  To study binary neutron star systems and to interpret observational data such
as gravitational-wave and kilonova signals, one needs an accurate description
of the processes that take place during the final stages of the coalescence,
e.g., through numerical-relativity simulations. In this work, we present an
updated version of the numerical-relativity code BAM in order to incorporate
nuclear-theory based Equations of State and a simple description of neutrino
interactions through a Neutrino Leakage Scheme. Different test simulations, for
stars undergoing a neutrino-induced gravitational collapse and for binary
neutron stars systems, validate our new implementation. For the binary neutron
stars systems, we show that we can evolve stably and accurately distinct
microphysical models employing the different equations of state: SFHo, DD2, and
the hyperonic BHB$\Lambda \phi$. Overall, our test simulations have good
agreement with those reported in the literature.
