scholarly journals RELATIVISTIC NON-THERMAL BREMSSTRAHLUNG RADIATION

2013 ◽  
Vol 28 (29) ◽  
pp. 1350141 ◽  
Author(s):  
VLADIMIR ZEKOVIĆ ◽  
BOJAN ARBUTINA ◽  
ALEKSANDRA DOBARDŽIĆ ◽  
MARKO Z. PAVLOVIĆ
Keyword(s):  
Electron Scattering ◽  
Relativistic Effects ◽  
Scattered Photon ◽  
Relativistic Electrons ◽  
Ion Scattering ◽  
Bremsstrahlung Radiation ◽  
Significant Component ◽  
Bremsstrahlung Emission ◽  
Relativistic Kinetic Energy ◽  
Thermal Bremsstrahlung

By applying a method of virtual quanta we derive formulae for relativistic non-thermal bremsstrahlung radiation from relativistic electrons as well as from protons and heavier particles with power-law momentum distribution N(p)dp = k p-qdp. We show that emission which originates from an electron scattering on an ion, represents the most significant component of relativistic non-thermal bremsstrahlung. Radiation from an ion scattering on electron, known as inverse bremsstrahlung, is shown to be negligible in overall non-thermal bremsstrahlung emission. These results arise from theory refinement, where we introduce the dependence of relativistic kinetic energy of an incident particle, upon the energy of scattered photon. In part, it is also a consequence of a different mass of particles and relativistic effects.

80 MHz Survey of Extra-Galactic X-ray Sources

1979 ◽  
Vol 3 (5) ◽  
pp. 332-341 ◽  
Author(s):  
O. B. Slee ◽  
P. J. Quinn
Keyword(s):  
Angular Size ◽  
Virgo Cluster ◽  
Relativistic Electrons ◽  
Clusters Of Galaxies ◽  
Coma Cluster ◽  
Microwave Background ◽  
Significant Information ◽  
X Ray ◽  
Inverse Compton Scattering ◽  
Bremsstrahlung Emission

The completion of the Uhuru (Forman et al. 1978) and Ariel V (Cooke et al. 1978) surveys of the sky for X-ray emission has resulted in many proposed identifications with individual galaxies and clusters of galaxies. The X-ray positions are not usually accurate enough to enable a positive identification to be made of the X-ray sources with optical or radio objects, and hence the identification is often based on statistical arguments — viz., the unexpected occurrence of unusual galaxies, radio sources or clusters of galaxies within or near the X-ray error boxes. There is usually no significant information available on the angular size of the X-ray emitter but in two or three cases (e.g. Perseus cluster, Coma cluster and Virgo cluster) the angular resolution is good enough to identify a broad component with dimensions approaching those of the whole cluster. This extended X-ray emission has been ascribed to either inverse Compton scattering of the 3° microwave background by relativistic electrons in the intra-cluster medium or to thermal-bremsstrahlung emission by an optically thin plasma at - 10s K.

scholarly journals Polarization of thermal bremsstrahlung emission due to electron pressure anisotropy

2016 ◽  
Vol 461 (2) ◽  
pp. 2162-2173 ◽  
Author(s):  
S. V. Komarov ◽  
I. I. Khabibullin ◽  
E. M. Churazov ◽  
A. A. Schekochihin
Keyword(s):  
Electron Pressure ◽  
Pressure Anisotropy ◽  
Bremsstrahlung Emission ◽  
Thermal Bremsstrahlung

Effects of Grain Size on the Bremsstrahlung Spectrum of Electron-Dust Grain Collisions in Dusty Plasmas

2009 ◽  
Vol 64 (3-4) ◽  
pp. 229-232
Author(s):  
Seo-Hee Kim ◽  
Young-Dae Jung
Keyword(s):  
Grain Size ◽  
Cross Section ◽  
Dusty Plasmas ◽  
Bremsstrahlung Spectrum ◽  
Final States ◽  
Bremsstrahlung Radiation ◽  
Dust Charge ◽  
Bremsstrahlung Emission ◽  
Debye Radius ◽  
Dust Grain

Abstract The grain size effects on the bremsstrahlung emission spectrum due to nonrelativisitc electrondust grain collisions are investigated in dusty plasmas. Using the Born approximation for the initial and final states of the projectile electron, the bremsstranhlung radiation cross section is obtained as a function of the grain size, dust charge, Debye radius, collision energy, and radiation photon energy. It is found that the effects of the grain size enhance the bremsstrahlung radiation cross section, especially for soft-photon radiations. The effect of the Debye radius on the bremsstrahlung cross section is found to be increased with an increase of the magnitude of the charge number of the dust grain. In addition, the grain size effect on the bremsstrahlung spectrum is found to be more significant for highly charged dusty grains

scholarly journals Generalized Bessel Functions and Their Use in Bremsstrahlung and Multi-Photon Processes

Symmetry ◽  
2021 ◽  
Vol 13 (2) ◽  
pp. 159
Author(s):  
Giuseppe Dattoli ◽  
Emanuele Di Palma ◽  
Silvia Licciardi ◽  
Elio Sabia
Keyword(s):  
Free Electron Laser ◽  
Spectral Properties ◽  
Bessel Functions ◽  
Relativistic Electrons ◽  
Bremsstrahlung Radiation ◽  
Pendulum Equation ◽  
Harmonic Content ◽  
Generalized Bessel Functions ◽  
Linearly Polarized ◽  
Electro Magnetic

The theory of Generalized Bessel Functions is reviewed and their application to various problems in the study of electro-magnetic processes is presented. We consider the cases of emission of bremsstrahlung radiation by ultra-relativistic electrons in linearly polarized undulators, including also exotic configurations, aimed at enhancing the harmonic content of the emitted radiation. The analysis is eventually extended to the generalization of the FEL pendulum equation to treat Free Electron Laser operating with multi-harmonic undulators. The paper aims at picking out those elements supporting the usefulness of the Generalized Bessel Functions in the elaboration of the theory underlying the study of the spectral properties of the bremsstrahlung radiation emitted by relativistic charges, along with the relevant flexibility in accounting for a large variety of apparently uncorrelated phenomenolgies, like multi-photon processes, including non linear Compton scattering.

Compton Scattering of 279.1 and 661.6 keV Photons by K-shell Electrons

1981 ◽  
Vol 34 (2) ◽  
pp. 163 ◽  
Author(s):  
IB Whittingham
Keyword(s):  
Cross Section ◽  
Cross Sections ◽  
Free Electron ◽  
Relativistic Effects ◽  
High Energy ◽  
Infrared Divergence ◽  
Scattered Photon ◽  
Conservation Of Energy ◽  
Energy Cutoff ◽  
Photon Spectra

The spectral distributions of 279?1 and 661? 6 keY photons incoherently scattered by the K electrons of U, Pb, Ta and Sm are calculated for a point-Coulomb potential using a theory previously developed by the author which accounts completely for electron binding and relativistic effects. WKB treatments of the regular and irregular continuum Dirac wavefunctions have been developed and used to mprove the computation of the 'absorption-first' radial matrix elements. The scattered photon spectra for the four elements and scattering angles for which the free electron Compton energy lies below the high energy cutoff due to conservation of energy have broad peaks shifted by 3 to 18 and by 30 to 50 keY, for 279?1 and 661? 6 keY photons respectively, from the free electron Compton energy towards higher scattered photon energies. An infrared divergence, whose magnitude increases strongly with atomic number, commences at ~ 56 keV and is present in those spectra where there is no peak or where the peak lies significantly above 56 keY. Differential cross sections daK' computed using a low energy cutoff, are nonzero for zero-angle scattering and are lower than the Klein-Nishina cross section daF for scattering angles ~ 50� for 661?6 keV photons and for all scattering angles for 279?1 keY photons (with the exception of 80�-130� in the case of Sm). The cross section ratio daK/daF increases with increasing scattering angle until about 100� and 80� for 279?1 and 661? 6 keY photons respectively and then subsequently decreases slowly.

A classical relativistic hydrodynamical model for strong EM wave-spin plasma interaction

2021 ◽  
Author(s):  
Qianglin Hu ◽  
Wen Hu
Keyword(s):  
Ponderomotive Force ◽  
Lagrange Equation ◽  
Relativistic Effects ◽  
High Energy ◽  
Magnetized Plasma ◽  
Relativistic Electrons ◽  
Plasma Interaction ◽  
Spin Effects ◽  
Relativistic Factor ◽  
Time Component

Abstract Based on the covariant Lagrangian function and Euler-Lagrange equation, a set of classical fluid equations for strong EM wave-spin plasma interaction is derived. Analysis shows that the relativistic effects may affect the interaction processes by three factors: the relativistic factor, the time component of four-spin, and the velocity-field coupling. This set of equations can be used to discuss the collective spin effects of relativistic electrons in classical regime, such as astrophysics, high-energy laser-plasma systems and so on. As an example, the spin induced ponderomotive force in the interaction of strong EM wave and magnetized plasma is investigated. Results show that the time component of four-spin, which approaches to zero in nonrelativistic situations, can increase the spin-ponderomotive force obviously in relativistic situation.

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