Abstract
In this work, after improving 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 γ -rays originated from the extragalactic M33 X-7 system, which is an X-ray binary discovered in 2006, located in the neighboring galaxy Messier 33, and has not yet been modeled in detail. The particle and radiation energy distributions, produced from magnetized hadronic 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 integrodifferential transport equations of multiparticle processes (reactions chain) following the inelastic proton-proton (p-p) collisions. For the detection of such high-energy neutrinos as well as multiwavelength (radio, X-ray, and gamma-ray) emissions, extremely sensitive space telescopes and other γ -ray and neutrino detection instruments are in operation or have been designed like the CTA, IceCube, ANTARES, KM3NeT, and IceCube-Gen-2.
Highlights
During the last few decades, collimated astrophysical outflows have been observed to emerge from a wide variety of galactic and extragalactic compact structures Mirabel_ Rodriguez_1999, Romero_Torres_et_al_2003, Reynoso08, Reynoso09, RomeroReview
We focus on the magnetized astrophysical outflows that are characterized by hadronic content (p, π±, light nuclei, etc.) in their jets
The number of protons appears reduced for the wide halfopening angle system of M33 X-7 (ξ = 7∘) as compared to the narrow of SS 433 (ξ = 0:6∘). This is because the jet radius rðzÞ is bigger and the magnetic field B is smaller in the case of M33 X-7 than that of SS 433
Summary
During the last few decades, collimated astrophysical outflows have been observed to emerge from a wide variety of galactic and extragalactic compact structures Mirabel_ Rodriguez_1999, Romero_Torres_et_al_2003, Reynoso, Reynoso, RomeroReview. One of the purposes of this work is to attempt, for a first time, to formulate in a compact way this differential system of transport equations (satisfied by the primary protons and the secondary multiparticles, multispecies) and derive advantageous algorithms [28] to perform the required simulations for persistent emissions (transient episodes or flares are ignored [6]) emanating from the hadronic component of the MQ jets These calculations are based on the particle distributions extracted from the solutions of the time-independent (steady-state approximation) system of integrodifferential transport equations mentioned above [29,30,31,32].
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