Binary neutron star initial data and single, rotating neutron stars as gravitational wave emitters

In the first part of this talk, we compare gravitational waveforms for the same irrotational binary configuration computed with two different initial-data codes, but evolved with the same evolution code. The impact of the difference on the estimation of physical parameters will be addressed. In the second part we present quasiequilibrium solutions of triaxially deformed rotating compact stars (generalization of Jacobi ellipsoids under relativistic gravity and compressible equations of state). We show that supramassive equilibrium solutions exist and a new scenario to probe the EOS of high density nuclear matter through gravitational wave detection will be discussed.