Cosmic Cerenkov emission

Details Cosmic Cerenkov emission Cosmic Cerenkov emission

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..37..449c&link_type=abstract

Astrophysics and Space Science, vol. 37, Oct. 1975, p. 449-454.

Astronomy and Astrophysics

Astrophysics

3

Cerenkov Radiation, High Energy Electrons, Pulsars, Quasars, Stellar Radiation, Brightness Temperature, Electromagnetic Absorption, Electron Energy, Luminous Intensity, Relativistic Particles

Scientific paper

In real intensive cosmic sources it is necessary to take into account the Cerenkov reabsorption which restricts the brightness temperature of Cerenkov emission by energies of emitted relativistic electrons. As Cerenkov optical depth is given by tau equal to about N/E, the brightness temperature of emission on frequencies near gyrofrequency is determined by electron energy Er in which tau (Er) = 1. It is shown that most of the synchrotron sources (quasars, pulsars) must be powerful sources of Cerenkov emission. In these sources the high density of low-frequency Cerenkov emission can give rise to many parametric effects.

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