges from 800 Hz to 1200 Hz, depending upon the EOS. Detailed
comparisons with 3rd order post-Newtonian results for point-mass binaries
reveals a very good agreement until hydrodynamical effects (dominated by
high-order functions of frequency) become important, which occurs at a
frequency ranging from 500 Hz to 1050 Hz, depending upon the EOS.
