<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Kirk, J. G.</style></author><author><style face="normal" font="default" size="100%">Mastichiadis, A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Neutrons from active galactic nuclei</style></title><short-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">active galactic nuclei</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics</style></keyword><keyword><style  face="normal" font="default" size="100%">Black Holes (Astronomy)</style></keyword><keyword><style  face="normal" font="default" size="100%">Continuous Radiation</style></keyword><keyword><style  face="normal" font="default" size="100%">Flux (Rate)</style></keyword><keyword><style  face="normal" font="default" size="100%">Gamma Rays</style></keyword><keyword><style  face="normal" font="default" size="100%">Interstellar Magnetic Fields</style></keyword><keyword><style  face="normal" font="default" size="100%">Neutrons</style></keyword><keyword><style  face="normal" font="default" size="100%">Protons</style></keyword><keyword><style  face="normal" font="default" size="100%">Relativistic Particles</style></keyword><keyword><style  face="normal" font="default" size="100%">Synchrotron radiation</style></keyword><keyword><style  face="normal" font="default" size="100%">X Ray Sources</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">1989</style></year><pub-dates><date><style  face="normal" font="default" size="100%">1989/04/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/1989A&amp;A...213...75K</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">213</style></volume><pages><style face="normal" font="default" size="100%">75 - 79</style></pages><isbn><style face="normal" font="default" size="100%">0004-6361</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">A recently proposed acceleration mechanism for ultra relativistic particles in the central engines of AGN's suggests that protons are the particles which are accelerated initially, and that these subsequently inject the electrons and positrons supposed responsible for the continuum emission. This model necessarily leads to the prediction of a strong flux of neutrons (with a luminosity at least as great as that in the photon continuum) from the central engine. We investigate some of the consequences of such a model. In particular, the neutron flux will, by means of spallation reactions, produce amounts of boron in the surrounding material which it may be possible to observe in the optical spectrum. In addition, the central engine will act as a source of high energy gamma-rays. Those which can propagate to the Earth (i.e., those with energy &amp;lt; 10^14^ eV) may be observed directly, whereas those of higher energy will be absorbed by radio photons from either the microwave background or the AGN itself. If this occurs in a typical interstellar magnetic field, the energy of the gamma-rays will be reradiated in the form of X-rays.</style></abstract></record></records></xml>