Pair models revivified for high energy emission of AGNs

Details Pair models revivified for high energy emission of AGNs Pair models revivified for high energy emission of AGNs

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..410.1313h&link_type=abstract

The fourth compton symposium. AIP Conference Proceedings, Volume 410, pp. 1313-1317 (1997).

Computer Science

Active And Peculiar Galaxies And Related Systems, Magnitudes And Colors, Luminosities, Jets And Bursts, Galactic Winds And Fountains, Infall, Accretion, And Accretion Disks

Scientific paper

We argue that although the high energy emission of radio-loud and radio-weak AGNs are markedly different, they all exhibit remarkable features (either spectral break or upper cut-off) around or just below MeV energy. The critical energy is correlated with the expected Doppler factor determined by radio characteristics of these objects. This supports the idea that high energy emission is closely linked to pair production, with absorption or annihilation features. In the case of radio-loud blasars, gamma-gamma absorption explains remarkably well the position and the magnitude of the spectral break, with very few ad-hoc assumption on the particle distribution. In the case of Seyfert galaxies, a static non thermal source, associating pair production and reacceleration, can explain the main features of high energy spectra. A self-consistent model associating anisotropic Inverse Compton process and disk reillumination predicts unambiguously the X/UV ratio, which is highly orientation dependant. We discuss some implications of this model for the understanding of present observations.

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