Modeling particle transport in astrophysical outflows and simulations of associated emissions

In this work, after making an attempt to improve the formulation of the model on particle transport within astrophysical plasma outflows and constructing the appropriate algorithms, we test the reliability and effectiveness of our method through numerical simulations on well-studied Galactic microquasars as the SS 433 and the Cyg X-1 systems. Then, we concentrate on predictions of the associated emissions, focusing on detectable high energy neutrinos and \(\gamma\)-rays originated from the extra-galactic M33 X-7 system, which is a recently discovered X-ray binary located in the neighboring galaxy Messier 33 and has not yet been modeled in detail. The particle and radiation energy distributions, produced from magnetized astrophysical jets in the context of our method, are assumed to originate from decay and scattering processes taking place among the secondary particles created when hot (relativistic) protons of the jet scatter on thermal (cold) ones (p-p interaction mechanism inside the jet). These distributions are computed by solving the system of coupled integro-differential transport equations of multi-particle processes (reactions chain) following the inelastic proton-proton (p-p) collisions. For the detection of such high energy neutrinos as well as multi-wavelength (radio, X-ray and gamma-ray) emissions, extremely sensitive detection instruments are in operation or have been designed like the CTA, IceCube, ANTARES, KM3NeT, IceCube-Gen-2, and other space telescopes.