Energy Distribution Of Relativistic Electrons Research Articles

Anisotropic inverse Compton scattering from the trans-relativistic to the ultra-relativistic regime and application to the radio galaxies

The problem of the anisotropic Inverse Compton scattering between a monochromatic photon beam and relativistic electrons is revisited and formally solved without approximations. Solutions are given for the single scattering with an electron beam and with a population of electrons isotropically distributed, under the assumption that the energy distribution of the relativistic particles follows a simple power law as it is the case in many astrophysical applications. Both the Thomson approximation and the Klein–Nishina regime are considered for the scattering of an unpolarized photon beam. The equations are obtained without the ultra-relativistic approximation and are compared with the ultra-relativistic solutions given in the literature. The main characteristics of the power distribution and spectra of the scattered radiation are discussed for relevant examples. In the Thomson case simple analytic and semi-analytic formulae holding down to the trans-relativistic energies are given. As an application the formulae of the anisotropic inverse Compton scattering are used to predict the properties of the X and γ-ray spectra from the radio lobes of strong FR II radio galaxies due to the interaction of the relativistic electrons with the incoming photons from the nucleus. The dependence of the broad band emitted power on the relativistic electron energy distribution and on its evolution with time is discussed.

Energy distribution of relativistic electrons in the tunneling ionization of atoms by super-intense laser radiation

We studied theoretically the influence of relativistic effects on the energy distribution of electrons in the tunneling ionization of atoms by a field of linearly polarized super-intense laser radiation. It was shown that the energy distribution of ejected electrons is determined by relativistic law though the electron kinetic energy can be less than its rest energy. The relativistic probability of ionization along the field strength decreases exponentially with the electron kinetic energy, but more quickly than in the non-relativistic case.

Improved e-beam electron range measurements: experiments and analysis

A thermoluminescent dosimeter electron range measurement technique has been used to measure the energy distribution of relativistic electrons in a diffuse e-beam. The doses produced by the e-beam at 12 aluminum absorber thicknesses have been measured. The experimental technique is described. Angular distributions of the electrons have also been obtained. The technique has been used to investigate a relativistic electron beam that has emerged from the steel exit port of a drift tube filled with He gas at a pressure below 1 torr. The sensitivity of the measuring technique to the beam energy and angular distribution has been investigated. The experimental results are compared to Monte Carlo calculations. The results are sensitive to maximum e-beam energy and can be used to explore e-beam physics. >

Source models with electron diffusion

The general solution for the energy distribution of relativistic electrons in which electrons generated within the source diffuse and decay through synchrotron or Compton radiation is given for the case in which the magnetic field and the diffusion coefficient are constant. A very simple spherically symmetric model with an electron point-source at the centre is considered and the equations are explicitly solved. It is shown that notwithstanding its great simplicity this model gives a fair representation of the continuous emission of the Crab nebula from the radio to the X-ray region, with the simple assumption that it is due only to ordinary synchrotron radiation. If the central point source is identified with the pulsar there appears to be an upper limit of about 107 MeV to the energy of the electrons accelerated by the pulsar mechanism.

The Spectra of Radio Sources in the Revised 3c Catalogue

Accurate values of the flux density are given for nearly all sources in the Revised Third Cambridge Catalogue at frequencies of 38, 178, 750, 1400, 2695, and 5000 MHz. These have been used to determine the spectrum of each source over this frequency range. It is concluded that the form of the spectra in many sources is determined not only by the energy distribution of relativistic electrons but also, as a result of self-absorption, by their spatial distribution. Sources identified with quasi-stellar objects have a wider dispersion of spectral indices than those identified with radio galaxies, particularly at the higher fre- quencies. Among the radio galaxies, the intrinsically strongest sources appear to have the steepest spectra. Unidentified sources have steep spectra similar to those of the stronger radio galaxies, and they are probably distant galaxies

The determination of the energy distribution of relativistic electrons by the frequency distribution of their “synchrotron radiation”

Relativistic electrons moving in a homogeneous magnetic field H emit “synchrotron radiation” with a frequency distribution which may be written in the following form.