Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Kosmas, Odysseas; Smponias, Theodoros

doi:10.1155/2018/9602960

Cited by 17 publications

(29 citation statements)

References 35 publications

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“…Another important cooling mechanism, that depends on the cold proton density inside the jet, is due to inelastic collisions of the accelerated particles with the cold ones. The inelastic cross section for the p-p scattering is given by [7][8][9]42]…”

Section: Interaction Mechanisms Inside the Jetmentioning

confidence: 99%

“…For the detection of such emissions, extremely sensitive detector tools are in operation for recording their signals reaching the Earth like IceCube, ANTARES, KM3NeT [4][5][6], and so forth. Modelling offers good support for future attempts to detect radiative multiwavelength emissions and neutrino emission, while in parallel, several numerical simulations may be performed towards this aim [7][8][9].…”

Section: Introductionmentioning

confidence: 99%

“…For detailed studies of this system based on hadronic modelling of its jets, the reader is referred to the Refs. [7][8][9] and references therein. Radiative transfer calculations may be performed at every point inside the jet for a range of frequencies (energies), at every location [27] providing the relevant emission and absorption coefficients.…”

Section: Introductionmentioning

confidence: 99%

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Simulations of Neutrino and Gamma-Ray Production from Relativistic Black-Hole Microquasar Jets

2021

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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.

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Section: Interaction Mechanisms Inside the Jetmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Simulations of Neutrino and Gamma-Ray Production from Relativistic Black-Hole Microquasar Jets

2021

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“…It should be noted that direct detection experiments are exposed to various neutrino emissions [27][28][29][30]. The interaction of these neutrinos, especially the astrophysical ones, with the material of the dark matter detectors, known as the neutrino-floor, is a serious background source.…”

Section: Introductionmentioning

confidence: 99%

Event Rates for the Scattering of Weakly Interacting Massive Particles from 23Na and 40Ar

2021

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Detection rates for the elastic and inelastic scattering of weakly interacting massive particles (WIMPs) off 23Na are calculated within the framework of Deformed Shell Model (DSM) based on Hartree-Fock states. At first, the spectroscopic properties of the detector nucleus, like energy spectra and magnetic moments, are evaluated and compared with experimental data. Following the good agreement of these results, DSM wave functions are used for obtaining elastic and inelastic spin structure functions, nuclear structure coefficients and so forth for the WIMP-23Na scattering. Then, the event rates are also computed with a given set of supersymmetric parameters. In the same manner, using DSM wavefunctions, nuclear structure coefficients and event rates for elastic scattering of WIMPs from 40Ar are also obtained. These results for event rates and also for annual modulation will be useful for the ongoing and future WIMP detection experiments involving detector materials with 23Na and 40Ar nuclei.

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“…Due to the fact that neutrinos interact very weakly, they are unique messengers from astrophysical sources (the Earth, the Sun, the supernovae and other stars) [1,2,21] allowing us to investigate deep into the astrophysical objects [21,[27][28][29]. In the near future, remarkably sensitive detectors as liquid-scintillator detectors, liquid argon time projection chambers and water-Cherenkov detectors would operate aiming to study neutrino physics issues of astrophysical neutrino sources [19,20,26] (for higher energy neutrinos, like e.g.…”

Section: Introductionmentioning

confidence: 99%

Simulated Neutrino Signals of Low and Intermediate Energy Neutrinos on Cd Detectors

Sinatkas¹,

Tsakstara

Kosmas

2019

Front. Phys.

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Neutrino-nucleus reactions cross sections, obtained for neutrino energies in the range εν ≤ 100 − 120 MeV (low-and intermediate-energy range), which refer to promising neutrino detection targets of current terrestrial neutrino experiments, are presented and discussed. At first, we evaluated original cross sections for elastic scattering of neutrinos produced from various astrophysical and laboratory neutrino sources with the most abundant Cd isotopes 112 Cd, 114 Cd and 116 Cd. These isotopes constitute the main material of the COBRA detector aiming to search for neutrinoless double beta decay events and neutrino-nucleus scattering events at the Gran Sasso laboratory (LNGS). The coherent ν-nucleus reaction channel addressed with emphasis here, dominates the neutral current ν-nucleus scattering, events of which have only recently been observed for a first time in the COHERENT experiment at Oak Ridge. Subsequently, simulated ν-signals expected to be recorded at Cd detectors are derived through the application of modern simulation techniques and employment of reliable neutrino distributions of astrophysical ν-sources (as the solar, supernova and Earth neutrinos), as well as laboratory neutrinos (like the reactor neutrinos, the neutrinos produced from pion-muon decay at rest and the β-beam neutrinos produced from the acceleration of radioactive isotopes at storage rings as e.g. at CERN).

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Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Cited by 17 publications

References 35 publications

Simulations of Neutrino and Gamma-Ray Production from Relativistic Black-Hole Microquasar Jets

Simulations of Neutrino and Gamma-Ray Production from Relativistic Black-Hole Microquasar Jets

Event Rates for the Scattering of Weakly Interacting Massive Particles from 23Na and 40Ar

Simulated Neutrino Signals of Low and Intermediate Energy Neutrinos on Cd Detectors

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