Synchrotron Emission Of Electrons Research Articles

The source and structure of the jovian radiation belt

The radio emission from Jupiter at 10, 21 cm wavelength has been measured with a spatial resolution of the order of 1 Jupiter radius. This may be analytically reduced to the emission per cubic centimeter of source at each measured frequency. The theoretically predicted synchrotron emission of electrons as a function of frequency, magnetic field and electron energy can then be compared to the observed source emissivity to obtain the number density and ‘temperature’ of the electrons. Present observations taken at different epochs are not sufficiently reliable to infer peak energies within an order of magnitude. Nevertheless the present results indicate that electrons diffuse in rapidly (in a time of the order of months) conserving the first adiabatic invariant and reach a peak energy at about 2 Jupiter radii. The electron energy decreases rapidly nearer the planet because of energy lost to radiation in the large magnetic field close to the planet.

Influence of the ionized medium on synchrotron emission of intermediate energy electrons

The suppression of synchrotron emission at low frequencies, owing to the influence of the ionized medium, is investigated. Explicit expressions and detailed numerical values of the emission spectra are presented for various electron energies and plasma and cyclotron frequencies. Unlike previous studies of this suppression effect, which were applicable only to ultrarelativistic electrons, the present treatment is valid for electrons of arbitrary energies and in particular for intermediate energy electrons such as those presumably accelerated in solar flares.

The relation between cosmic γ-rays and synchrotron X-rays

A quantitative relation between the intensities of cosmic γ-rays with energies near 1014 eV and X-rays generated by synchrotron emission of cosmic electrons is derived on the basis of the fact that these two radiations have a common energy source in the interactions between cosmic-ray nuclei and interstellar matter. The relation depends on the intensity of the magnetic field in the region of production. Quantitative estimates based on recent data indicate that synchrotron X-rays may constitute a significant component of cosmic X-rays below 3 a at high galactic latitudes. It may therefore be possible to obtain a new measurement of the interstellar magnetic field by a comparison of the intensities of cosmic X-rays and ultra-high-energy cosmic γ-rays.