Deconfinement phase transition in relativistic neutron star mergers

We consider the influence of the deconfinement phase transition on gravitational waves (GW) emitted in a binary neutron star merger. We perform 3D hydrodynamic simulations based on the conformally flat approximation to general relativity and the GW signal extracted Lip to quadrupole order. We vary the initial constituent masses of the binary by use of physically-motivated equations of state (EoS) at zero temperature in two ways - allowing stellar matter to undergo or not the hadron-quark phase transition. It has been shown, that for a binary system close to the innermost stable circular orbit (ISCO) with constituent gravitational masses larger than M-infinity similar or equal to 1.5 M-circle dot the EoS dependent effects in GW signals begin to play a role. The difference in the gravitational wave frequency at the ISCO is to up to similar or equal to 1.0% for the maximal allowed mass given by the used model EsoS - M-infinity similar or equal to 1.75 M-circle dot. We determine the characteristic GW frequencies of the merger remnants, where the pronounced implications of quark matter show up as a phase difference in the post-merger GW signal, for stellar matter undergoing or not the deconfinement phase transition and collapse does not take place immediately after merger.