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By means of HARM\_COOL\_EOS, which is our code for conservative relativisticmagnetohydrodynamics, we developed a new scheme for the simulation of a systemformed after compact binary merger. Our code works with a tabulated equation ofstate of dense matter, accounts for the neutrino leakage, and follows the massoutflows via the tracer particle method. We discuss the numerical scheme, andpresent the recovery method included in our code. We also show results of anumerical simulation, addressed to the post-merger system after the coalescenceof binary neutron stars, or a neutron star with a stellar mass black hole. Theplasma is very neutron-rich, so the r-process nucleosynthesis in the ejectedmaterial may lead to unstable heavy isotopes creation. They are responsible foran electromagnetic signal, observed as a kilonova. In addition, the magnetized,neutrino-driven wind can act as a collimating mechanism for the relativisticjet.

Numerical GR MHD simulations of the post-merger system with a composition-dependent equation of state