A role of cosmic rays in generation of radio and optical radiation by plasma mechanisms

Топтыгин, И. Н.; Fleishman, G. D.

doi:10.1007/bf00641755

Cited by 41 publications

(65 citation statements)

References 13 publications

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“…Here, B is the strength of the magnetic field as a function of the height of the jet, and other parameters have a conventional meaning. On the contrary, λ ≪ R L , the emission is referred to as diffusive synchrotron radiation (Toptygin & Fleishman 1987), or jitter radiation (Medvedev 2000;Kelner et al 2013). Below, we first study the evolution of relativistic electrons in jets, which has an isotropic distribution along the jets.…”

Section: Model Descriptionsmentioning

confidence: 99%

Polarization Radiation with Turbulent Magnetic Fields from X-Ray Binaries

Zhang

Xiang

2017

ApJ

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We study the properties of polarized radiation in turbulent magnetic fields from X-ray binary jets. These turbulent magnetic fields are composed of large-and small-scale configurations, which result in the polarized jitter radiation when the characteristic length of turbulence is less than the nonrelativistic Larmor radius. On the contrary, the polarized synchrotron emission occurs, corresponding to a large-scale turbulent environment. We calculate the spectral energy distributions and the degree of polarization for a general microquasar. Numerical results show that turbulent magnetic field configurations can indeed provide a high degree of polarization, which does not mean that a uniform, large-scale magnetic field structure exists. The model is applied to investigate the properties of polarized radiation of black hole X-ray binary Cygnus X-1. Under the constraint of multiband observations of this source, our studies demonstrate that the model can explain the high polarization degree at MeV tail and predict the highly polarized properties at high-energy γ-ray region, and that the dominant small-scale turbulent magnetic field plays an important role for explaining the highly polarized observation at hard X-ray/soft γ-ray bands. This model can be tested by polarization observations of upcoming polarimeters at high-energy γ-ray bands.

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Section: Model Descriptionsmentioning

confidence: 99%

Polarization Radiation with Turbulent Magnetic Fields from X-Ray Binaries

Zhang

Xiang

2017

ApJ

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“…10 and 11 requires that electron's motion is random small-angle scattering, that implies the magnetic field is effectively uncorrelated on scales larger than ℓ c or -more preciselythat the power spectrum of the magnetic field B 2 k peaks at k = 1/ℓ c and decreases towards smaller wavenumbers faster than B 2 k ∝ k. Under such circumstances, the electrons emit mostly due to their interaction with small-scale magnetic field inhomogeneities. If ℓ c < r g0 , then electrons radiate in the undulator regime [5,6] and the typical frequency of their emission increases with decreasing magnetic-field scale.…”

Section: Location Of the Peakmentioning

confidence: 99%

Synchrotron emission in the fast cooling regime: which spectra can be explained?

Derishev

2007

Astrophys Space Sci

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We consider the synchrotron emission from relativistic shocks assuming that the radiating electrons cool rapidly (either through synchrotron or any other radiation mechanism). It is shown that the theory of synchrotron emission in the fast cooling regime can account for a wide range of spectral shapes. In particular, the magnetic field, which decays behind the shock front, brings enough flexibility to the theory to explain the majority of gamma-ray burst spectra even in the parameterfree fast cooling regime. Also, we discuss whether location of the peak in observed spectral energy distributions of gamma-ray bursts and active galactic nuclei can be made consistent with predictions of diffusive shock acceleration theory, and find that the answer is negative. This result is a strong indication that a particle injection mechanism, other than the standard shock acceleration, works in relativistic shocks.

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“…Equation (17) in the presence of both uniform and random magnetic fields has been solved in [4] (sf [5]):…”

Section: Solution Of the Kinetic Equationmentioning

confidence: 99%

“…Then, calculation of (29), described in detail in [4] and reformulated here to more convenient notations, results in…”

Section: General Casementioning

confidence: 99%

“…Let us consider first the case of hard spectrum [4], which is typical, e.g., for supernova remnants and radio galaxies. Assuming the small-scale field to be small compared with the regular field, we may expect the contribution of diffusive synchrotron radiation to be noticeable only in those frequency ranges where synchrotron emission is small.…”

Section: Hard Electron Spectrummentioning

confidence: 99%

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Generation of Emissions by Fast Particles in Stochastic Media

Fleishman

Geospace Electromagnetic Waves and Radiation

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A role of cosmic rays in generation of radio and optical radiation by plasma mechanisms

Cited by 41 publications

References 13 publications

Polarization Radiation with Turbulent Magnetic Fields from X-Ray Binaries

Polarization Radiation with Turbulent Magnetic Fields from X-Ray Binaries

Synchrotron emission in the fast cooling regime: which spectra can be explained?

Generation of Emissions by Fast Particles in Stochastic Media

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