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We discuss neutrino fluxes and energy dependent flavor ratios of cosmicaccelerators as a function of the size of the acceleration region and themagnetic field, which are the parameters of the Hillas plot. We assume thatphotohadronic interactions between Fermi accelerated protons and synchrotronphotons from co-accelerated electrons (or positrons) lead to charged pionproduction. We include synchrotron cooling of the charged pions andsuccessively produced muons, which then further decay into neutrinos, as wellas the helicity dependence of the muon decays. Our photohadronic interactionmodel includes direct production, higher resonances, and high energy processesin order to model the neutrino flavor and neutrino-antineutrino ratios withsufficient accuracy. Since we assume that the sources are optically thin toneutron interactions, we include the neutrino fluxes from neutron decays. Weclassify the Hillas plot into regions with different characteristic flavorratios over 20x24 orders of magnitude in R and B. In some examples with sizablemagnetic fields, we recover neutron beam, pion beam, and muon damped beam as afunction of energy. However, we also find anomalous or new sources, such asmuon beam sources with a flavor ratio nu_e:nu_mu:nu_tau of 1:1:0 in energyregions where the synchrotron-damped muons pile up. We also discuss the use ofthe Glashow resonance to identify pgamma optically thin sources with a strongimbalance between pi^+ and pi^- production. We find that these can, inprinciple, be identified in most cases in spite of the pi^- contamination fromhigh energy photohadronic processes and the mixing parameter uncertainties.

Energy dependent neutrino flavor ratios from cosmic accelerators on the Hillas plot