LOWER LIMITS ON ULTRAHIGH-ENERGY COSMIC RAY AND JET POWERS OF TeV BLAZARS

Lower limits on the power emitted in ultrahigh-energy cosmic rays (UHECRs), which are assumed to be protons with energy greater than or similar to 10(17)-10(20) eV, are derived for TeV blazars with the assumption that the observed TeV gamma-rays are generated due to interactions of these protons with cosmic microwave photons. The limits depend on the spectrum of the injected UHECR protons. While for a -2.2 injection spectrum the lower limits on the powers emitted in UHECRs by 1ES 0229+200, 1ES 1101-232, and 1ES 0347-121 are lower than their respective synchrotron luminosities (similar to 10(46) erg s(-1)), in the case of 1ES 1426+428 it exceeds the corresponding synchrotron luminosity by up to an order of magnitude. The proposed Auger North Observatory should be able to detect 4 x 10(19) eV cosmic-ray (CR) protons from 1ES 1426+428 within a few years of operation and test the TeV gamma-ray production model by UHECR energy losses while propagating along the line of sight or constrain the intergalactic magnetic field to be larger than similar to 10(-16) G in case of no detection. The lower limits on the apparent-isotropic jet power from accelerated 10(10)-10(20) eV proton spectra in the blazar jet is of the order of the Eddington luminosity of a 10(9) M-circle dot black hole for a CR injection spectrum -2.2 or harder for all blazars considered except for 1ES 1426+428. In the case of the latter, the apparent-isotropic jet power exceeds the Eddington luminosity by an order of magnitude. For an injection spectrum softer than -2.2, as is required to fit the observed CR data above similar to 10(17)-10(18) eV, the Eddington luminosity is exceeded by the lower limits on the jet power for all blazars considered.