Simulations of neutrino and gamma-ray production from relativistic black-hole microquasar jets. (arXiv:2011.12939v1 [hep-ph] CROSS LISTED)
<a href="http://arxiv.org/find/hep-ph/1/au:+Papavasileiou_T/0/1/0/all/0/1">Th. V. Papavasileiou</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kosmas_O/0/1/0/all/0/1">O. T. Kosmas</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sinatkas_J/0/1/0/all/0/1">J. Sinatkas</a>
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 their hadronic content in their jets. Such emissions are
reliably described within the context of the relativistic
magneto-hydrodynamics. Our model calculations are based on the Fermi
acceleration mechanism through which the primary particles (mainly protons) 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, $eta$-particles, etc.) are created as well as electromagnetic radiation
from the radio wavelength band, to X-rays and even to very high energy
$gamma$-ray emission. 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 distributions within hadronic astrophysical jets. After testing our
method 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 few
years ago.
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 their hadronic content in their jets. Such emissions are
reliably described within the context of the relativistic
magneto-hydrodynamics. Our model calculations are based on the Fermi
acceleration mechanism through which the primary particles (mainly protons) 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, $eta$-particles, etc.) are created as well as electromagnetic radiation
from the radio wavelength band, to X-rays and even to very high energy
$gamma$-ray emission. 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 distributions within hadronic astrophysical jets. After testing our
method 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 few
years ago.
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