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

Incorporating a radiative hydrodynamics scheme in the numerical-relativity code BAM