Relativistic neutrons in active galactic nuclei. I - Energy transport from the core. II - Gamma-rays of high and very high energies

Details Relativistic neutrons in active galactic nuclei. I - Energy transport from the core. II - Gamma-rays of high and very high energies Relativistic neutrons in active galactic nuclei. I - Energy transport from the core. II - Gamma-rays of high and very high energies

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...257..465a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 257, no. 2, p. 465-488.

Statistics

Computation

9

Active Galactic Nuclei, Energy Transfer, Gamma Ray Astronomy, Neutron Flux Density, Nuclear Astrophysics, Relativistic Particles, Computational Astrophysics, Cosmic Plasma, Distribution Functions, Elementary Particle Interactions

Scientific paper

An AGN model is considered where the relativistic proton acceleration in the vicinity of supermassive black hole is assumed, in which case the energy transport should naturally occur due to the relativistic neutrons (RNs) produced at nuclear p-p and p-gamma collisions in the proton acceleration region r not greater than r(0). In the framework of this AGN model, the problem of the electromagnetic cascade initiated in a spatially nonhomogeneous field of background photons due to propagation of RNs from the proton acceleration region r not greater than r(0) of about 10, and their decay at large radii (r greater than r(0) but less than 10 exp 7 to 10 exp 8), is considered (the N-cascade). It is shown that the radiation spectra resulting from the N-cascade can be described by the power-law functions gradually steepening with increasing gamma-ray energies.

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