@article {30282,
	title = {Proton Synchrotron Gamma-Rays and the Energy Crisis in Blazars},
	volume = {893},
	year = {2020},
	month = {2020/04/1},
	pages = {L20},
	abstract = {The origin of high-energy emission in blazars jets (I.e., leptonic versus hadronic) has been a longstanding matter of debate. Here, we focus on one variant of hadronic models where proton synchrotron radiation accounts for the observed steady γ-ray blazar emission. Using analytical methods, we derive the minimum jet power ( ${P}_{j,\min }$ ) for the largest blazar sample analyzed to date (145 sources), taking into account uncertainties of observables and jet{\textquoteright}s physical parameters. We compare ${P}_{j,\min }$ against three characteristic energy estimators for accreting systems, I.e., the Eddington luminosity, the accretion disk luminosity, and the power of the Blandford-Znajek process, and find that ${P}_{j,\min }$ is about 2 orders of magnitude higher than all energetic estimators for the majority of our sample. The derived magnetic field strengths in the emission region require either large amplification of the jet{\textquoteright}s magnetic field (factor of 30) or place the γ-ray production site at sub-pc scales. The expected neutrino emission peaks at \~{}0.1-10 EeV, with typical peak neutrino fluxes \~{}10<SUP>-4</SUP> times lower than the peak γ-ray fluxes. We conclude that if relativistic hadrons are present in blazar jets, they can only produce a radiatively subdominant component of the overall spectral energy distribution of the blazar{\textquoteright}s steady emission.},
	keywords = {1100, 1119, 1390, 159, 164, 1663, 2055, Astrophysics - High Energy Astrophysical Phenomena, black hole physics, Blazars, Neutrino astronomy, Non-thermal radiation sources, Radiative processes, Relativistic jets, Supermassive black holes},
	isbn = {0004-637X},
	url = {https://ui.adsabs.harvard.edu/abs/2020ApJ...893L..20L},
	author = {Liodakis, Ioannis and Petropoulou, Maria}
}
