Origin of Gamma-Ray Emissions from the MeV Blazars

Details Origin of Gamma-Ray Emissions from the MeV Blazars Origin of Gamma-Ray Emissions from the MeV Blazars

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998stin...0025439g&link_type=abstract

Conference Paper, International Gamma-Ray Astrophysics Lab. Workshop (INTEGRAL)

Astronomy and Astrophysics

Astrophysics

Gamma Ray Spectra, Blazars, Synchrotrons, Photons, High Energy Electrons, Gamma Ray Observatory, X Rays, Electrons, Cooling, Color, Backscattering

Scientific paper

More than sixty gamma-ray emitting blazars have been detected by the Compton Gamma Ray Observatory (CGRO). A sub-class of these blazars is known as MeV blazars that are most luminous at the MeV energies. Spectra of these sources show a break somewhere between 1 MeV and 30 MeV with break amplitude as large as Delta(Gamma) = 1.5. Different models like Compton cooling jet models, synchrotron self-Compton models, etc., have been suggested to explain the observed properties of the MeV luminous blazars. However these models are unable to account for spectral break amplitudes in excess of 0.5. Here we suggest an inverse-Compton model based on recent published experimental data where MeV gamma rays were produced via Compton backscattering of UV photons with 500 MeV electrons. We show that the high energy electrons of the relativistic jet can collide with the copious ultraviolet photons of the big blue bump of the blazar, and produce photons peaked in the MeV region. Also we show that the X rays and the soft gamma rays in these sources are produced through the synchrotron self-Compton process. Flux computed from our model have been used to compare with the observed X-ray/ gamma-ray spectra of the MeV luminous blazars. Details of the model are discussed in the present paper.

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