Thermal effects of the nuclear equation of state on binary neutron star mergers

Binary neutron star merger calculations often rely on a zero-temperature approximation to the equation of state. While this approximation holds well during the inspiral phase, it breaks down during the merger. Using the numerical relativity code THC_M1, we study thermal effects in binary neutron star mergers using full microphysical equations of state which differ only by their finite-temperature behavior. We present preliminary results, including gravitational waveforms and an ejecta analysis, and highlight potential observational consequences.