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Relativistic Magnetized Astrophysical Plasma Outflows in Black-Hole Microquasars

Department of Informatics, University of Western Macedonia, GR-52100 Kastoria, Greece
Department of MACE, University of Manchester, George Begg Building, Manchester M1 3BB, UK
Author to whom correspondence should be addressed.
Symmetry 2022, 14(3), 485;
Received: 12 November 2021 / Revised: 16 December 2021 / Accepted: 17 December 2021 / Published: 27 February 2022
(This article belongs to the Special Issue The Nuclear Physics of Neutron Stars)


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the existence of such jets in black hole microquasars (and also in AGNs), the spherical symmetry of emissions is no longer valid, i.e., it is broken, and the system needs to be studied accordingly.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.

1. Introduction

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]. Despite their different scales concerning the size, the velocity, the amount of energy transported, etc., these cosmic structures have strong similarities. The observations of multi-wavelength and multi-particle emissions from the black-hole X-ray binaries (BHXRBs) [3,4,5] and the AGNs have shown that they are mainly due to the mass accretion onto the compact object (black hole or neutron star). The accreted matter comes from a companion (donor) star which is often a nearby main sequence star [6,7]. Thus, the inflow (from the companion star) into the accretion disc and the outflow in the jet motivate the investigation of the disc–jet connection [8] in the latter systems. They are governed by non-linear partial differential equations that must be solved through the use of advanced numerical techniques [9,10,11].
Recently, 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 [3,4,5,12] compared to emissions of smaller energy ranges but also in their advanced theoretical modeling [9,10,11,13,14]. Up to now, multidimensional numerical simulations and theoretical calculations have attempted to shed light on the nature of the interaction mechanisms as well as on the dynamics involved in the associated emissions [7,11]. They offer good support for experimental efforts of astrophysical particles and radiation detection (for more details the reader is referred to References [13,15]).
From an astronomy and astrophysics viewpoint, XRBs are binary systems consisted of a compact object (mostly stellar black hole or neutron star) and a donor star in rotational trajectory around the central star. Due to the presence of very high gravitational field around the compact object, mass is absorbed out of the companion star. The result is the creation of a rotating accretion disc of very high temperature matter and gas along the equatorial plane of the compact object. Subsequently, the magnetic field lines created by the rotating charged matter of the disc, collimate the ejected plasma. This way two oppositely directed astrophysical jets are formed [16]. From a magnetohydrodynamical point of view, the jets (astrophysical plasma outflows) are considered as fluid flows emanating from the region of the compact object. Then, they may be strongly accelerated within a cone of radius r ( z ) dependent on its half-opening angle ξ ( r = z t a n ξ ). It is worth noting that, in some systems (e.g., the M87 and some AGNs) the consideration of a parabolic jet is geometrically more realistic. For example, in describing the jet acceleration, the parabolic shape favors the region near the jet’s base. In the conical geometry, however, assumed in this work the acceleration region is put at greater distances from the base.
The plasma ejection is closely connected with the accretion disc formation and its thickness as well as the jet creation mechanisms. Ideally, spherical symmetry would be well suited to describe thin accretion-disc plasma outflows. Initially, prominent theoretical models have been developed by assuming isotropic emissions from the jets (in such models solution through analytic calculations are possible). Realistically (even under slow black-hole rotation and small-scale magnetic fields) there are rather strong deviations from a perfectly symmetrical geometry. In addition, the formation of two oppositely directed jets destroys the spherical symmetry of many systems which become mostly axisymmetric (around the z-axis, the jet-ejection axis). That is why in various types of microquasars (and AGNs) the statistical analysis was made on the basis of the jet’s orientation. Moreover, astrophysical jets are often observed to be one-sided and associated with a Doppler factor that confirms the existence of bulk relativistic motion inside the jet. Recently, with the development of advanced efficient computational tools, the employment of more realistic, anisotropic emission (non-symmetric) models became possible. A prominent example would be the relativistic hydrocode PLUTO implemented in References [9,10,11,17].
For the purposes of our present study, we adopt a lepto-hadronic model for neutrino and gamma-ray production [18,19,20]. Therefore, we consider that the jet’s matter consists mainly of hadrons and electrons (their portion is determined by defining the ratio α of protons to leptons) that are strongly collimated by the system’s magnetic field. Furthermore, we assume that a portion of the main jet’s content (electrons and protons) [21] is accelerated to rather relativistic velocities through shock-waves [22,23,24,25]. A power-law is best suited to describe the energy distribution of the fast protons N ( E ) , which in the jet’s rest frame, is given by the expression:
N ( E ) = K 0 E 2 G e V 1 c m 3 ,
where K 0 is a normalization constant. The accelerated fast protons scatter with the cold protons of the jet or the protons of the stellar wind [26,27,28]. They can also scatter with the radiation fields (gamma-rays) emanating from sources inside or outside the jet. The result is high-energy secondary particles (pions, muons, neutrinos, etc.) production as well as secondary gamma-ray photons emission through various reaction chains [18,19,29].
In this work, initially, we discuss some of the possible interactions resulting in secondary particle and radiation production. In our previous works, we have addressed the proton-proton (p-p) mechanism and estimated the respective energy distributions as well as the emissivities of neutrino and gamma-ray emissions [7,30,31]. In the current study, we concentrate on the proton-photon (p- γ ) interaction mechanism and its dependence on geometric characteristics of the binary systems of our interest. These include the Galactic Cygnus X-1 microquasar [32] and the extragalactic LMC X-1 system [33] located at the neighboring galaxy of the Large Magellanic Cloud. 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].

2. Radiation Field Density and Transport Equation in Microquasar Jets

The radiation fields that interact with the accelerated (fast) protons of the jet, may consist of soft X-ray photons emanating from the system’s accretion disc. They could also include synchrotron radiation emitted by the charged particles (accelerated by the magnetic field inside the jet), or ultra violet (UV) photons originated from the corona region [18,19,36]. In the context of this study, we will take into account the first two cases that are involved in p- γ collisions leading to a reaction chain producing neutrinos and gamma-rays of high energies. We note that UV photons do not contribute significantly to the energy range of our interest.

2.1. Microquasar Jet Mechanisms Leading to Neutrino and Gamma-Ray Production

In our previous works [7,9], we have adopted the proton-proton (p-p) interaction mechanism taking place inside the relativistic astrophysical outflows of microquasar jets. This also leads to the particle (pions, muons, neutrinos, etc.) production and radiation emission (gamma-rays, etc.) (see Ref. [7]). Such emissions present axial symmetry around the jet’s ejection z-axis. In Refs. [10,11], the employed PLUTO hydro-code permits emission calculations without the assumption of axial symmetry which are considered more realistic jet emission simulations. In this paper, however, we focus on the proton-photon (p- γ ) interactions described below.
The p- γ mechanism reflects the collisions of the relativistic protons with the photons of the radiation fields discussed before. This results in the known photo-pion production shortly represented by the following scattering and/or decay reactions:
p + γ p + π 0 p + γ p + π 0 + π + + π p + γ n + π + .
The above pions ( π 0 , π + , π ) decay to gamma-ray photons, charged muons, neutrinos, etc., according to the following reactions:
π 0 γ + γ π + μ + + ν μ e + + ν ¯ μ + ν e + ν μ π μ + ν ¯ μ e + ν ¯ e + ν μ + ν ¯ μ .
In the above reaction chains (2) and (3), gamma-ray photons are emitted through the neutral pions decay. Furthermore, through the subsequent decay of the secondary muons which create electrons e (or positrons e + ), neutrinos or anti-neutrinos are produced too. By implementing the p- γ mechanism, the above reactions constitute the main processes feeding the neutrino and gamma-ray production channels in the lepto-hadronic model employed [18,19].
In general, the radiation density that interacts with the non-thermal (relativistic) protons, is due to mainly two contributing factors. The first is the synchrotron emission, by accelerated charged particles, that create a photon distribution, n p h S (produced by relativistic electrons as well as protons). It is given by [18,19]:
n p h S ( ϵ , z ) ε s y n r ( z ) ϵ c ,
where ε s y n corresponds to the total power radiated by electron and proton distributions and is given in Appendix A.1. The second contributing factor is an X-ray distribution, n p h X (for 2 keV < ϵ < 100 keV ), originated from the corona that surrounds the inner accretion disc. For the latter distribution, we have [19,36]:
n p h X ( ϵ , z ) = L X e ϵ / k T e 4 π c z 2 ϵ 2 ,
where X-ray luminosity is L X = 10 36 ergs 1 and k T e 30 keV.
Furthermore, within our approximation it holds n p h = n p h X + n p h S . It should be noted that, the primary particles (protons, electrons) as well as the secondary particles take part also in energy loss interactions and processes. These include the energy losses due to jet adiabatic expansion, the losses due to inelastic collisions with the cold protons and losses due to the emission of synchrotron radiation [30,31,37].
Concerning the fast (non-thermal or relativistic) proton distribution, its shape in the one-zone approximation, resembles to a power-law type (defined by a normalization constant K 0 ) [38] assumed in our model (see Equation (1)).

2.2. Solution of the Transfer Equation

In the lepto-hadronic model employed in the present work, the acceleration mechanism (it is not included in the transport equation) is used to fix the injection function of the primary electrons and protons. Then, it determines the maximum energies that can be acquired by the relativistic particles inside the jet. To this aim, the particle transfer (transport) equation must be solved which, assuming a steady-state model, is written as [9,10,11]:
N ( E , z ) b ( E , z ) E + t 1 N ( E , z ) = Q ( E , z ) .
N ( E , z ) represents the particle density per unit of energy ( cm 3 GeV 1 ) and Q ( E , z ) denotes the particle source function (in units of cm 3 GeV 1 s 1 ). Obviously, this is not a spherical but an axisymmetric model, hence the particle distributions and injection functions depend on z (i.e., the distance to the central object on the ejection-axis of the jet). In the latter equation, b ( E ) stands for the total energy loss rate given by:
b ( E ) = d E d t = E t l o s s 1 ,
while t 1 represents the particles’ reduction rate as:
t 1 = t e s c 1 + t d e c 1 .
Here, t d e c 1 is the decay rate (in the case of pions and muons) and t e s c 1 the escape rate of the particles from the jet’s region. The latter rate is given by:
t e s c 1 = c z m a x z 0 ,
with ( z m a x z 0 ) being the length of the acceleration zone inside the jet.
The solution of the differential Equation (6) is written as:
N ( E , z ) = 1 b ( E ) E E m a x Q ( E , z ) e τ ( E , E ) d E ,
where the maximum proton energy is approximated by E p m a x 10 7 GeV, while:
τ ( E , E ) = E E d E t 1 b ( E ) .
The source function Q ( E , z ) , for the relativistic particles (in the jet’s rest frame) is given by [19]:
Q ( E , z ) = Q 0 z 0 z 3 E 2 .
In the observer’s reference frame, Q ( E , z ) takes the form given in the Appendix (see Equation (A8) of Appendix A.2) where the normalization constant Q 0 of Equation (12) is also given in the Appendix A.

3. Interaction Frequency and Particle Emission through p- γ Mechanism

The injection function for the pions produced through the p- γ interaction mechanism is the following:
Q π ( p γ ) ( E , z ) = 5 N p ( 5 E , z ) ω p γ ( 5 E , z ) N ¯ π ( p γ ) ( 5 E ) ,
where N p ( E , z ) denotes the proton energy distribution. Furthermore, ω p γ is the p- γ collision frequency that results in pion production. The mean number N ¯ π ( p γ ) of positive or negative pions produced per p- γ collision is given by:
N ¯ π ( p γ ) = p p n p 1 + 2 p 2 ,
where the parameter p p n 0.5 is to express the probability of conversion of a primary proton to a neutron. Furthermore, p 1 and p 2 are defined as:
p 1 = K 2 K ¯ p γ K 2 K 1 ,
and p 2 = 1 p 1 . Moreover, we have K 1 = 0.2 and K 2 = 0.6 . In the latter equation, for the mean inelasticity parameter K ¯ p γ it holds:
K ¯ p γ = t p γ 1 ω p γ .
The p- γ collision frequency ω p γ in Equations (13) and (16) is given by [19,39]:
ω p γ ( E p , z ) = c 2 γ p 2 ϵ t h / 2 γ p n p h ( ϵ , z ) ϵ 2 d ϵ ϵ t h 2 ϵ γ p σ p γ ( π ) ( ϵ ) ϵ d ϵ ,
where γ p = E p / m p c 2 , n p h ( ϵ , z ) is the radiation field density that was discussed in Section 2. The threshold energy ϵ t h is assumed to be ϵ t h = 0.15 GeV [39].
After the above definitions, the respective cross-section σ p γ ( π ) is given by [39,40]:
σ p γ ( π ) = [ 3.4 Θ ( ϵ 0.2 ) Θ ( 0.5 ϵ ) + 1.2 Θ ( ϵ 0.5 ) ] × 10 28 c m 2 ,
where Θ ( x ) denotes the well-known step function. In the latter relationships, the proton-photon collision rate t p γ 1 was obtained from the expression [39]:
t p γ 1 = c 2 γ p 2 ϵ t h / 2 γ p n p h ( ϵ , z ) ϵ 2 d ϵ ϵ t h 2 ϵ γ p σ p γ ( π ) ( ϵ ) K p γ ( π ) ( ϵ ) ϵ d ϵ .
In the above expression, K p γ ( π ) ( ϵ ) is the respective inelasticity function [39,40] which is equal to:
K p γ ( π ) ( ϵ ) = 0.2 Θ ( ϵ 0.2 ) Θ ( 0.5 ϵ ) + 0.6 Θ ( ϵ 0.5 ) .

4. Results and Discussion

In the context of the model chosen in this study, at first the p- γ collision rate t p γ 1 of Equation (19) was calculated for the X-ray binary systems Cygnus X-1 and LMC X-1. The geometric properties and other parameters of these systems are listed in Table 1. The results obtained for the t p γ 1 in the latter microquasars are presented in Figure 1. In the upper two sub-figures, we illustrate the interaction rate as a function of the proton energy E for three different distances of the studied point up to the system’s central object (z). The range of z covers the length of the acceleration zone (from z 0 to z m a x = 5 z 0 ). It is supported by theoretical calculations that, for greater distances, the p- γ collision rate decreases. The reason is the dependence of X-ray photon density (see Equation (5)) as well as the fast particle density on z. It is reasonable that as the jet expands (e.g., its radius increases), the mean-free path of the particles and photons involved in the collisions increases as well. That leads to reduced collision rates.
In the lower two sub-figures of Figure 1, we illustrate the p- γ collision rate for three different values of the half-opening angle ξ of the jet. This angle strongly depends on the magnetic field strength and characterizes the jet’s collimation. The values of ξ considered are representative and cover the assumed range extended up to 10 . We notice that the collision rate decreases as the jet expands perpendicularly to its ejection axis (i.e., for greater angles). This is validated by the corresponding theoretical expressions if we consider the decrease of the synchrotron emission which is due to the magnetic field that controls the jet’s collimation. In addition, the mean-free path of the proton-photon collisions increases causing the reduction of the respective rate.
We have, also, calculated the pion energy distributions for different typical values of the angle ( θ ) between the jet axis and the direction of the line of sight as well as the bulk velocity of the jet’s matter ( u b ) for the Cygnus X-1 binary system, see Figure 2. It is evident that the particle production is higher for smaller values of θ as demonstrated in Equation (A8) in the Appendix A.2. Furthermore, the particle production increases for greater bulk velocities u b (i.e., it is u b = β j c where c corresponds to the speed of light constant) as shown in sub-figure (b) of Figure 2. This result is justified by considering the relation of bulk velocity to the jet’s collimation and the proton-photon interaction rate which increases for larger energies. It is hoped that, our present results would be helpful for future relevant experimental and observational measurements.
In this work, we, furthermore study the pion distributions produced by p- γ interactions for three different values of the parameter α defined as:
α = L h L e .
L h and L e denote the hadronic and leptonic luminosity, respectively. These values correspond to: (i) a leptonic model ( α = 0.001 ), (ii) a hadronic model ( α = 100 ) and (iii) an extreme-hadronic model ( α = 1000 ). The results are shown in Figure 3. Our main purpose, here, is the comparison between the particle (pions) production in these well-implemented models (leptonic and hadronic). For that reason, we have not considered the possible energy losses that the aforementioned particles are subjected through the various mechanisms [30,31]. In Figure 3, we notice the reasonable decrease in pion production in the leptonic case as the protons are reduced compared to electrons inside the jet. However, as can be seen, there is no essential difference between the hadronic and the extreme-hadronic model, therefore, a ratio of α 100 is deemed sufficient enough.

5. Summary and Conclusions

Astrophysical binary systems, consisted of a high-mass compact object (black hole or neutron star) that absorbs mass out of a companion star (forming a rotating accretion disc) are studied extensively in recent years. More specifically, their magnetohydrodynamical astrophysical flow ejection and high-energy radiation as well as particle emissions have been the research subject of many authors working in this field. In our present work, we go beyond the spherically symmetric models of neutrino and gamma-ray emissions and adopt conical jets, i.e., axially symmetric plasma outflows from microquasar jets.
We, furthermore, assume that strong shock-waves accelerate a portion of the jets’ charged particles (mostly protons but also electrons) to rather relativistic energies obeying a power-law energy-dependent distribution. Under the above circumstances, these particles interact with thermal protons of the jet (or of stellar winds) or with the radiation fields originating from energy-exchanging mechanisms (i.e., between electrons and low-energy photons) inside or outside the jet’s region. The outcomes of these interactions are secondary particles and photons such as pions, muons, neutrinos, gamma-ray photons, etc. The multi-messenger signals created this way are detectable by the terrestrial extremely sensitive detectors like the IceCube, ANTARES, KM3NeT, etc.
In our study, we mainly focus on the p- γ interaction mechanism (which was not taken explicitly into account in our previous works) and the parameters (e.g., geometric characteristics of the binary systems, the jet’s matter composition of leptons or hadrons, etc.) which affect the associated emissions of particle and radiation. In particular, we have selected two concrete examples, the Galactic Cygnus X-1 and the extragalactic LMC X-1 binary systems, to study with the model chosen and present numerical calculations for the collision rates and energy distributions of particles that come out (pions). Our results show that the particle density production strongly increases in more collimated flow ejections which is highly dependent on the prevailing magnetic field. In addition, we find that the smaller the distance z from the central region the larger the production of particles and radiation is emitted.

Author Contributions

Conceptualization, O.K. and I.S.; methodology, O.K.; software, T.P.; validation, O.K. and I.S.; formal analysis, T.P.; investigation, T.P. and O.K.; writing—original draft preparation, T.P. and O.K.; writing—review and editing, O.K. and I.S.; visualization, T.P. and O.K.; supervision, O.K. and I.S.; project administration, O.K. and I.S. All authors have read and agreed to the published version of the manuscript.


This research was funded in the context of the PhD dissertation of T.P. by the Department of Informatics, School of Sciences of University of Western Macedonia.

Institutional Review Board Statement

Not applicable.

Informed Consent Statement

Not applicable.

Data Availability Statement

There is no data used in this paper.

Conflicts of Interest

The authors declare no conflict of interest.

Appendix A

Appendix A.1. Synchrotron Power Radiation by Particle Distributions

When a charged particle of energy E is being accelerated by a magnetic field with pitch angle a, it emits synchrotron radiation. The power of the radiation per units of the emitted photons’ energy and pitch angle a is given by [37]
P s y n ( ϵ , E , z , α ) = 3 e 3 B ( z ) s i n ( a ) h m c 2 ϵ E c r ϵ E c r K 5 / 3 ( ζ ) d ζ ,
where B ( z ) is the binary system’s magnetic field responsible for the jet’s collimation. e is the electric charge, h denotes the Planck constant and E c r corresponds to the critical frequency of the emitted radiation which is written as
E c r = 3 h e B ( z ) s i n ( a ) 4 π m c γ 2 .
In Equation (A1), we integrate over the modified Bessel function of order 5/3 which we calculate through the following relationships
K 1 3 ( ζ ) = 3 0 e x p ζ 1 + 4 x 2 3 1 + x 2 3 d x
K 2 3 ( ζ ) = 1 3 0 3 + 2 x 2 1 + x 2 3 e x p ζ 1 + 4 x 2 3 1 + x 2 3 d x
K 5 3 ( ζ ) = K 1 3 ( ζ ) + 4 3 ζ K 2 3 ( ζ ) .
After calculating P s y n , we integrate over the pitch angle a as well as the particle energy distribution in order to obtain the total power radiated per unit energy by a particle (electron or proton) distribution such as those we discussed before. The result for electron or proton distributions is given below
ε s y n ( e , p ) ( ϵ ) = d Ω α E e , p ( m i n ) E e , p ( m a x ) P s y n N e , p ( E , z ) d E ,
where E p m i n = 1.2 GeV and E e m i n = 0.001 GeV are the minimum proton and electron energies, respectively. For the maximum energies, we have E p m a x 10 7 GeV and E e m a x 7 GeV.
The total power radiated by both electrons and protons is given by
ε s y n ( ϵ ) = ε s y n ( e ) ( ϵ ) + ε s y n ( p ) ( ϵ ) .

Appendix A.2. Injection Function in Observer’s Reference Frame

The transformation of the proton injection function to the observer’s reference frame is given by [10,11,44]
Q ( E , z ) = Q 0 z 0 z 3 Γ b 1 ( E β b c o s θ E 2 m 2 c 4 ) 2 s i n 2 θ + Γ b 2 c o s θ β b E E 2 m 2 c 4 2 .
Here, Γ b is the Lorentz factor responding to the jet’s bulk velocity ( u b = β b c and Γ b = ( 1 β b 2 ) 1 2 ) and Q 0 is given by
Q 0 = 8 q r L k z 0 r 0 2 l n ( E p m a x / E p m i n ) ,
where r 0 is the jet radius that corresponds to the distance z 0 from the central object. Moreover, the kinetic luminosity that is transferred in the jet L k is considered to be 10% of the central object’s Eddington luminosity [8]. We, also, adopt the value q r = 0.1 for the portion of relativistic protons and electrons inside the jet.


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Figure 1. Proton-photon (p- γ ) interaction rate t p γ 1 as a function of proton energy E for the binary systems Cygnus X-1 (left column) and LMC X-1 (right column). In the upper two sub-figures (a,b), we show the p- γ interaction rate for three different values of the distance z (in factors of z 0 ) inside the jet from the compact object. In the lower two sub-figures (c,d), we plot the t p γ 1 for three different values of the jet’s half-opening angle ξ .
Figure 1. Proton-photon (p- γ ) interaction rate t p γ 1 as a function of proton energy E for the binary systems Cygnus X-1 (left column) and LMC X-1 (right column). In the upper two sub-figures (a,b), we show the p- γ interaction rate for three different values of the distance z (in factors of z 0 ) inside the jet from the compact object. In the lower two sub-figures (c,d), we plot the t p γ 1 for three different values of the jet’s half-opening angle ξ .
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Figure 2. For Cygnus X-1, we present pion distributions for different values of the system’s angle to the line of sight (a) and bulk velocity of the jet’s ejected matter (b). The pions in this case have not been subjected to energy loss mechanisms.
Figure 2. For Cygnus X-1, we present pion distributions for different values of the system’s angle to the line of sight (a) and bulk velocity of the jet’s ejected matter (b). The pions in this case have not been subjected to energy loss mechanisms.
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Figure 3. Pion energy distributions from p- γ collisions in the jets of binary systems Cygnus X-1 (a) and LMC X-1 (b) for three different values of hadron-to-lepton ratio α .
Figure 3. Pion energy distributions from p- γ collisions in the jets of binary systems Cygnus X-1 (a) and LMC X-1 (b) for three different values of hadron-to-lepton ratio α .
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Table 1. Model parameters describing geometric characteristics of the Galactic Cygnus X-1 binary system and the extragalactic LMC X-1 located at the Large Magellanic Cloud.
Table 1. Model parameters describing geometric characteristics of the Galactic Cygnus X-1 binary system and the extragalactic LMC X-1 located at the Large Magellanic Cloud.
DescriptionParameterCygnus X-1LMC X-1
Jet’s base z 0 (cm) 191 R S c h 95 R S c h
Acceleration zone limit z m a x (cm) 956 R S c h 477 R S c h
Mass of compact object M B H 14.8 M [41]10.91 M [42]
Angle to the line-of-sight θ ( )27.1 [41]36.38 [42]
Jet’s half-opening angle ξ ( )1.5 [43]3 *
Jet’s bulk velocity υ b 0.6c [43]0.92c *
* Indicative values that we consider for our calculations.
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Papavasileiou, T.; Kosmas, O.; Sinatkas, I. Relativistic Magnetized Astrophysical Plasma Outflows in Black-Hole Microquasars. Symmetry 2022, 14, 485.

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Papavasileiou T, Kosmas O, Sinatkas I. Relativistic Magnetized Astrophysical Plasma Outflows in Black-Hole Microquasars. Symmetry. 2022; 14(3):485.

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Papavasileiou, Theodora, Odysseas Kosmas, and Ioannis Sinatkas. 2022. "Relativistic Magnetized Astrophysical Plasma Outflows in Black-Hole Microquasars" Symmetry 14, no. 3: 485.

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