General Relativistic Simulations of Binary Neutron Star Mergers

          @misc{ scivideos_PIRSA:10060084,
            doi = {10.48660/10060084},
            url = {https://pirsa.org/10060084},
            author = {Giacomazzo, Bruno},
            keywords = {},
            language = {en},
            title = {General Relativistic Simulations of Binary Neutron Star Mergers},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2010},
            month = {jun},
            note = {PIRSA:10060084 see, \url{https://scivideos.org/index.php/pirsa/10060084}}
          }
          

Abstract

I will report on some recent results obtained using the fully general relativistic magnetohydrodynamic code Whisky in simulating equal and unequal-mass binary neutron star (BNS) systems during the last phases of inspiral, merger and collapse to black hole surrounded by a torus. BNSs are among the most important sources of gravitational waves which are expected to be detected by the current or next generation of gravitational wave detectors, such as LIGO and Virgo, and they are also thought to be at the origin of very important astrophysical phenomena, such as short gamma-ray bursts. I will in particular describe both the gravitational wave signals generated by these sources and the properties of the tori that can be formed. I will also describe how the Effective One Body (EOB) model can be used to accurately compute the gravitational wave signal generated during the inspiral of BNSs by comparing it with the longest general relativistic numerical simulations of BNSs performed up to now.