DEFORMATION OF RAPIDLY ROTATING COMPACT STARS

We have developed a numerical code to study the deformation (epsilon = (I-zz - I-xx)/I-zz where I-ii are the moments of inertia) of neutron stars in rapidly rotation in a fully general relativistic calculation. We have found that the deformation is larger, depending on the angula r velocity, than is generally assumed for gravitational wave estimatio ns. Calculations were performed by employing the Bethe-Johnson I EOS ( equation of state) and a new set of models by the Frankfurt group incl uding Lambda hyperons for several choices of their coupling constants to ordinary nucleons. Possible implications for gravitational wave sea rches are briefly discussed.