Abstract
In this work, we deal with collimated outflows of magnetized astrophysical plasma known as astrophysical jets, which have been observed to emerge from a wide variety of astrophysical compact objects. The latter systems can be considered as either hydrodynamic (HD) or magnetohydrodynamic (MHD) in nature, which means that they are governed by non-linear partial differential equations. In some of these systems, the velocity of the jet is very high and they require relativistic MHD (RMHD) treatment. We mainly focus on the appropriate numerical solutions of the MHD (and/or RMHD) equations as well as the transfer equation inside the jet and simulate multi-messenger emissions from specific astrophysical compact objects. We use a steady state axisymmetric model assuming relativistic magnetohydrodynamic descriptions for the jets (astrophysical plasma outflows) and perform numerical simulations for neutrino, gamma-ray and secondary particle emissions. By adopting the existence of such jets in black hole microquasars (and also in AGNs), the spherical symmetry of emissions is no longer valid, i.e., it is broken, and the system needs to be studied accordingly. One of the main goals is to estimate particle collision rates and particle energy distributions inside the jet, from black-hole microquasars. As concrete examples, we choose the Galactic Cygnus X-1 and the extragalactic LMC X-1 systems.
Highlights
The last decades, collimated plasma outflows have been observed to emerge from a wide variety of astrophysical objects
The inflow into the accretion disc and the outflow in the jet motivate the investigation of the disc–jet connection [8] in the latter systems
The X-ray binary systems (XRBs) and the microquasars (MQ) along with their astrophysical magnetohydrodynamical outflows have aroused great interest among the researches dealing with the mechanisms of production and emission of high-energy particles and/or photons (X-rays, gamma-rays, etc.) from such cosmic structures
Summary
The last decades, collimated plasma outflows have been observed to emerge from a wide variety of astrophysical objects These include the proto-planetary nebulae, the compact objects (like galactic black holes or microquasars and X-ray binary stars), as well as the nuclei of active galaxies (AGNs) [1,2]. The X-ray binary systems (XRBs) and the microquasars (MQ) along with their astrophysical magnetohydrodynamical outflows have aroused great interest among the researches dealing with the mechanisms of production and emission of high-energy particles (mostly neutrinos) and/or photons (X-rays, gamma-rays, etc.) from such cosmic structures. This is not restricted only in the analysis of the very large amount of observations [3–5,12]. For the detection of such emissions, extremely sensitive detector facilities, like the IceCube (at the South pole), the ANTARES and KM3NeT (at the Mediterranean Sea), etc., are in operation to record the relevant signals reaching the Earth [34,35]
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