  In this work, we simulate $\gamma$-rays created in the hadronic jets of the
compact object in binary stellar systems known as microquasars. We utilize as
main computational tool the $3$-D relativistic magneto-hydro-dynamical code
PLUTO combined with in house derived codes. Our simulated experiments refer to
the SS433 X-ray binary, a stellar system in which hadronic jets have been
observed. We examine two new model configurations that employ hadron-based
emission mechanisms. The simulations aim to explore the dependence of the
$\gamma$-ray emissions on the dynamical as well as the radiative properties of
the jet (hydrodynamic parameters of the mass-flow density, gas-pressure,
temperature of the ejected matter, high energy proton population inside the jet
plasma, etc.). The results of the two new scenarios of initial conditions for
the micro-quasar stellar system studied, are compared to those of previously
considered scenarios.
