  We report on numerical results from an independent formalism to describe the
quasi-equilibrium structure of nonsynchronous binary neutron stars in general
relativity. This is an important independent test of controversial numerical
hydrodynamic simulations which suggested that nonsynchronous neutron stars in a
close binary can experience compression and even collapse prior to the last
stable circular orbit. We show that the interior density indeed increases as
irrotational binary neutron stars approach their last orbits for particular
values of the compaction ratio. The observed compression is however at a
significantly reduced level.
