A proton synchrotron blazar model for flaring in Markarian 501

The spectral energy distribution (SED) of gamma-ray (gamma -ray) loud BL Lac objects typically has a double-humped appearance usually interpreted in terms of synchrotron self-Compton models. In proton blazar models, the SED is instead explained in terms of acceleration of protons and subsequent cascading. We discuss a variation of the synchrotron proton blazar model, first proposed by Mucke and Protheroe (Proc. Workshop GeV-TeV Astrophysics: Toward a Major Atmospheric Cherenkov Telescope VI, Snowbird, Utah, submitted for publication), in which the low energy part of the SED is mainly proton synchrotron radiation by electrons co-accelerated with protons, which produce the high energy part of the SED mainly as synchrotron radiation. As an approximation, we assume non-relativistic shock acceleration which could apply if the bulk of the plasma in the jet frame were non-relativistic. Our results may therefore change if a relativistic equation of state was used. We consider the case where the maximum energy of the accelerated protons is above the threshold for pion photoproduction interactions on the synchrotron photons of the low energy part of the SED. Using a Monte Carlo/numerical technique to simulate the interactions and subsequent cascading of the accelerated protons, we are able to fit the high-energy gamma -ray portion of the observed SED of Markarian 501 during the April 1997 flare. We find that the emerging cascade spectra initiated by gamma -rays from pi (0) decay and by e(+/-) from mu (+/-) decay turn out to be relatively featureless. Synchrotron radiation produced by mu (+/-) from pi (+/-) decay, and even more importantly by protons, and subsequent synchrotron-pair cascading, is able to reproduce well the high energy part of the SED. For this fit, we find that synchrotron radiation by protons dominates the TeV emission, pion photoproduction being less important with the consequence that we predict a lower neutrino flux than in other proton blazar models. (C) 2001 Elsevier Science B.V. All rights reserved.