  We perform binary neutron star merger simulations using a newly derived set
of finite-temperature equations of state in the Brueckner-Hartree-Fock
approach. We point out the important and opposite roles of finite temperature
and rotation for stellar stability and systematically investigate the
gravitational-wave properties, matter distribution, and ejecta properties in
the postmerger phase for the different cases. The validity of several universal
relations is also examined and the most suitable EOSs are identified.
