The Experts below are selected from a list of 135 Experts worldwide ranked by ideXlab platform
V.g. Sinitsyna - One of the best experts on this subject based on the ideXlab platform.
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TeV Gamma-rays from Galactic sources: Tycho's SNR, Geminga and Crab Nebula
2020Co-Authors: V.g. Sinitsyna, T. P. Arsov, A. A. Malyshko, S. I. Nikolsky, G. F. Platonov, P. N. LebedevAbstract:The Gamma-Quantum spectra produced by the electronic and hadronic components of cos- mic rays have similar shapes at the energies from 1GeV to 1 TeV due to the synchrotron losses of the electrons. So, the only observational possibility to discriminate between leptonic and hadronic contribu- tions is to measure the Gamma-Quantum spectrum at energies higher than 1 TeV, where these two spectra are expected to be essentially different. The Gamma-Quantum emitting objects in our Galaxy are the supernova remnants and binary. According to the theoretical prediction about 20 Supernova Remnants should be visible in the TeV Gamma-rays whereas only two were detected up to now by SHALON in northern hemisphere, namely Tycho's SNR and Geminga. The observation results of Gamma-Quantum sources Tycho Brage and Geminga by SHALON Gamma-telescope are presented. The energy spectra of Geminga supernova remnants and Tycho's SNR F(EO > 0:8 TeV ) / E k are found to be harder than Crab Nebula spectrum. The integral energy spectrum of Crab Nebula is well described by the single power law I(> E∞) / E i1:44§0:07 ∞ . Geminga is one of the brightest sources of MeV - GeV Gamma-ray. The value Geminga flux obtained by SHALON is lower than the upper limits published before. Its integral Gamma-ray flux is found to be (0:48 § 0:17) £ 10 i12 at energies of > 0:8 TeV . Within the range 0.8 - 5 TeV, the integral energy spectrum is well described by the single power law I(> E i ∞) / E i0:58§0:11 ∞ . The integral Gamma-ray flux of Tycho.s SNR above 0.8 TeV by SHALON was estimated as (0:52 § 0:09) £ 10 i12 . The energy spectrum of Tycho's SNR at 0.8 - 20 TeV can be approximated by the power law I(> E∞) / E k ∞ , with k∞ = i1:00 § 0:06. The expected … - -decay Gamma-Quantum flux F∞ / E i1 ∞ extends up to 30 TeV, whereas the Inverse Compton Gamma-ray flux has a cutoff above the few TeV. So, the detection of Gamma-rays at energies of 10 - 40 TeV by SHALON is the evidence of hadron origin.
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TeV Gamma-ray emission from binaries: 2129+47XR and Cygnus X-3
Nuclear Physics B - Proceedings Supplements, 2008Co-Authors: V.g. Sinitsyna, T. P. Arsov, S. I. Nikolsky, G. F. Platonov, A. Y. Alaverdian, S. S. Borisov, R. M. Mirzafatikhov, F.i. Musin, V. Y. Sinitsyna, J. N. CapdevielleAbstract:The new galactic Gamma-source (neutron star) 2129+47XR is detected at energy > 0.8 TeV with flux ( 0.19 ± 0.09 ) × 10 −12 cm 2 s −1 and indices of the integral spectra are k γ = − 1.12 ± 0.06 , k O N = − 1.28 ± 0.07 and k O f f = − 1.73 ± 0.07 . The results of ten-year observation of galactic source Cygnus X-3 by SHALON mirror Cherenkov telescope are discussed. The Gamma -Quantum spectra and images of the sources are presented. The Cygnus X-3 binary, known for more than 20 years as a source with variable intensity have been regularly observed since a 1995. The the increase of Gamma-Quantum flux was observed in 1997 and 2003 years.
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Extensive air showers generated by Gamma-quanta from Geminga and Tycho's SNR at energy range 1–30 TeV
Nuclear Physics B - Proceedings Supplements, 2005Co-Authors: V.g. Sinitsyna, T. P. Arsov, S. I. Nikolsky, A. Y. Alaverdian, S. S. Borisov, F.i. Musin, V. Y. Sinitsyna, G. F. PlatonovAbstract:The Gamma-Quantum emitting objects in our Galaxy are supernova remnants and binary. The observed results of Gamma-Quantum sources Tycho Brahe and Geminga by the SHALON Gamma-telescope are presented. The integral spectra of events from the source - k o n and background events, observing simultaneously with source's events - k o f f , and the source image are presented. The energy spectra of Tycho's SNR and Geminga supernova remnant F ( E 0 > 0.8 T e V ) ∼ E k are harder than the Crab Nebula spectrum. Tycho's SNR has long been considered as a candidate cosmic ray source in Northern Hemisphere. A non-linear kinetic model of cosmic ray acceleration in supernova remnants was used for Tycho's SNR. The expected π °-decay Gamma-quanta flux F γ ∼ E γ −1 extends up to ∼30TeV, whereas the Inverse Compton Gamma-ray flux has a cut-off above a few TeV. So, the detection of Gamma-rays at energies of ∼ 10 − 30 T e V by SHALON is evidence for hadron origin.
G. F. Platonov - One of the best experts on this subject based on the ideXlab platform.
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TeV Gamma-rays from Galactic sources: Tycho's SNR, Geminga and Crab Nebula
2020Co-Authors: V.g. Sinitsyna, T. P. Arsov, A. A. Malyshko, S. I. Nikolsky, G. F. Platonov, P. N. LebedevAbstract:The Gamma-Quantum spectra produced by the electronic and hadronic components of cos- mic rays have similar shapes at the energies from 1GeV to 1 TeV due to the synchrotron losses of the electrons. So, the only observational possibility to discriminate between leptonic and hadronic contribu- tions is to measure the Gamma-Quantum spectrum at energies higher than 1 TeV, where these two spectra are expected to be essentially different. The Gamma-Quantum emitting objects in our Galaxy are the supernova remnants and binary. According to the theoretical prediction about 20 Supernova Remnants should be visible in the TeV Gamma-rays whereas only two were detected up to now by SHALON in northern hemisphere, namely Tycho's SNR and Geminga. The observation results of Gamma-Quantum sources Tycho Brage and Geminga by SHALON Gamma-telescope are presented. The energy spectra of Geminga supernova remnants and Tycho's SNR F(EO > 0:8 TeV ) / E k are found to be harder than Crab Nebula spectrum. The integral energy spectrum of Crab Nebula is well described by the single power law I(> E∞) / E i1:44§0:07 ∞ . Geminga is one of the brightest sources of MeV - GeV Gamma-ray. The value Geminga flux obtained by SHALON is lower than the upper limits published before. Its integral Gamma-ray flux is found to be (0:48 § 0:17) £ 10 i12 at energies of > 0:8 TeV . Within the range 0.8 - 5 TeV, the integral energy spectrum is well described by the single power law I(> E i ∞) / E i0:58§0:11 ∞ . The integral Gamma-ray flux of Tycho.s SNR above 0.8 TeV by SHALON was estimated as (0:52 § 0:09) £ 10 i12 . The energy spectrum of Tycho's SNR at 0.8 - 20 TeV can be approximated by the power law I(> E∞) / E k ∞ , with k∞ = i1:00 § 0:06. The expected … - -decay Gamma-Quantum flux F∞ / E i1 ∞ extends up to 30 TeV, whereas the Inverse Compton Gamma-ray flux has a cutoff above the few TeV. So, the detection of Gamma-rays at energies of 10 - 40 TeV by SHALON is the evidence of hadron origin.
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TeV Gamma-ray emission from binaries: 2129+47XR and Cygnus X-3
Nuclear Physics B - Proceedings Supplements, 2008Co-Authors: V.g. Sinitsyna, T. P. Arsov, S. I. Nikolsky, G. F. Platonov, A. Y. Alaverdian, S. S. Borisov, R. M. Mirzafatikhov, F.i. Musin, V. Y. Sinitsyna, J. N. CapdevielleAbstract:The new galactic Gamma-source (neutron star) 2129+47XR is detected at energy > 0.8 TeV with flux ( 0.19 ± 0.09 ) × 10 −12 cm 2 s −1 and indices of the integral spectra are k γ = − 1.12 ± 0.06 , k O N = − 1.28 ± 0.07 and k O f f = − 1.73 ± 0.07 . The results of ten-year observation of galactic source Cygnus X-3 by SHALON mirror Cherenkov telescope are discussed. The Gamma -Quantum spectra and images of the sources are presented. The Cygnus X-3 binary, known for more than 20 years as a source with variable intensity have been regularly observed since a 1995. The the increase of Gamma-Quantum flux was observed in 1997 and 2003 years.
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Extensive air showers generated by Gamma-quanta from Geminga and Tycho's SNR at energy range 1–30 TeV
Nuclear Physics B - Proceedings Supplements, 2005Co-Authors: V.g. Sinitsyna, T. P. Arsov, S. I. Nikolsky, A. Y. Alaverdian, S. S. Borisov, F.i. Musin, V. Y. Sinitsyna, G. F. PlatonovAbstract:The Gamma-Quantum emitting objects in our Galaxy are supernova remnants and binary. The observed results of Gamma-Quantum sources Tycho Brahe and Geminga by the SHALON Gamma-telescope are presented. The integral spectra of events from the source - k o n and background events, observing simultaneously with source's events - k o f f , and the source image are presented. The energy spectra of Tycho's SNR and Geminga supernova remnant F ( E 0 > 0.8 T e V ) ∼ E k are harder than the Crab Nebula spectrum. Tycho's SNR has long been considered as a candidate cosmic ray source in Northern Hemisphere. A non-linear kinetic model of cosmic ray acceleration in supernova remnants was used for Tycho's SNR. The expected π °-decay Gamma-quanta flux F γ ∼ E γ −1 extends up to ∼30TeV, whereas the Inverse Compton Gamma-ray flux has a cut-off above a few TeV. So, the detection of Gamma-rays at energies of ∼ 10 − 30 T e V by SHALON is evidence for hadron origin.
Sergei P. Roshchupkin - One of the best experts on this subject based on the ideXlab platform.
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Resonant effect at the ultrarelativistic electron-positron pairs production by Gamma quanta in the field of a nucleus and a pulsed light wave.
arXiv: Atomic Physics, 2020Co-Authors: Sergei P. Roshchupkin, Nikita R. Larin, Victor V. DubovAbstract:Resonant electron-positron pair production by a high-energy Gamma Quantum in the field of a nucleus and a quasi-monochromatic laser wave was theoretically studied. Under the resonant condition an intermediate virtual electron (positron) in the laser field becomes a real particle. Due to that fact the initial process of the second order in the fine structure constant in a laser field effectively reduces into two successive processes of the first order: the laser-stimulated Breit-Wheeler process and the laser-assisted process of an intermediate electron (positron) scattering by a nucleus. It is shown that there is a threshold energy for the initial Gamma Quantum, which significantly depends on the number of absorbed photons of a wave. In the resonant condition the electron-positron pair energy is determined by the outgoing angle of a positron (for the channel A) or an electron (for the channel B) relative to the initial Gamma Quantum momentum. The differential cross sections for the first few resonances with simultaneous registration of the energy and the outgoing angle of a positron or an electron were obtained. For the initial Gamma Quantum energy ${\omega_i} = 125\;{\rm{GeV}}$ the resonant energies of an electron-positron pair for the case of first three resonances can be measured with a very high magnitude of the differential cross section: from $ \sim {10^{13}}$ for the first resonance to $ \sim {10^8}$ (in the units of $\alpha {Z^2}r_e^2$) for the third resonance.
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Resonant emission of hard Gamma-quanta at scattering of ultrarelativistic electrons on a nucleus within the external light field
Modern Physics Letters A, 2020Co-Authors: Alexander Dubov, Victor V. Dubov, Sergei P. RoshchupkinAbstract:The contemporary theoretical investigation researches the resonant emission of high-energy Gamma-quanta within the process of scattering of ultrarelativistic electrons on a nucleus in the external electromagnetic field. With implementation of the resonant conditions under the field ambience the particle in the intermediate state re-modulates into the real form. Therefore, the phenomenon examination determines the functional splitting of the second order process into a pair of first-order effects that possess a possibility to develop within two reaction channels. Consequently, the first channel characterizes the kinematics of electron scattering by a nucleus and following radiation of a spontaneous Gamma-Quantum. The second channel delineates the spontaneous Gamma-Quantum radiation by an electron with subsequent scattering on a nucleus. It is important to emphasize that within a specific range of observation the calculations derive three discrete magnitudes for the resonant frequency dependency on the angle of spontaneous photon radiation. As a result, the work represents an estimation of the resonant differential scattering cross-section in ratio to the scattering cross-section computed without the external field. In conclusion, various scientific facilities may verify the project data simulation (SLAC, FAIR, XFEL, ELI, XCELS).
Victor V. Dubov - One of the best experts on this subject based on the ideXlab platform.
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Resonant effect at the ultrarelativistic electron-positron pairs production by Gamma quanta in the field of a nucleus and a pulsed light wave.
arXiv: Atomic Physics, 2020Co-Authors: Sergei P. Roshchupkin, Nikita R. Larin, Victor V. DubovAbstract:Resonant electron-positron pair production by a high-energy Gamma Quantum in the field of a nucleus and a quasi-monochromatic laser wave was theoretically studied. Under the resonant condition an intermediate virtual electron (positron) in the laser field becomes a real particle. Due to that fact the initial process of the second order in the fine structure constant in a laser field effectively reduces into two successive processes of the first order: the laser-stimulated Breit-Wheeler process and the laser-assisted process of an intermediate electron (positron) scattering by a nucleus. It is shown that there is a threshold energy for the initial Gamma Quantum, which significantly depends on the number of absorbed photons of a wave. In the resonant condition the electron-positron pair energy is determined by the outgoing angle of a positron (for the channel A) or an electron (for the channel B) relative to the initial Gamma Quantum momentum. The differential cross sections for the first few resonances with simultaneous registration of the energy and the outgoing angle of a positron or an electron were obtained. For the initial Gamma Quantum energy ${\omega_i} = 125\;{\rm{GeV}}$ the resonant energies of an electron-positron pair for the case of first three resonances can be measured with a very high magnitude of the differential cross section: from $ \sim {10^{13}}$ for the first resonance to $ \sim {10^8}$ (in the units of $\alpha {Z^2}r_e^2$) for the third resonance.
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Resonant emission of hard Gamma-quanta at scattering of ultrarelativistic electrons on a nucleus within the external light field
Modern Physics Letters A, 2020Co-Authors: Alexander Dubov, Victor V. Dubov, Sergei P. RoshchupkinAbstract:The contemporary theoretical investigation researches the resonant emission of high-energy Gamma-quanta within the process of scattering of ultrarelativistic electrons on a nucleus in the external electromagnetic field. With implementation of the resonant conditions under the field ambience the particle in the intermediate state re-modulates into the real form. Therefore, the phenomenon examination determines the functional splitting of the second order process into a pair of first-order effects that possess a possibility to develop within two reaction channels. Consequently, the first channel characterizes the kinematics of electron scattering by a nucleus and following radiation of a spontaneous Gamma-Quantum. The second channel delineates the spontaneous Gamma-Quantum radiation by an electron with subsequent scattering on a nucleus. It is important to emphasize that within a specific range of observation the calculations derive three discrete magnitudes for the resonant frequency dependency on the angle of spontaneous photon radiation. As a result, the work represents an estimation of the resonant differential scattering cross-section in ratio to the scattering cross-section computed without the external field. In conclusion, various scientific facilities may verify the project data simulation (SLAC, FAIR, XFEL, ELI, XCELS).
T. P. Arsov - One of the best experts on this subject based on the ideXlab platform.
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TeV Gamma-rays from Galactic sources: Tycho's SNR, Geminga and Crab Nebula
2020Co-Authors: V.g. Sinitsyna, T. P. Arsov, A. A. Malyshko, S. I. Nikolsky, G. F. Platonov, P. N. LebedevAbstract:The Gamma-Quantum spectra produced by the electronic and hadronic components of cos- mic rays have similar shapes at the energies from 1GeV to 1 TeV due to the synchrotron losses of the electrons. So, the only observational possibility to discriminate between leptonic and hadronic contribu- tions is to measure the Gamma-Quantum spectrum at energies higher than 1 TeV, where these two spectra are expected to be essentially different. The Gamma-Quantum emitting objects in our Galaxy are the supernova remnants and binary. According to the theoretical prediction about 20 Supernova Remnants should be visible in the TeV Gamma-rays whereas only two were detected up to now by SHALON in northern hemisphere, namely Tycho's SNR and Geminga. The observation results of Gamma-Quantum sources Tycho Brage and Geminga by SHALON Gamma-telescope are presented. The energy spectra of Geminga supernova remnants and Tycho's SNR F(EO > 0:8 TeV ) / E k are found to be harder than Crab Nebula spectrum. The integral energy spectrum of Crab Nebula is well described by the single power law I(> E∞) / E i1:44§0:07 ∞ . Geminga is one of the brightest sources of MeV - GeV Gamma-ray. The value Geminga flux obtained by SHALON is lower than the upper limits published before. Its integral Gamma-ray flux is found to be (0:48 § 0:17) £ 10 i12 at energies of > 0:8 TeV . Within the range 0.8 - 5 TeV, the integral energy spectrum is well described by the single power law I(> E i ∞) / E i0:58§0:11 ∞ . The integral Gamma-ray flux of Tycho.s SNR above 0.8 TeV by SHALON was estimated as (0:52 § 0:09) £ 10 i12 . The energy spectrum of Tycho's SNR at 0.8 - 20 TeV can be approximated by the power law I(> E∞) / E k ∞ , with k∞ = i1:00 § 0:06. The expected … - -decay Gamma-Quantum flux F∞ / E i1 ∞ extends up to 30 TeV, whereas the Inverse Compton Gamma-ray flux has a cutoff above the few TeV. So, the detection of Gamma-rays at energies of 10 - 40 TeV by SHALON is the evidence of hadron origin.
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TeV Gamma-ray emission from binaries: 2129+47XR and Cygnus X-3
Nuclear Physics B - Proceedings Supplements, 2008Co-Authors: V.g. Sinitsyna, T. P. Arsov, S. I. Nikolsky, G. F. Platonov, A. Y. Alaverdian, S. S. Borisov, R. M. Mirzafatikhov, F.i. Musin, V. Y. Sinitsyna, J. N. CapdevielleAbstract:The new galactic Gamma-source (neutron star) 2129+47XR is detected at energy > 0.8 TeV with flux ( 0.19 ± 0.09 ) × 10 −12 cm 2 s −1 and indices of the integral spectra are k γ = − 1.12 ± 0.06 , k O N = − 1.28 ± 0.07 and k O f f = − 1.73 ± 0.07 . The results of ten-year observation of galactic source Cygnus X-3 by SHALON mirror Cherenkov telescope are discussed. The Gamma -Quantum spectra and images of the sources are presented. The Cygnus X-3 binary, known for more than 20 years as a source with variable intensity have been regularly observed since a 1995. The the increase of Gamma-Quantum flux was observed in 1997 and 2003 years.
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Extensive air showers generated by Gamma-quanta from Geminga and Tycho's SNR at energy range 1–30 TeV
Nuclear Physics B - Proceedings Supplements, 2005Co-Authors: V.g. Sinitsyna, T. P. Arsov, S. I. Nikolsky, A. Y. Alaverdian, S. S. Borisov, F.i. Musin, V. Y. Sinitsyna, G. F. PlatonovAbstract:The Gamma-Quantum emitting objects in our Galaxy are supernova remnants and binary. The observed results of Gamma-Quantum sources Tycho Brahe and Geminga by the SHALON Gamma-telescope are presented. The integral spectra of events from the source - k o n and background events, observing simultaneously with source's events - k o f f , and the source image are presented. The energy spectra of Tycho's SNR and Geminga supernova remnant F ( E 0 > 0.8 T e V ) ∼ E k are harder than the Crab Nebula spectrum. Tycho's SNR has long been considered as a candidate cosmic ray source in Northern Hemisphere. A non-linear kinetic model of cosmic ray acceleration in supernova remnants was used for Tycho's SNR. The expected π °-decay Gamma-quanta flux F γ ∼ E γ −1 extends up to ∼30TeV, whereas the Inverse Compton Gamma-ray flux has a cut-off above a few TeV. So, the detection of Gamma-rays at energies of ∼ 10 − 30 T e V by SHALON is evidence for hadron origin.
