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The expected high-energy to ultra-high-energy gamma-ray spectrum of the Crab Nebula
de Jager, O. C.; Harding, A. K.
AA(NASA, Goddard Space Flight Center, Greenbelt, MD), AB(NASA, Goddard Space Flight Center, Greenbelt, MD)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 396, no. 1, Sept. 1, 1992, p. 161-172. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Crab Nebula, Energy Spectra, Gamma Ray Spectra, High Energy Interactions, Interstellar Matter, Pulsars, Compton Effect, Magnetic Field Configurations, Magnetohydrodynamic Flow, Synchrotron Radiation
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The inverse Compton scattering model for the unpulsed TeV emission from the Crab Nebula is reexamined using the magnetic field distribution derived from MHD flow models of the nebula. It is shown that the observed flux can be explained if the average nebular field is indeed about 0.0003, as is predicted by the spectral break between radio and optical. The brightness distribution of the TeV gamma-ray signal is expected to extend out to about 1.5 arcmin from the pulsar. The present estimates predict a steady flux of unpulsed ultrahigh-energy gamma-rays due to the inverse Compton scattering of soft photons by shock-accelerated electrons and/or positrons in the vicinity of the shock.

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