Abstract
Recently, microquasar jets have aroused the interest of many researchers focusing on the astrophysical plasma outflows and various jet ejections. In this work, we concentrate on the investigation of electromagnetic radiation and particle emissions from the jets of stellar black hole binary systems characterized by the hadronic content in their jets. Such emissions are reliably described within the context of relativistic magneto-hydrodynamics. Our model calculations are based on the Fermi acceleration mechanism through which the primary particles (mainly protons and electrons) of the jet are accelerated. As a result, a small portion of thermal protons of the jet acquire relativistic energies, through shock-waves generated into the jet plasma. From the inelastic collisions of fast (non-thermal) protons with the thermal (cold) ones, secondary charged and neutral particles (pions, kaons, muons, η-particles, etc.) are created, as well as electromagnetic radiation from the radio wavelength band to X-rays and even very high energy gamma-rays. One of our main goals is, through the appropriate solution of the transport equation and taking into account the various mechanisms that cause energy losses to the particles, to study the secondary particle concentrations within hadronic astrophysical jets. After assessing the suitability and sensitivity of the derived (for this purpose) algorithms on the Galactic MQs SS 433 and Cyg X-1, as a concrete extragalactic binary system, we examine the LMC X-1 located in the Large Magellanic Cloud, a satellite galaxy of our Milky Way Galaxy. It is worth mentioning that, for the companion O star (and its extended nebula structure) of the LMC X-1 system, new observations using spectroscopic data from VLT/UVES have been published a few years ago.
Highlights
In recent years, astrophysical magnetohydrodynamical flows in Galactic, extragalactic microquasars (MQs), and X-ray binary systems (XRBs) have been modelled with the purpose of studying their multi-messenger emissions, for example, neutrinos, gamma-rays, and so forth. [1,2,3]
Microquasars are binary systems consisting of a compact stellar object and a donor star [10]
The most well-studied microquasar systems include the Galactic X-ray binaries SS 433, Cyg X-1, Cyg X-3, and so forth. [20,21,22], while from the extragalactic systems we mention the LMC X-1, LMC X-3 located in the neighbouring galaxy of the Large Magellanic Cloud [23], and the Messier X-7 in the Messier 33 galaxy [24]
Summary
Astrophysical magnetohydrodynamical flows in Galactic, extragalactic microquasars (MQs), and X-ray binary systems (XRBs) have been modelled with the purpose of studying their multi-messenger emissions, for example, neutrinos, gamma-rays, and so forth. [1,2,3]. [20,21,22], while from the extragalactic systems we mention the LMC X-1, LMC X-3 located in the neighbouring galaxy of the Large Magellanic Cloud [23], and the Messier X-7 in the Messier 33 galaxy [24] Their respective relativistic jets are emission sources in various wavelength bands and high-energy neutrinos. It is worth mentioning that, a photon field emanating from the companion star in many X-ray binaries may cause γ-ray absorption of photons with energies in the same range of those emitted from the donor star [29,30,31] This absorption becomes important when the distance from the central object of the gamma-ray production region is of the same order with the binary system’s separation, that is, the distance between the two stellar objects [29,30]. (Section 5), we summarize the main conclusions extracted from the present study
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