Threshold mass of prompt collapse for binary quark stars
Zhou, Enping
The multi-messenger observations of binary merger events have provided us unprecedented opportunities to study the state of matter under extreme conditions, such as those inside neutron stars. For instance, depending on the total mass of the merging binary, the post-merger remnant could undergo collapse to black hole at different timescales, producing very different gravitational wave and electromagnetic signals. The post-merger evolution scenarios have been extensively explored for binary neutron star mergers by numerical relativity simulations and the ways of constraining neutron star EoS via multi-messenger observations have been suggested accordingly. In my talk, I will introduce our modifications to the numerical relativity code SACRA-MPI which allows us to perform full GR-hydrodynamic simulations for mergers of binary bare quark stars (i.e., without crusts and with finite surface density) for the first time. The results of threshold mass for prompt collapse of a binary quark star merger will be demonstrated and its difference with binary neutron star case will be discussed.