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COMPTON RADIATION OF THE CRAB NEBULA

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Usually radioemission from a compact source is considered as a radiation of the pulsar, and the observed spectrum is joined. In the model of radioemission presented here the frequency spectrum of a compact source and a pulsar described separately. The observed spectrum is a superposition of independent spectra of a compact source and a pulsar, with the indices <$>\alpha_c=2.09<$> and <$>\alpha_p=3.5<$>. The pulsar spectrum continues to high frequencies beyond <$>100\,\hbox{MHz}<$>, with a cutoff at lower frequencies. The pressure of magnetic dipole radiation from a rotating pulsar with <$>\Omega=33\,\hbox{Hz}<$> sweeps up the plasma from the cavity around pulsar. The size of the cavity determines the size of the compact source, which have brightness temperature above <$>10^{12}\,\hbox{K}<$>, and negligible reabsorbtion. Therefore radiating particles must be relativistic protons. The photons of the magnetic dipole radiation scatter on these protons, and trough inverse Compton effect their frequencies grow significantly. Compton radiation is observed as a radiation of the compact source. The radiating protons must have energies <$>10^{11} \lt E\lt 2\times 10^{12}\,\hbox{eV}<$>.
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Keywords: Compact source; Compton radiation; Magnetic dipole radiation; Pulsar; Radioemission; Relativistic proton; Scattering

Document Type: Research Article

Affiliations: Radiophysical Research Institute, Bolshaya Pecherskaya 25, Nizhny Novgorod 603950, Russia

Publication date: 2002-01-01

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